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1. Future Perspectives for Gamma-ray Burst Detection from Space

Author

Enrico Bozzo, Lorenzo Amati, Wayne Baumgartner, Tzu-Ching Chang, Bertrand Cordier, Nicolas De Angelis, Akihiro Doi, Marco Feroci, Cynthia Froning, Jessica Gaskin, Adam Goldstein, Diego Götz, Jon E. Grove, Sylvain Guiriec, Margarita Hernanz, C. Michelle Hui, Peter Jenke, Daniel Kocevski, Merlin Kole, Chryssa Kouveliotou, Thomas Maccarone, Mark L. McConnell, Hideo Matsuhara, Paul O’Brien, Nicolas Produit, Paul S. Ray, Peter Roming, Andrea Santangelo, Michael Seiffert, Hui Sun, Alexander van der Horst, Peter Veres, Jianyan Wei, Nicholas White, Colleen Wilson-Hodge, Daisuke Yonetoku, Weimin Yuan, and Shuang-Nan Zhang

Subjects
γ-ray astrophysics, Gamma-ray bursts, X-ray polarimetry, X-ray surveys, X-ray instrumentation, Elementary particle physics, QC793-793.5
Abstract

Since their first discovery in the late 1960s, gamma-ray bursts have attracted an exponentially growing interest from the international community due to their central role in the most highly debated open questions of the modern research of astronomy, astrophysics, cosmology, and fundamental physics. These range from the intimate nuclear composition of high-density material within the core of ultra-dense neuron stars, to stellar evolution via the collapse of massive stars, the production and propagation of gravitational waves, as well as the exploration of the early universe by unveiling the first stars and galaxies (assessing also their evolution and cosmic re-ionization). GRBs in the past ∼50 years have stimulated the development of cutting-edge technological instruments for observations of high-energy celestial sources from space, leading to the launch and successful operations of many different scientific missions (several of them still in data-taking mode currently). In this review, we provide a brief description of the GRB-dedicated missions from space being designed and developed for the future. The list of these projects, not meant to be exhaustive, shall serve as a reference to interested readers to understand what is likely to come next to lead the further development of GRB research and the associated phenomenology.

Published
2024
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2. STROBE-X: X-ray timing and spectroscopy on dynamical timescales from microseconds to years

Author

Colleen A. Wilson-Hodge, Paul S. Ray, Keith Gendreau, Deepto Chakrabarty, Marco Feroci, Zaven Arzoumanian, Soren Brandt, Margarita Hernanz, C. Michelle Hui, Peter A. Jenke, Thomas Maccarone, Ron Remillard, Kent Wood, and Silvia Zane

Subjects
Physics, QC1-999
Abstract

The Spectroscopic Time-Resolving Observatory for Broadband Energy X-rays (STROBE-X) probes strong gravity for stellar mass to supermassive black holes and ultradense matter with unprecedented effective area, high time-resolution, and good spectral resolution, while providing a powerful time-domain X-ray observatory. Keywords: Missions, X-ray timing, X-ray spectroscopy, Compact objects

Published
2017
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4. 7Be in the outburst of the ONe nova V6595 Sgr

Author

M. Della Valle, P. Selvelli, Piercarlo Bonifacio, E. Aydi, G. Cescutti, E. J. Harvey, Paolo Molaro, Valentina D'Odorico, Luca Izzo, Margarita Hernanz, Villum Fonden, Ministerio de Ciencia, Innovación y Universidades (España), Molaro, P., Izzo, L., D'Odorico, V., Aydi, E., Bonifacio, P., Cescutti, G., Harvey, E. J., Hernanz, M., Selvelli, P., Della Valle, M., ITA, USA, and ESP

Subjects
GIANT, Astrophysics, nuclear reaction, Spectral line, nucleosynthesis abundances, Neon, ABSORPTION, ELEMENTS, Abundances, Emission spectrum, Absorption (electromagnetic radiation), Novae, Physics, cataclysmic variables, GAMMA-RAY LINES, Isotope, ORIGIN, nucleosynthesis, stars individual V6595 Sgr, Astrophysics - Solar and Stellar Astrophysics, Stars: individual: V6595 Sgr, novae cataclysmic variable, stars abundance, Nucleosynthesis, Cataclysmic variable, V5668 SGR, LI-7, chemistry.chemical_element, evolution [Galaxy], Galaxy evolution, LITHIUM, stars abundances, nucleosynthesis abundance, nuclear reactions, Galaxy: evolution, novae, abundances, novae cataclysmic variables, Stars: abundances, Resonance, Astronomy and Astrophysics, Nova (laser), K-line, EVOLUTION, abundances [stars], individual: V6595 Sgr [stars], chemistry, Space and Planetary Science, EMISSION
Abstract

We report on the search for the 7Be ii isotope in the outbursts of the classical nova V6595 Sgr by means of high-resolution Ultraviolet and Visual Echelle Spectrograph (UVES) observations taken at the European Southern Observatory's Very Large Telescope in 2021 April, about two weeks after its discovery and under difficult circumstances due to the pandemic. Narrow absorption components with velocities at -2620 and-2820 km s-1, superposed on broader and shallow absorption, are observed in the outburst spectra for the 7Be ii λλ313.0583, 313.1228 nm doublet resonance lines, as well as in several other elements such as Ca ii, Fe i, Mg i, Na i, H i and Li i. Using the Ca ii K line as a reference element, we infer N(7Be)/N(H) ≈ 7.4 × 10-6, or ≈ 9.8 × 10-6 when the 7Be decay is taken into account. The 7Be abundance is about half of the value most frequently measured in novae. The possible presence of overionization in the layers where 7Be ii is detected is also discussed. Observations taken at the Telescopio Nazionale Galileo in La Palma 91 days after discovery showed prominent emission lines of oxygen and neon, which allow us to classify the nova as ONe type. Therefore, although 7Be is expected to be higher in CO novae, it is found at comparable levels in both nova types., LI was supported by two grants from VILLUM FONDEN (project number 16599 and 25501). M. H. acknowledges support from grant PID2019-108709GB-100 from MICINN (Spain).

Published
2021
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5. The digital data processing concepts of the large area detector and the wide field monitor onboard eXTP

Author

Hao Xiong, Andrea Argan, David Baudin, Jörg Bayer, Florent Bouyjou, Nicolas De Angelis, Ettore Del Monte, Yuri Evangelista, Yannick Favre, Marco Feroci, José-Luis Galvez, Olivier Gevin, Paul Hedderman, Margarita Hernanz, Merlin R. Kole, Aline Meuris, Samuel Pliego-Caballero, Andrea Santangelo, Chris Tenzer, Alessio Trois, Xianqi Wang, and Gianluigi Zampa

Published
2022
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7. The detector/readout-electronics assembly of the eXTP wide field monitor

Author

Frans Zwart, Roland Tacken, Jean In't Zand, Rob de la Rie, Max Limpens, Cor Kochanowski, Gabby Aitink-Kroes, Coen van Baren, Jörg Bayer, David Baudin, Fabio Crescenti, Yuri Evangelista, Marco Feroci, Martin Frericks, José-Luis Gálvez, Olivier Gevin, Margarita Hernanz, Ander Hormaetxe, Phillip Laubert, Aline Meuris, Jasper Nab, John Neelis, Chris Tenzer, Channah Vogel, and Gianluigi Zampa

Published
2022
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8. The Instrument Control Unit processing hardware and software of the Wide Field Monitor on eXTP

Author

Emrah Kalemci, Onur Turhan, Irfan Kuvvetli, Stéphane Schanne, Margarita Hernanz, Piotr Orleanski, Chris Tenzer, Müberra Sungur, Ahmet Onat, Ayhan Bozkurt, Mehmet A. Baltaci, José-Luis . Galvez, Søren Brandt, Konrad R. Skup, Denis Tcherniak, Malgorzata Michalska, den Herder, Jan-Willem A., Nikzad, Shouleh, and Nakazawa, Kazuhiro

Subjects
LaTeX, SPIE Proceedings, Template, Manuscript format
Abstract

The eXTP (enhanced X-ray Timing and Polarimetry) mission is a joint large mission of the Chinese Academy of Sciences (CAS) and European partners designed to study the state of matter under extreme conditions of density, gravity and magnetism. One of the four major instruments on eXTP is the Wide Field Monitor (WFM) which consist of 3 pairs of coded mask cameras with a total combined Field of View (FoV) of 90×180 degrees at zero response. With its enormous FoV, a source localization accuracy of 1 arcmin and an energy range of 2-50 keV the primary objective of the WFM is to provide triggers for the pointing instruments on the eXTP with less than one day reaction time. Its large area and resolution will be enough to detect state changes in compact objects as well. The WFM instrument is controlled by the Data Handling Unit located inside the Instrument Control Unit. The challenging requirement of broadcasting time and end-position of the triggering event to end-users in 30s necessitates special on-board data processing software (the eXTP burst online trigger, or XBOT), a hardware that can perform such processing and associated control software that would feed the raw data from the cameras into the XBOT and relaying alerts to the on-board data handling unit on the spacecraft side. Moreover, the WFM software performs several tasks related to the science data preparation, telecommand and telemetry management, and control of the cameras utilizing four LEON4 processing cores of E698 PM SoC from OCE Technology. This presentation discusses the details of the processing hardware and the interaction between different software components of the WFM on eXTP.

Published
2022
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9. Detection of $^7$Be II in the Small Magellanic Cloud

Author

Luca Izzo, Paolo Molaro, Gabriele Cescutti, Elias Aydi, Pierluigi Selvelli, Eamonn Harvey, Adriano Agnello, Piercarlo Bonifacio, Massimo Della Valle, Ernesto Guido, Margarita Hernanz, ITA, USA, FRA, ESP, Villum Fonden, European Commission, National Aeronautics and Space Administration (US), Ministerio de Ciencia e Innovación (España), Izzo, L., Molaro, P., Cescutti, G., Aydi, E., Selvelli, P., Harvey, E., Agnello, A., Bonifacio, P., Della Valle, M., Guido, E., and Hernanz, M.

Subjects
Galaxy Abundances, Stars Individual ASSASN-19qv, Galaxy Evolution, FOS: Physical sciences, evolution [Galaxy], Galaxy Abundance, individuals: ASSASN-19qv [Stars], ASASSN-20ni, Abundances, Solar and Stellar Astrophysics (astro-ph.SR), Galaxy: evolution, abundance, abundances, stars novae, nucleosynthesis, abundances [Galaxy], Astronomy and Astrophysics, Nuclear reaction, Astrophysics - Astrophysics of Galaxies, Nuclear reactions, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, nucleosynthesi, Astrophysics of Galaxies (astro-ph.GA), Galaxy: abundances, novae [Stars], Stars: individuals: ASSASN-19qv, Stars: novae, Nucleosynthesis
Abstract

We analyse high resolution spectra of two classical novae that exploded in the Small Magellanic Cloud. $^7$Be II resonance transitions are detected in both ASASSN-19qv and ASASSN-20ni novae. This is the first detection outside the Galaxy and confirms that thermo-nuclear runaway reactions, leading to the $^7$Be formation, are effective also in the low metallicity regime, characteristic of the SMC. Derived yields are of N($^7$Be=$^7$Li)/N(H) = (5.3 $\pm$ 0.2) $\times$ 10$^{-6}$ which are a factor 4 lower than the typical values of the Galaxy. Inspection of two historical novae in the Large Magellanic Cloud observed with IUE in 1991 and 1992 showed also the possible presence of $^7$Be and similar yields. For an ejecta of $M_{H,ej} =$ 10$^{-5}$ M$_{\odot}$, the amount of $^7$Li produced is of $M_{^7 Li} = (3.7 \pm 0.6) \times 10^{-10}$ M$_{\odot}$ per nova event. Detailed chemical evolutionary model for the SMC shows that novae could have made an amount of lithium in the SMC corresponding to a fractional abundance of A(Li) $\approx$ 2.6. Therefore, it is argued that a comparison with the abundance of Li in the SMC, as measured by its interstellar medium, could effectively constrain the amount of the initial abundance of primordial Li, which is currently controversial., 13 pages, 17 figures, 4 tables. Accepted for publication in MNRAS

Published
2021
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10. INTEGRAL reloaded: Spacecraft, instruments and ground system

Author

Marius Baab, Diego Götz, Jérôme Chenevez, Julia Alfonso-Garzon, R. A. Sunyaev, Norbert Schartel, Margarita Hernanz, Richard Southworth, Ian Benson, Lorenzo Natalucci, Aymeric Sauvageon, Alexis Coleiro, Stefano De Padova, Liviu Toma, Claudia Dietze, Christoph Winkler, Andrea Goldwurm, Jochen Greiner, Christian Gouiffes, Gianluca Gaudenzi, Cristina Hernandez, Niels Lund, W. Hermsen, Angela Bazzano, Mariateresa Fiocchi, Alexander Lehanka, B. McBreen, Lorraine Hanlon, Roland Diehl, James Madison, S. A. Grebenev, Sibylle Peschke, Dave Salt, Alastair McDonald, Julie McEnery, Guillaume Belanger, Peter Kretschmar, Sergey Sazonov, Elliott Coe, A. Domingo, Jim Martin, J. Rodriguez, Mark Drapes, Thomas Siegert, Nikolai von Krusenstiern, Julien Malzac, Isabel Caballero, Sandro Mereghetti, Thomas Godard, Jan-Uwe Ness, E. Jourdain, Edward van den Heuvel, E. Kuulkers, Matthias Ehle, Norbert Pfeil, Søren Brandt, Elena Garcia Tomas, Claudio Labanti, Ugo Zannoni, John Palmer, F. Cangemi, J. Rodi, P. Laurent, Pietro Ubertini, J. P. Roques, J. Miguel Mas-Hesse, A. J. Bird, Michael Reichenbaecher, Carlo Ferrigno, Stefano Scaglioni, Francesco Petrucciani, N. Eismont, Celia Sanchez-Fernandez, Andreas von Kienlin, Jacobo Ebrero, Timothy Finn, Aleksandra Gros, V. G. Savchenko, Mithrajith Edirimanne, Enrico Bozzo, Bradley Cenko, Jutta Hübner, Giovanni La Rosa, Nebil Cinar, Emilio Salazar Donate, Eleonora D’uva, W. Hajdas, Carol Anne Oxborrow, Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Agenzia Spaziale Italiana, German Research Foundation, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
neutron star: binary, gamma ray: polarization, energy resolution, 7. Clean energy, 01 natural sciences, High Energy Physics - Experiment, 99-00, Gamma-ray observatory, High Energy Physics - Experiment (hep-ex), optical, time resolution, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gamma-ray instruments, 00-01, charged particle, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, satellite: orbit, radiation: electromagnetic, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, positron: annihilation, X-ray, Target of opportunity, supernova, 0103 physical sciences, gamma ray: detector, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Spectral resolution, Instrumentation and Methods for Astrophysics (astro-ph.IM), Gamma-ray sources, Spectrometer, Spacecraft, 010308 nuclear & particles physics, Gravitational wave, business.industry, INTEGRAL, resolution, Astronomy, Astronomy and Astrophysics, monitoring, Neutron star, angular resolution, Space and Planetary Science, spectral, direct detection, Satellite, spectrometer, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], business, Space environment
Abstract

The European Space Agency's INTErnational Gamma-Ray Astrophysics Laboratory (ESA/INTEGRAL) was launched aboard a Proton-DM2 rocket on 17 October 2002 at 06:41 CEST, from Baikonur in Kazakhstan. Since then, INTEGRAL has been providing long, uninterrupted observations (up to about 47h, or 170ksec, per satellite orbit of 2.7 days) with a large field-of-view (FOV, fully coded: 100 deg), millisecond time resolution, keV energy resolution, polarization measurements, as well as additional wavelength coverage at optical wavelengths. This is realized by two main instruments in the 15keV to 10MeV energy range, the spectrometer SPI (spectral resolution 3keV at 1.8MeV) and the imager IBIS (angular resolution: 12arcmin FWHM), complemented by X-ray (JEM-X; 3–35keV) and optical (OMC; Johnson V-band) monitor instruments. All instruments are co-aligned to simultaneously observe the target region. A particle radiation monitor (IREM) measures charged particle fluxes near the spacecraft. The Anti-coincidence subsystems of the main instruments, built to reduce the background, are also very efficient all-sky γ-ray detectors, which provide virtually omni-directional monitoring above ∼75keV. Besides the long, scheduled observations, INTEGRAL can rapidly (within a couple of hours) re-point and conduct Target of Opportunity (ToO) observations on a large variety of sources. INTEGRAL observations and their scientific results have been building an impressive legacy: The discovery of currently more than 600 new high-energy sources; the first-ever direct detection of Ni and Co radio-active decay lines from a Type Ia supernova; spectroscopy of isotopes from galactic nucleo-synthesis sources; new insights on enigmatic positron annihilation in the Galactic bulge and disk; and pioneering gamma-ray polarization studies. INTEGRAL is also a successful actor in the new multi-messenger astronomy introduced by non-electromagnetic signals from gravitational waves and from neutrinos: INTEGRAL found the first prompt electromagnetic radiation in coincidence with a binary neutron star merger. Up to now more than 1750 scientific papers based on INTEGRAL data have been published in refereed journals. In this paper, we will give a comprehensive update of the satellite status after more than 18 years of operations in a harsh space environment, and an account of the successful Ground Segment., Kuulkers, Erik, et al., he OMC team has been funded by different Spanish grants, including Spanish State Research Agency grants PID2019–107061GB–C61 and MDM–2017-0737 (Unidad de Excelencia María de Maeztu – CAB). The INTEGRAL French teams acknowledge partial funding from the French Space Agency (CNES). The Danish JEM-X gratefully acknowledges support from the Danish PRODEX delegation through contract C90057. The INTEGRAL Italian team acknowledges support form the Italian Space Agency, ASI, along these years via different agreements, last of which is 2019–35-HH.0. LH acknowledges support from SFI under grant 19/FFP/6777 and the EU AHEAD2020 project (grant agreement 871158). MH acknowledges support from Spanish MICINN grant PID2019-108709GB-I00. TS is supported by the German Research Society (DFG-Forschungsstipendium SI 2502/1-1 & SI 2502/3-1).

Published
2021
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11. Nova LMC 2009a as observed with XMM¿Newton, compared with other novae

Author

Jan-Uwe Ness, Sou Her, Martin Henze, Ehud Behar, Ciro Pinto, A. Dobrotka, N. Ospina, Marina Orio, Gloria Sala, S. Pei, Michael F. Bode, Margarita Hernanz, National Aeronautics and Space Administration (US), European Commission, Universitat Politècnica de Catalunya. Departament de Física, and Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica

Subjects
Transients: novae, 010504 meteorology & atmospheric sciences, Line: identification, Continuum (design consultancy), individual" KT Eri [X-rays], Flux, FOS: Physical sciences, Astrophysics, novae [Transients], 01 natural sciences, Spectral line, 0103 physical sciences, Emission spectrum, identification [Line], Ejecta, 010303 astronomy & astrophysics, Profiles, Novae, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Cataclysmic variables, X-Rays, White dwarf, Astronomy and Astrophysics, Effective temperature, Stars, Estels, Amplitude, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], X-rays: individual" KT Eri, individual [X-rays], Astrophysics - High Energy Astrophysical Phenomena
Abstract

We examine four high resolution reflection grating spectrometers (RGS) spectra of the February 2009 outburst of the luminous recurrent nova LMC 2009a. They were very complex and rich in intricate absorption and emission features. The continuum was consistent with a dominant component originating in the atmosphere of a shell burning white dwarf (WD) with peak effective temperature between 810,000 K and a million K, and mass in the 1.2-1.4 M$_\odot$ range. A moderate blue shift of the absorption features of a few hundred km s$^{-1}$ can be explained with a residual nova wind depleting the WD surface at a rate of about 10$^{-8}$ M$_\odot$ yr$^{-1}$. The emission spectrum seems to be due to both photoionization and shock ionization in the ejecta. The supersoft X-ray flux was irregularly variable on time scales of hours, with decreasing amplitude of the variability. We find that both the period and the amplitude of another, already known 33.3 s modulation, varied within timescales of hours. We compared N LMC 2009a with other Magellanic Clouds novae, including 4 serendipitously discovered as supersoft X-ray sources (SSS) among 13 observed within 16 years after the eruption. The new detected targets were much less luminous than expected: we suggest that they were partially obscured by the accretion disk. Lack of SSS detections in the Magellanic Clouds novae more than 5.5 years after the eruption constrains the average duration of the nuclear burning phase., Comment: Accepted for publication in MNRAS

Published
2021

12. Mission analysis and preliminary spacecraft design of the enhanced x-ray timing and polarimetry observatory

Author

Junwang He, Shuang-Nan Zhang, Marco Feroci, Yuan Fang, Jinpei Yu, Yueting Zhang, Kuoxiang Zhang, Qi Shi, Yehai Chen, Weiwei Zhao, Zhencai Zhu, Xingzi Bi, Yupeng Xu, Shi Xingjian, Fangjun Lu, Margarita Hernanz, Yang Yingquan, Xiangyu Chao, Riu Liu, Xingbo Han, Huili Yuan, Wen Chen, Cheng Zhu, and Chinese Academy of Sciences

Subjects
Physics, Observatory, Astrophysics::High Energy Astrophysical Phenomena, Mission analysis, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimetry, Gamma ray, Astrophysics::Solar and Stellar Astrophysics, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Instrumentation (computer programming), Spacecraft design
Abstract

Event: Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray, 114442E (13 December 2020)., The enhanced X-ray Timing and Polarimetry Observatory (eXTP) is a flagship international collaboration mission led by Chinese Academy of Sciences, with a large contribution from more than 20 European institutes. eXTP mission is designed to study the equation of state of ultra-dense matter under extreme conditions of strong density, gravity and magnetic field. The satellite carries four main instruments, including the Spectroscopy Focusing Array (SFA), the Large Area Detector (LAD), the Polarimetry Focusing array (PFA) and the Wide Field Monitor (WFM), enabling simultaneous spectral-timing-polarimetry studies of celestial sources in the energy range from 0.5-30 keV. The satellite will fly at a near-zero-inclination Low Earth Orbit, and is featured with long-time steady high-precision coaxial pointing, near realtime burst alert distribution, and follow-up maneuver capabilities. This paper describes the primary mission requirements and constraints, and presents an overall mission analysis including orbit analysis, pointing strategy, and board-ground communications, etc. The preliminary design of eXTP satellite is also introduced, including satellite overall configuration, observation modes, avionics architecture and development plan., The mission is led by China, currently supported by Chinese Academy of Sciences and executed under the management of the National Space Science Center of CAS. The project has officially kicked off Phase B in November 2019. After Phase C1, official mission adoption is expected. With Phase C2 and Phase D planned in 2023-2027, the eXTP satellite is targeted to be launched in 2027.

Published
2020

13. Application of the THM to the investigation of reactions induced by unstable nuclei: the 18F(p,a)15O case

Author

R. G. Pizzone, Jordi José, Marco La Cognata, Silvio Cherubini, Marisa Gulino, Claudio Spitaleri, Margarita Hernanz, G. G. Rapisarda, Universitat Politècnica de Catalunya. Departament de Física, and Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica

Subjects
Physics, Astrofísica nuclear, 010308 nuclear & particles physics, QC1-999, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], 0103 physical sciences, 010303 astronomy & astrophysics, 01 natural sciences
Abstract

The Trojan Horse Method is applied to the investigation of the18F(p,α)15O reaction, by extracting the quasi free contribution to the2H(18F,α15O)nprocess. For the first time the method is applied to a reaction of astrophysical importance involving a radioactive nucleus. After investigating the reaction mechanism populating the a +15O + n exit channel, we could extract the18F(p,α)15O cross section and calculate the astrophysical factor over the 0 – 1 MeV energy interval. The possibility of exploring the cross section with no need of extrapolation allowed us to to point out the possible occurrence of a 7/2+state at 126 keV, which would strongly influence the trend of the astrophysical factor at the energies of astrophysical interest. However, the low energy resolution prevents us to draw definite conclusions. Possible astrophysical consequences are also discussed, motivating further work on this reaction.

Published
2019

14. Synthesis of radioactive elements in novae and supernovae and their use as a diagnostic tool

Author

P. Jean, Thomas Siegert, S. A. Grebenev, Eduardo Bravo, Margarita Hernanz, Matthieu Renaud, Jacco Vink, Jordi Isern, Ministerio de Economía y Competitividad (España), European Commission, Generalitat de Catalunya, German Research Foundation, Russian Science Foundation, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, Cosmology, general-gamma rays [Novae], Supernovae: general-gamma rays, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Supernova remnant, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Novae: general-gamma rays, High Energy Astrophysical Phenomena (astro-ph.HE), [PHYS]Physics [physics], Physics, Novae: general–gamma rays, 010308 nuclear & particles physics, Supernovae: general–gamma rays, Astronomy and Astrophysics, Type II supernova, Galaxy, Supernova, general-gamma rays [Supernovae], Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Thermal state, Astrophysics - High Energy Astrophysical Phenomena, Radioactive decay
Abstract

Novae and supernovae play a key role in many fields of Astrophysics and Cosmology. Despite their importance, an accurate description of which objects explode and why and how they explode is still lacking. One of the main characteristics of such explosions is that they are the main suppliers of newly synthesized chemical elements in the Galaxy. Since some of these isotopes are radioactive, it is possible to use the corresponding gamma-rays as a diagnostic tool of the explosion thanks to their independence on the thermal state of the debris. The drawback is the poor sensitivity of detectors in the MeV energy domain. As a consequence, the radioactive lines have only been detected in one core collapse supernova (SN 1987A), one Type Ia supernova (SN 2014J), and one supernova remnant (Cas A). Nevertheless these observations have provided and are providing important information about the explosion mechanisms. Unfortunately, novae are still eluding detection. These results emphasize the necessity to place as soon as possible a new instrument in orbit with enough sensitivity to noticeably enlarge the sample of detected events., This work has been supported by MINECO grants AYA2015-63588-P and PGC2018-095317-B-C21 (EB), ESP2017-82674-R (MH, JI), by EU FEDER funds and by grants 2014SGR1458 and CERCA Programme of the Generalitat de Catalunya (MH, JI), by the German Research Society, DFG-Forschungsstipedium SI 2502/1-1 (TS), by project no. 18-12-00522 of the Russian Science Foundation (SG).

Published
2021
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15. The enhanced X-ray Timing and Polarimetry mission—eXTP

Author

ShuangNan Zhang, Andrea Santangelo, Marco Feroci, YuPeng Xu, FangJun Lu, Yong Chen, Hua Feng, Shu Zhang, Søren Brandt, Margarita Hernanz, Luca Baldini, Enrico Bozzo, Riccardo Campana, Alessandra De Rosa, YongWei Dong, Yuri Evangelista, Vladimir Karas, Norbert Meidinger, Aline Meuris, Kirpal Nandra, Teng Pan, Giovanni Pareschi, Piotr Orleanski, QiuShi Huang, Stephane Schanne, Giorgia Sironi, Daniele Spiga, Jiri Svoboda, Gianpiero Tagliaferri, Christoph Tenzer, Andrea Vacchi, Silvia Zane, Dave Walton, ZhanShan Wang, Berend Winter, Xin Wu, Jean J. M. in’ t Zand, Mahdi Ahangarianabhari, Giovanni Ambrosi, Filippo Ambrosino, Marco Barbera, Stefano Basso, Jörg Bayer, Ronaldo Bellazzini, Pierluigi Bellutti, Bruna Bertucci, Giuseppe Bertuccio, Giacomo Borghi, XueLei Cao, Franck Cadoux, Francesco Ceraudo, TianXiang Chen, YuPeng Chen, Jerome Chevenez, Marta Civitani, Wei Cui, WeiWei Cui, Thomas Dauser, Ettore Del Monte, Sergio Di Cosimo, Sebastian Diebold, Victor Doroshenko, Michal Dovciak, YuanYuan Du, Lorenzo Ducci, QingMei Fan, Yannick Favre, Fabio Fuschino, José Luis Gálvez, Min Gao, MingYu Ge, Olivier Gevin, Marco Grassi, QuanYing Gu, YuDong Gu, DaWei Han, Bin Hong, Wei Hu, Long Ji, ShuMei Jia, WeiChun Jiang, Thomas Kennedy, Ingo Kreykenbohm, Irfan Kuvvetli, Claudio Labanti, Luca Latronico, Gang Li, MaoShun Li, Xian Li, Wei Li, ZhengWei Li, Olivier Limousin, HongWei Liu, XiaoJing Liu, Bo Lu, Tao Luo, Daniele Macera, Piero Malcovati, Adrian Martindale, Malgorzata Michalska, Bin Meng, Massimo Minuti, Alfredo Morbidini, Fabio Muleri, Stephane Paltani, Emanuele Perinati, Antonino Picciotto, Claudio Piemonte, JinLu Qu, Alexandre Rachevski, Irina Rashevskaya, Jerome Rodriguez, Thomas Schanz, ZhengXiang Shen, LiZhi Sheng, JiangBo Song, LiMing Song, Carmelo Sgro, Liang Sun, Ying Tan, Phil Uttley, Bo Wang, DianLong Wang, GuoFeng Wang, Juan Wang, LangPing Wang, YuSa Wang, Anna L. Watts, XiangYang Wen, Jörn Wilms, ShaoLin Xiong, JiaWei Yang, Sheng Yang, YanJi Yang, Nian Yu, WenDa Zhang, Gianluigi Zampa, Nicola Zampa, Andrzej A. Zdziarski, AiMei Zhang, ChengMo Zhang, Fan Zhang, Long Zhang, Tong Zhang, Yi Zhang, XiaoLi Zhang, ZiLiang Zhang, BaoSheng Zhao, ShiJie Zheng, YuPeng Zhou, Nicola Zorzi, J. Frans Zwart, ITA, GBR, FRA, DEU, ESP, DNK, POL, CZE, CHN, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, eXTP, Zhang, ShuangNan, Santangelo, Andrea, Feroci, Marco, Xu, YuPeng, Lu, FangJun, Chen, Yong, Feng, Hua, Zhang, Shu, Brandt, Søren, Hernanz, Margarita, Baldini, Luca, Bozzo, Enrico, Campana, Riccardo, De Rosa, Alessandra, Dong, YongWei, Evangelista, Yuri, Karas, Vladimir, Meidinger, Norbert, Meuris, Aline, Nandra, Kirpal, Pan, Teng, Pareschi, Giovanni, Orleanski, Piotr, Huang, QiuShi, Schanne, Stephane, Sironi, Giorgia, Spiga, Daniele, Svoboda, Jiri, Tagliaferri, Gianpiero, Tenzer, Christoph, Vacchi, Andrea, Zane, Silvia, Walton, Dave, Wang, ZhanShan, Winter, Berend, Wu, Xin, in’ t Zand, Jean J. M., Ahangarianabhari, Mahdi, Ambrosi, Giovanni, Ambrosino, Filippo, Barbera, Marco, Basso, Stefano, Bayer, Jörg, Bellazzini, Ronaldo, Bellutti, Pierluigi, Bertucci, Bruna, Bertuccio, Giuseppe, Borghi, Giacomo, Cao, XueLei, Cadoux, Franck, Ceraudo, Francesco, Chen, TianXiang, Chen, YuPeng, Chevenez, Jerome, Civitani, Marta, Cui, Wei, Cui, WeiWei, Dauser, Thoma, Del Monte, Ettore, Di Cosimo, Sergio, Diebold, Sebastian, Doroshenko, Victor, Dovciak, Michal, Du, YuanYuan, Ducci, Lorenzo, Fan, QingMei, Favre, Yannick, Fuschino, Fabio, Gálvez, José Lui, Gao, Min, Ge, MingYu, Gevin, Olivier, Grassi, Marco, Gu, QuanYing, Gu, YuDong, Han, DaWei, Hong, Bin, Hu, Wei, Ji, Long, Jia, ShuMei, Jiang, WeiChun, Kennedy, Thoma, Kreykenbohm, Ingo, Kuvvetli, Irfan, Labanti, Claudio, Latronico, Luca, Li, Gang, Li, MaoShun, Li, Xian, Li, Wei, Li, ZhengWei, Limousin, Olivier, Liu, HongWei, Liu, XiaoJing, Lu, Bo, Luo, Tao, Macera, Daniele, Malcovati, Piero, Martindale, Adrian, Michalska, Malgorzata, Meng, Bin, Minuti, Massimo, Morbidini, Alfredo, Muleri, Fabio, Paltani, Stephane, Perinati, Emanuele, Picciotto, Antonino, Piemonte, Claudio, Qu, JinLu, Rachevski, Alexandre, Rashevskaya, Irina, Rodriguez, Jerome, Schanz, Thoma, Shen, ZhengXiang, Sheng, LiZhi, Song, JiangBo, Song, LiMing, Sgro, Carmelo, Sun, Liang, Tan, Ying, Uttley, Phil, Wang, Bo, Wang, DianLong, Wang, GuoFeng, Wang, Juan, Wang, LangPing, Wang, YuSa, Watts, Anna L., Wen, XiangYang, Wilms, Jörn, Xiong, ShaoLin, Yang, JiaWei, Yang, Sheng, Yang, YanJi, Yu, Nian, Zhang, WenDa, Zampa, Gianluigi, Zampa, Nicola, Zdziarski, Andrzej A., Zhang, AiMei, Zhang, ChengMo, Zhang, Fan, Zhang, Long, Zhang, Tong, Zhang, Yi, Zhang, XiaoLi, Zhang, ZiLiang, Zhao, BaoSheng, Zheng, ShiJie, Zhou, YuPeng, Zorzi, Nicola, Zwart, J. Frans, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Gravity (chemistry), Computer science, space mission: eXTP, X-ray timing, Polarimetry, General Physics and Astronomy, FOS: Physical sciences, 01 natural sciences, 7. Clean energy, Physics and Astronomy (all), Settore FIS/05 - Astronomia E Astrofisica, Observatory, X-ray instrumentation, 0103 physical sciences, X-ray polarimetry, Ground segment, Aerospace engineering, 010306 general physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), High Energy Astrophysical Phenomena (astro-ph.HE), Spacecraft, sezele, business.industry, Payload, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, Space Science, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

In this paper we present the enhanced X-ray Timing and Polarimetry mission - eXTP. eXTP is a space science mission designed to study fundamental physics under extreme conditions of density, gravity and magnetism. The mission aims at determining the equation of state of matter at supra-nuclear density, measuring effects of QED, and understanding the dynamics of matter in strong-field gravity. In addition to investigating fundamental physics, eXTP will be a very powerful observatory for astrophysics that will provide observations of unprecedented quality on a variety of galactic and extragalactic objects. In particular, its wide field monitoring capabilities will be highly instrumental to detect the electro-magnetic counterparts of gravitational wave sources. The paper provides a detailed description of: (1) the technological and technical aspects, and the expected performance of the instruments of the scientific payload; (2) the elements and functions of the mission, from the spacecraft to the ground segment., Accepted for publication on Sci. China Phys. Mech. Astron. (2019)

Published
2019
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16. Background for a gamma-ray satellite on a low-Earth orbit

Author

Jurgen Kiener, Andreas Zoglauer, Margarita Hernanz, V. Tatischeff, P. Cumani, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), and Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Photon, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, 01 natural sciences, 7. Clean energy, Spectral line, Gamma-ray, Nuclear physics, 0103 physical sciences, Neutron, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Isotope, 010308 nuclear & particles physics, Gamma ray, Astronomy and Astrophysics, LEO, Charged particle, South Atlantic Anomaly, Earth's magnetic field, Background, 13. Climate action, Space and Planetary Science, Satellite, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The different background components in a low-Earth orbit have been modeled in the 10 keV to 100 GeV energy range. The model is based on data from previous instruments and it considers both primary and secondary particles, charged particles, neutrons and photons. The necessary corrections to consider the geomagnetic cutoff are applied to calculate the flux at different inclinations and altitudes for a mean solar activity. Activation simulations from such a background have been carried out using the model of a possible future gamma-ray mission (e-ASTROGAM). The event rates and spectra from these simulations were then compared to those from the isotopes created by the particles present in the South Atlantic Anomaly (SAA). The primary protons are found to be the main contributor of the activation, while the contributions of the neutrons, and that of the secondary protons can be considered negligible. The long-term activation from the passage through the SAA becomes the main source of background at high inclination (i$\gtrsim10^\circ$). The used models have been collected in a Python class openly available on github., accepted for publication in Experimental Astronomy

Published
2019
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17. The wide field monitor onboard the eXTP mission

Author

Irina Rashevskaya, Andrea Vacchi, Alexander Rachevski, Niels Lund, Carl Budtz-Jorgensen, Ettore Del Monte, Andrea Argan, F. Ambrosino, Tianxiang Cheng, Shu Zhang, Fanjung Lu, Frans Zwart, Chris Tenzer, José Luis Gálvez, Yuri Evangelista, Enrico Bozzo, Yupeng Xu, Aline Meris, Olivier Limousin, Nicola Zorzi, Antonino Picciotto, Francesco Ficorella, Giacomo Borghi, Pierluigi Bellutti, Nicola Zampa, Gianluigi Zampa, Claudio Labanti, F. Fuschino, Riccardo Campana, Carlos Mansanet, Poul Erik Olsen, Shuangnan Zhang, Jean in't Zand, Xin Wu, Stéphane Schanne, Andrea Santangelo, Piotr Orleański, Marco Feroci, Margarita Hernanz, Søren K. Brandt, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and eXTP

Subjects
Computer science, X-ray timing, Polarimetry, FOS: Physical sciences, Silicon Drift Detectors, Field of view, Context (language use), coded mask imaging, compact objects, eXTP, gamma-ray bursts, LOFT, X-ray spectroscopy, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, Electrical and Electronic Engineering, 7. Clean energy, 01 natural sciences, 0103 physical sciences, Electronic, Optical and Magnetic Materials, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Remote sensing, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Payload, Suite, Detector, Orbit (dynamics), Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Energy (signal processing)
Abstract

The eXTP (enhanced X-ray Timing and Polarimetry) mission is a major project of the Chinese Academy of Sciences (CAS) and China National Space Administration (CNSA) currently performing an extended phase A study and proposed for a launch by 2025 in a low-earth orbit. The eXTP scientific payload envisages a suite of instruments (Spectroscopy Focusing Array, Polarimetry Focusing Array, Large Area Detector and Wide Field Monitor) offering unprecedented simultaneous wide-band X-ray timing and polarimetry sensitivity. A large European consortium is contributing to the eXTP study and it is expected to provide key hardware elements, including a Wide Field Monitor (WFM). The WFM instrument for eXTP is based on the design originally proposed for the LOFT mission within the ESA context. The eXTP/WFM envisages a wide field X-ray monitor system in the 2-50 keV energy range, achieved through the technology of the large-area Silicon Drift Detectors. The WFM will consist of 3 pairs of coded mask cameras with a total combined Field of View (FoV) of 90x180 degrees at zero response and a source localization accuracy of ~1 arcmin. In this paper we provide an overview of the WFM instrument design, including new elements with respect to the earlier LOFT configuration, and anticipated performance., Comment: 16 pages, 15 figures, to appear in proceedings of SPIE, Space Telescopes and Instrumentation 2018: Ultraviolet to Gamma Ray

Published
2018
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18. What we learn from the X-Ray grating spectra of Nova SMC 2016

Author

Gloria Sala, Stefano Ciroi, E. Aydi, Robert E. Williams, J. P. Osborne, K. L. Page, David A. H. Buckley, Marina Orio, Ehud Behar, Polina Zemko, Charles E. Woodward, Thomas Rauch, A. Dobrotka, Sumner Starrfield, M. Della Valle, Margarita Hernanz, Martin Henze, N. Ospina, Efrain Gatuzz, Jan-Uwe Ness, Universitat Politècnica de Catalunya. Departament de Física, and Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica

Subjects
Astrofísica, stars: abundances, 010504 meteorology & atmospheric sciences, education, stars: individual (N SMC 2016a), chemistry.chemical_element, FOS: Physical sciences, X-rays: stars, Astrophysics, 01 natural sciences, Spectral line, 0103 physical sciences, 010303 astronomy & astrophysics, novae, cataclysmic variables, stars: dwarf novae, 0105 earth and related environmental sciences, stars [X-rays], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), novae, cataclysmic variables, Argon, Atmospheric models, White dwarf, Astronomy and Astrophysics, Effective temperature, Light curve, Interstellar medium, abundances [stars], individual (N SMC 2016a) [stars], chemistry, Space and Planetary Science, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], dwarf novae [stars], Small Magellanic Cloud, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Nova SMC 2016 has been the most luminous nova known in the direction of the Magellanic Clouds. It turned into a very luminous supersoft X-ray source between day 16 and 28 after the optical maximum. We observed it with Chandra, the HRC-S camera and the Low Energy Transmission Grating (LETG) on 2016 November and 2017 January (days 39 and 88 after optical maximum), and with XMM-Newton on 2016 December (day 75). We detected the compact white dwarf (WD) spectrum as a luminous supersoft X-ray continuum with deep absorption features of carbon, nitrogen, magnesium, calcium, probably argon and sulfur on day 39, and oxygen, nitrogen and carbon on days 75 and 88. The spectral features attributed to the WD atmosphere are all blue-shifted, by about 1800 km/s on day 39 and up to 2100 km/s in the following observations. Spectral lines attributed to low ionization potential transitions in the interstellar medium are also observed. Assuming the distance of the Small Magellanic Cloud, the bolometric luminosity exceeded Eddington level for at least three months. A preliminary analysis with atmospheric models indicates effective temperature around 700,000 K on day 39, peaking at the later dates in the 850,000-900,000 K range, as expected for a 1.25 m(sol) WD. We suggest a possible classification as an oxygen-neon WD, but more precise modeling is needed to accurately determine the abundances. The X-ray light curves show large, aperiodic ux variability, not associated with spectral variability. We detected red noise, but did not find periodic or quasi-periodic modulations., Accepted for publication in the Astrophysical Journal, pending final editorial review after "minor changes"

Published
2018
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19. Gamma-Ray Observations of Nova Sgr 2015 No. 2 with INTEGRAL

Author

Laura Delgado, Paolo Molaro, Vincent Tatischeff, Thomas Siegert, Pierre Jean, V. G. Savchenko, Alain Coc, Roland Diehl, Sumner Starrfield, Margarita Hernanz, Christoph Weinberger, Jordi José, Moritz M. M. Pleintinger, Jochen Greiner, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre de Sciences Nucléaires et de Sciences de la Matière ( CSNSM ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Universitat Politècnica de Catalunya. Departament de Física, and Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica

Subjects
Nuclear reaction, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, education, FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, Nucleosynthesis, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, nuclear reactions, Astrophysics::Galaxy Astrophysics, white dwarfs, Physics, novae, High Energy Astrophysical Phenomena (astro-ph.HE), Solar mass, cataclysmic variables, Spectrometer, Reaccions nuclears, abundances, Gamma ray, White dwarf, nucleosynthesis, Astronomy and Astrophysics, Nova (laser), gamma rays: general, Stars, Estels, Space and Planetary Science, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], spectroscopic [techniques], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], general [gamma rays], techniques: spectroscopic
Abstract

INTEGRAL observed the nova V5668 Sgr around the time of its optical maximum on March 21, 2015. Studies at UV wavelengths showed spectral lines of freshly produced Be-7. This could be measurable also in gamma-rays at 478 keV from the decay to Li-7. Novae are also expected to synthesise Na-22 which decays to Ne-22, emitting a 1275 keV photon. About one week before the optical maximum, a strong gamma-ray flash on time-scales of hours is expected from short-lived radioactive nuclei, such as N-13 and F-18. These beta-plus-unstable nuclei should yield emission up to 511 keV, but which has never been observed. The spectrometer SPI aboard INTEGRAL pointed towards V5668 by chance. We use these observations to search for possible gamma-ray emission of decaying Be-7, and to directly measure the synthesised mass during explosive burning. We also aim to constrain possible burst-like emission days to weeks before the optical maximum using the SPI anticoincidence shield (ACS). We extract spectral and temporal information to determine the fluxes of gamma-ray lines at 478 keV, 511 keV, and 1275 keV. A measured flux value directly converts into abundances produced by the nova. The SPI-ACS rates are analysed for burst-like emission using a nova model light-curve. For the obtained nova flash candidate events, we discuss possible origins. No significant excess for the expected gamma-ray lines is found. Our upper limits on the synthesised Be-7 and Na-22 mass depend on the uncertainties of the distance to the nova: The Be-7 mass is constrained to less than $4.8\times10^{-9}\,(d/kpc)^2$, and Na-22 to less than $2.4\times10^{-8}\,(d/kpc)^2$ solar masses. For the Be-7 mass estimate from UV studies, the distance to V5668 Sgr must be larger than 1.2 kpc. During three weeks before the optical maximum, we find 23 burst-like events in the ACS rate, of which six could possibly be associated with V5668 Sgr., Comment: 11 pages, 7 figures, 1 table, accepted by A&A

Published
2018
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20. The e-ASTROGAM mission: Exploring the extreme Universe with gamma rays in the MeV – GeV range

Author

Barbara Patricelli, V. Bonvicini, Riccardo Rando, Sandro Mereghetti, Andrea Vacchi, Kazuhiro Nakazawa, Claudio Labanti, Jordi Isern, M. Hayashida, Josep M. Paredes, J. Eric Grove, C. Hamadache, Andreas Zoglauer, Olivier Limousin, Julie McEnery, Andrei M. Bykov, G. Ambrosi, D. de Martino, Francesco Longo, Irfan Kuvvetli, Alexander Moiseev, Xin Wu, Fabrizio Tavecchio, I. Donnarumma, M. I. Martínez, Marco Tavani, J. Peyré, Elisa Bernardini, A. Argan, Roland Walter, J. Kiener, Piotr Orleanski, Mark Pearce, Ignasi Reichardt, A. Morselli, Andrzej A. Zdziarski, Martino Marisaldi, Vincent Tatischeff, Andrea Bulgarelli, Marica Branchesi, Uwe Oberlack, Rui Curado da Silva, Dieter H. Hartmann, Lorraine Hanlon, Philippe Laurent, Marco Ajello, D. Bernard, Valentina Fioretti, Martin Pohl, Alessio Aboudan, Gottfried Kanbach, Alessandro De Angelis, Gabriele Ghisellini, Stefan Funk, Peter von Ballmoos, Michele Doro, M. N. Mazziotta, Marco Roncadelli, Harald Ramarijaona, Roland Diehl, Margarita Hernanz, Alexei Ulyanov, G. Minervini, G. Piano, Riccardo Campana, Carl Budtz-Jørgensen, D. J. Thompson, M. Cardillo, Paolo De Coppi, Karl Mannheim, Roberto Turolla, Jürgen Knödlseder, Isabelle Grenier, A. Brogna, De Angelis, A., Tatischeff, V., Tavani, M., Oberlack, U., Grenier, I., Hanlon, L., Walter, R., Argan, A., von Ballmoos, P., Bulgarelli, A., Donnarumma, I., Hernanz, M., Kuvvetli, I., Pearce, M., Zdziarski, A., Aboudan, A., Ajello, M., Ambrosi, G., Bernard, D., Bernardini, E., Bonvicini, V., Brogna, A., Branchesi, M., Budtz-Jorgensen, C., Bykov, A., Campana, R., Cardillo, M., Coppi, P., De Martino, D., Diehl, R., Doro, M., Fioretti, V., Funk, S., Ghisellini, G., Grove, E., Hamadache, C., Hartmann, D. H., Hayashida, M., Isern, J., Kanbach, G., Kiener, J., Knödlseder, J., Labanti, C., Laurent, P., Limousin, O., Longo, F., Mannheim, K., Marisaldi, M., Martinez, M., Mazziotta, M. N., Mcenery, J., Mereghetti, S., Minervini, G., Moiseev, A., Morselli, A., Nakazawa, K., Orleanski, P., Paredes, J. M., Patricelli, B., Peyré, J., Piano, G., Pohl, M., Ramarijaona, H., Rando, R., Reichardt, I., Roncadelli, M., Silva, R., Tavecchio, F., Thompson, D. J., Turolla, R., Ulyanov, A., Vacchi, A., Wu, X., Zoglauer, A., and ITA

Subjects
Counterparts of gravitational wave, Multiwavelength Observations of the Universe, 01 natural sciences, Early Universe, Observatory, Jets, Nuclear Astrophysics, Nuclear astrophysics, Dark Matter, Nuclear Experiment (nucl-ex), Nuclear Astrophysic, Nuclear Experiment, 010303 astronomy & astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::Instrumentation and Methods for Astrophysics, Counterparts of gravitational waves, Gamma-Ray Burst, Cosmic Rays, Compton and Pair Creation Telescope, Supernovae, Astrophysics - Solar and Stellar Astrophysics, High-Energy Astrophysics, Active Galactic Nuclei, Cosmic Antimatter, Fermi, Gamma-Ray Bursts, High-Energy Gamma-Ray Astronomy, Nucleosynthesis, Outflows, Astronomy and Astrophysics, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Active galactic nucleus, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Cosmic Ray, High-Energy Astrophysic, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Nucleosynthesi, 010308 nuclear & particles physics, Institut für Physik und Astronomie, Astronomy, Outflow, Astronomy and Astrophysic, Universe, Galaxy, Jet, Fermi Gamma-ray Space Telescope
Abstract

e-ASTROGAM (`enhanced ASTROGAM') is a breakthrough Observatory mission dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. In the largely unexplored MeV-GeV domain, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on Galactic ecosystems. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and the promise of eLISA. Keywords: High-energy gamma-ray astronomy, High-energy astrophysics, Nuclear Astrophysics, Compton and Pair creation telescope, Gamma-ray bursts, Active Galactic Nuclei, Jets, Outflows, Multiwavelength observations of the Universe, Counterparts of gravitational waves, Fermi, Dark Matter, Nucleosynthesis, Early Universe, Supernovae, Cosmic Rays, Cosmic antimatter., Comment: Exp Astron (2017)

Published
2017

21. STROBE-X: X-Ray Timing and Spectroscopy on Dynamical Timescales from Microseconds to Years

Author

Silvia Zane, Keith C. Gendreau, Margarita Hernanz, Thomas J. Maccarone, Marco Feroci, C. Michelle Hui, Paul S. Ray, Kent S. Wood, Ron Remillard, Zaven Arzoumanian, P. A. Jenke, Søren Brandt, Deepto Chakrabarty, and Colleen A. Wilson-Hodge

Subjects
Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, X-ray timing, FOS: Physical sciences, General Physics and Astronomy, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Missions, 010309 optics, General Relativity and Quantum Cosmology, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spectral resolution, Spectroscopy, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Compact objects, Astrophysics::Galaxy Astrophysics, Physics, X-ray spectroscopy, Supermassive black hole, Strong gravity, lcsh:QC1-999, Microsecond, Astrophysics - Instrumentation and Methods for Astrophysics, lcsh:Physics
Abstract

The Spectroscopic Time-Resolving Observatory for Broadband Energy X-rays (STROBE-X) probes strong gravity for stellar mass to supermassive black holes and ultradense matter with unprecedented effective area, high time-resolution, and good spectral resolution, while providing a powerful time-domain X-ray observatory., Accepted for Publication in Results in Physics

Published
2017
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22. Bright radio emission from an ultraluminous stellar-mass microquasar in M 31

Author

Massimo Della Valle, Despina Hatzidimitriou, Rob Fender, Natasha Hurley-Walker, James Miller-Jones, David Titterington, Geoffrey C. Bower, Mark Gurwell, Sera Markoff, Margarita Hernanz, Matthew Middleton, Michael Freyberg, Arne Rau, Anna M. M. Scaife, Chris Done, Dominic J. Walton, Junayd Miah, Hugh Dickinson, Gloria Sala, Dieter H. Hartmann, P. A. Charles, John Morgan, Jochen Greiner, John M. Carpenter, Pablo Reig, M. K. Daniel, Frank Haberl, Wolfgang Pietsch, Vadim Burwitz, Martin Henze, Marina Orio, J. Harris, A. Riffeser, Timothy P.L. Roberts, Jean-Pierre Macquart, Stella Seitz, Keith Grainge, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Multidisciplinary, Active galactic nucleus, Stellar mass, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Accretion (astrophysics), Interstellar medium, Black hole, symbols.namesake, X-shaped radio galaxy, 0103 physical sciences, Eddington luminosity, symbols, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

A subset of ultraluminous X-ray sources (those with luminosities < 10^40 erg/s) are thought to be powered by the accretion of gas onto black holes with masses of ~5-20 M_solar, probably via an accretion disc. The X-ray and radio emission are coupled in such Galactic sources, with the radio emission originating in a relativistic jet thought to be launched from the innermost regions near the black hole, with the most powerful emission occurring when the rate of infalling matter approaches a theoretical maximum (the Eddington limit). Only four such maximal sources are known in the Milky Way, and the absorption of soft X-rays in the interstellar medium precludes determining the causal sequence of events that leads to the ejection of the jet. Here we report radio and X-ray observations of a bright new X-ray source whose peak luminosity can exceed 10^39 erg/s in the nearby galaxy, M31. The radio luminosity is extremely high and shows variability on a timescale of tens of minutes, arguing that the source is highly compact and powered by accretion close to the Eddington limit onto a stellar mass black hole. Continued radio and X-ray monitoring of such sources should reveal the causal relationship between the accretion flow and the powerful jet emission., 23 pages, 4 figures accepted by Nature (AOP 12/12/12)

Published
2013

23. The e-ASTROGAM gamma-ray space mission

Author

Andrei M. Bykov, A. De Angelis, Dieter H. Hartmann, Sheila McBreen, Uwe Oberlack, M. Cardillo, C. Pittori, D. Bernard, Sandro Mereghetti, Francesco Longo, Philippe Laurent, Jürgen Knödlseder, R. Walter, Andreas Zoglauer, Valentina Fioretti, Marco Tavani, S. Sabatini, A. Brogna, Martino Marisaldi, C. Labanti, Jordi Isern, Kazuhiro Nakazawa, J. Peyré, Paolo Coppi, Julie McEnery, A. Morselli, J. Kiener, Lorraine Hanlon, G. Piano, Andrzej A. Zdziarski, Xin Wu, A. Argan, Andrea Bulgarelli, Riccardo Campana, D. J. Thompson, P. A. Caraveo, Margarita Hernanz, Alessio Aboudan, P. von Ballmoos, F. Mirabel, I. Donnarumma, V. Tatischeff, I. A. Grenier, Olivier Limousin, G. Kanbach, Roland Diehl, Alexei Ulyanov, J. E. Grove, L. Stawarz, A. Giuliani, C. Hamadache, Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Centre de Sciences Nucléaires et de Sciences de la Matière ( CSNSM ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Leprince-Ringuet ( LLR ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -École polytechnique ( X ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Jan-Willem A. den Herder, Tadayuki Takahashi, Marshall Bautz, Tatischeff, V., Tavani, M., Von Ballmoos, P., Hanlon, L., Oberlack, U., Aboudan, A., Argan, A., Bernard, D., Brogna, A., Bulgarelli, A., Bykov, A., Campana, R., Caraveo, P., Cardillo, M., Coppi, P., De Angelis, A., Diehl, R., Donnarumma, I., Fioretti, V., Giuliani, A., Grenier, I., Grove, J. E., Hamadache, C., Hartmann, D., Hernanz, M., Isern, J., Kanbach, G., Kiener, J., Knodlseder, J., Labanti, C., Laurent, P., Limousin, O., Longo, F., Marisaldi, M., Mcbreen, S., Mcenery, J. E., Mereghetti, S., Mirabel, F., Morselli, A., Nakazawa, K., Peyre, J., Piano, G., Pittori, C., Sabatini, S., Stawarz, L., Thompson, D. J., Ulyanov, A., Walter, R., Wu, X., Zdziarski, A., Zoglauer, A., Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Compton and pair creation telescope, Gamma-ray astronomy, gamma-ray polarization, high-energy astrophysical phenomena, space mission, time-domain astronomy, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Dark matter, Observatories, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Polarization, 0103 physical sciences, Galaxy groups and clusters, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Supermassive black hole, Active galactic nuclei, 010308 nuclear & particles physics, Sensors, Galactic Center, Galaxy, Particle accelerators, Neutron star, Gamma radiation, Chemicals, Electronics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope, Telescopes
Abstract

The e-ASTROGAM is a gamma-ray space mission to be proposed as the M5 Medium-size mission of the European Space Agency. It is dedicated to the observation of the Universe with unprecedented sensitivity in the energy range 0.2 - 100 MeV, extending up to GeV energies, together with a groundbreaking polarization capability. It is designed to substantially improve the COMPTEL and Fermi sensitivities in the MeV-GeV energy range and to open new windows of opportunity for astrophysical and fundamental physics space research. e-ASTROGAM will operate as an open astronomical observatory, with a core science focused on (1) the activity from extreme particle accelerators, including gamma-ray bursts and active galactic nuclei and the link of jet astrophysics to the new astronomy of gravitational waves, neutrinos, ultra-high energy cosmic rays, (2) the high-energy mysteries of the Galactic center and inner Galaxy, including the activity of the supermassive black hole, the Fermi Bubbles, the origin of the Galactic positrons, and the search for dark matter signatures in a new energy window; (3) nucleosynthesis and chemical evolution, including the life cycle of elements produced by supernovae in the Milky Way and the Local Group of galaxies. e-ASTROGAM will be ideal for the study of high-energy sources in general, including pulsars and pulsar wind nebulae, accreting neutron stars and black holes, novae, supernova remnants, and magnetars. And it will also provide important contributions to solar and terrestrial physics. The e-ASTROGAM telescope is optimized for the simultaneous detection of Compton and pair-producing gamma-ray events over a large spectral band. It is based on a very high technology readiness level for all subsystems and includes many innovative features for the detectors and associated electronics., 11 pages, 5 figures, published in the proceedings of SPIE Astronomical Telescopes and Instrumentation: Ultraviolet to Gamma Ray conference, Edinburgh 2016. Addition of an acknowledgment statement in version 2

Published
2016
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24. Classical Novae as Supersoft X-ray Sources in the Andromeda Galaxy

Author

Gloria Sala, Dieter H. Hartmann, Massimo Della Valle, Despina Hatzidimitriou, Arne Rau, Frank Haberl, Wolfgang Pietsch, Margarita Hernanz, Martin Henze, Vadim Burwitz, and Jochen Greiner

Subjects
Physics, education.field_of_study, Andromeda Galaxy, Population, White dwarf, Astronomy, Cataclysmic variable star, Astronomy and Astrophysics, Astrophysics, Central region, Luminosity, Space and Planetary Science, Binary system, Variable star, education
Abstract

We review the first results of a dedicated, on-going monitoring project for supersoft X-ray source (SSS) states of classical novae (CNe) in the central region of the Andromeda galaxy (M 31). So far, during three high-cadence observation campaigns with the X-ray telescopes XMM-Newton and Chandra from 2006 until 2009 we detected 21 CNe, only four of which were seen in X-rays before. This increased the total number of known CNe with X-ray counterparts in M 31 to 60, which is significantly larger than for any other galaxy, including the Milky Way. We compiled a catalog of X-ray and optical properties for these 60 sources which allowed us to perform source statistics and population studies of CNe with SSS state in M 31 for the first time. Here we review the results of this analysis: (i) several correlations between X-ray and optical parameters, (ii) an analysis of the intrinsic fraction of CNe with SSS state, and (iii) the first nova population study in X-rays. Our first results are promising, however a continuing monitoring of the unique target M 31 is strongly needed to extend this valuable data base and to refine the early statements and predictions.

Published
2011
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25. The first two transient supersoft X-ray sources in M 31 globular clusters and the connection to classical novae

Author

M. Della Valle, Albert K. H. Kong, K. Hornoch, Vadim Burwitz, Robert Quimby, Jochen Greiner, Martin Henze, Margarita Hernanz, Peter A. Milne, G. Grant Williams, Gloria Sala, Frank Haberl, Wolfgang Pietsch, Holger Stiele, and Dieter H. Hartmann

Subjects
Physics, Astrophysics (astro-ph), X-ray, FOS: Physical sciences, White dwarf, Astronomy and Astrophysics, Astrophysics, EPIC, Light curve, Galaxy, Spectral line, SSS, Space and Planetary Science, Globular cluster
Abstract

Classical novae (CNe) have been found to represent the major class of supersoft X-ray sources (SSS) in our neighbour galaxy M 31. We determine properties and evolution of the two first SSSs ever discovered in the M 31 globular cluster (GC) system. We have used XMM-Newton, Chandra and Swift observations of the centre region of M 31 to discover both SSS and to determine their X-ray light curves and spectra. We performed detailed analysis of XMM-Newton EPIC PN spectra of the source in Bol 111 (SS1) using blackbody and NLTE white dwarf (WD) atmosphere models. For the SSS in Bol 194 (SS2) we used optical monitoring data to search for an optical counterpart. Both GC X-ray sources were classified as SSS. We identify SS1 with the CN M31N 2007-06b recently discovered in the M 31 GC Bol 111. For SS2 we did not find evidence for a recent nova outburst and can only provide useful constraints on the time of the outburst of a hypothetical nova. The only known CN in a M 31 GC can be identified with the first SSS found in a M31 GC. We discuss the impact of our observations on the nova rate for the M 31 GC system., Comment: 11 pages, 9 figures, 4 tables, submitted to A&A; v2: accepted version

Published
2009
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26. V5116 Sagittarii, an Eclipsing Supersoft Postoutburst Nova?

Author

Gloria Sala, Carlo Ferri, Jochen Greiner, and Margarita Hernanz

Subjects
Atmosphere, Physics, Space and Planetary Science, White dwarf, Flux, Astronomy and Astrophysics, Black-body radiation, Nova (laser), Astrophysics, Orbital period, Atmospheric temperature, Spectral line
Abstract

V5116 Sgr (Nova Sgr 2005 No. 2), discovered on 2005 July 4, was observed with XMM-Newton in March 2007, 20 months after the optical outburst. The X-ray spectrum shows that the nova had evolved to a pure supersoft X-ray source, with no significant emission at energies above 1 keV. The X-ray light-curve shows abrupt decreases and increases of the flux by a factor ~8. It is consistent with a periodicity of 2.97 h, the orbital period suggested by Dobrotka et al. (2007), although the observation lasted just a little more than a whole period. We estimate the distance to V5116 Sgr to be 11+/-3 kpc. A simple blackbody model does not fit correctly the EPIC spectra, with reduced chi^2>4. In contrast, ONe rich white dwarf atmosphere models provide a good fit, with nH=1.3(+/-0.1)e21 cm^-2, T=6.1(+/-0.1)e5 K, and L=3.9(+/-0.8)e37(D/10kpc)^2 erg/s (during the high-flux periods). This is consistent with residual hydrogen burning in the white dwarf envelope. The white dwarf atmosphere temperature is the same both in the low and the high flux periods, ruling out an intrinsic variation of the X-ray source as the origin of the flux changes. We speculate that the X-ray light-curve may result from a partial coverage by an asymmetric accretion disk in a high inclination system.

Published
2008
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27. Gamma-Ray emission from SN2014J near maximum optical light

Author

Jürgen Knödlseder, G. Vedrenne, Rashid Sunyaev, G. G. Lichti, Simona Soldi, A. Domingo, Matthieu Renaud, P. von Ballmoos, Jordi Isern, E. M. Churazov, Inmaculada Domínguez, F. Lebrun, P. Hoeflich, C. Badenes, Domingo García-Senz, P. Jean, Nancy Elias-Rosa, Margarita Hernanz, Eduardo Bravo, Dieter H. Hartmann, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GRPFM - Grup de Recerca en Propietats Físiques dels Materials, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire Univers et Particules de Montpellier ( LUPM ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Université de Montpellier ( UM )

Subjects
Thermonuclear fusion, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, individual: SN2014J / gamma rays: stars [supernovae], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, supernovae: individual: SN2014J, gamma rays: stars, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Ejecta, 010303 astronomy & astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Solar mass, 010308 nuclear & particles physics, Supernoves, Gamma ray, White dwarf, Astronomy and Astrophysics, Light curve, Supernova, Supernovae, 13. Climate action, Space and Planetary Science, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Radioactive decay
Abstract

Context. The optical light curve of Type Ia supernovae (SNIa) is powered by thermalized gamma-rays produced by the decay of 56Ni and 56Co, the main radioactive isotopes synthesized by the thermonuclear explosion of a C/O white dwarf. Aims: Gamma-rays escaping the ejecta can be used as a diagnostic tool for studying the characteristics of the explosion. In particular, it is expected that the analysis of the early gamma emission, near the maximum of the optical light curve, could provide information about the distribution of the radioactive elements in the debris. Methods: The gamma data obtained from SN2014J in M 82 by the instruments on board INTEGRAL were analysed paying special attention to the effect that the detailed spectral response has on the measurements of the intensity of the lines. Results: The 158 keV emission of 56Ni has been detected in SN2014J at ~5σ at low energy with both ISGRI and SPI around the maximum of the optical light curve. After correcting the spectral response of the detector, the fluxes in the lines suggest that, in addition to the bulk of radioactive elements buried in the central layers of the debris, there is a plume of 56Ni, with a significance of ~3σ, moving at high velocity and receding from the observer. The mass of the plume is in the range of ~0.03-0.08 Msun. Conclusions: No SNIa explosion model has ever predicted the mass and geometrical distribution of 56Ni suggested here. According to its optical properties, SN2014J looks like a normal SNIa, so it is extremely important to discern whether it is also representative in the gamma-ray band. Based on observations with INTEGRAL, an ESA project with instruments and the science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland, and Spain), the Czech Republic, and Poland and with the participation of Russia and USA.

Published
2016
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28. Large Observatory for x-ray Timing (LOFT-P): a Probe-class mission concept study

Author

S. Korpela, Luigi Stella, M. Michalska, Stéphane Schanne, Randall C. Hopkins, Berend Winter, Robert Hickman, Billy Carson, Andrea Santangelo, Bert Gangl, Marco Feroci, Chris Becker, Jay Garcia, Silvia Zane, A. Domínguez, Thomas J. Maccarone, Laura Alvarez, Michelle Hui, Luster Ingram, Leo Fabisinski, Peter Jenke, Margarita Hernanz, Paul S. Ray, Enrico Bozzo, Søren Brandt, Christopher V. Griffith, Martin Pohl, Michiel van der Klis, Michael Baysinger, Anna L. Watts, Andrew Schnell, Deepto Chakrabarty, Jack Chapman, Colleen A. Wilson-Hodge, High Energy Astrophys. & Astropart. Phys (API, FNWI), den Herder, Jan-Willem A., Takahashi, Tadayuki, and Bautz, Marshall

Subjects
Equation of state, Event horizon, Computer science, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Mission Concepts, FOS: Physical sciences, Silicon Drift Detectors, 01 natural sciences, Neutron stars, Observatory, 0103 physical sciences, Spectral resolution, Spectroscopy, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, media_common, 010308 nuclear & particles physics, Black holes, Strong gravity, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Black hole, Interferometry, Neutron star, Sky, Astrophysics - Instrumentation and Methods for Astrophysics, X-ray Timing
Abstract

LOFT-P is a concept for a NASA Astrophysics Probe-Class (6 m^2, >10x RXTE), high time resolution, good spectral resolution, broad-band spectral coverage (2-30 keV), highly flexible scheduling, and an ability to detect and respond promptly to time-critical targets of opportunity. It addresses science questions such as: What is the equation of state of ultra dense matter? What are the effects of strong gravity on matter spiraling into black holes? It would be optimized for sub-millisecond timing to study phenomena at the natural timescales of neutron star surfaces and black hole event horizons and to measure mass and spin of black holes. These measurements are synergistic to imaging and high-resolution spectroscopy instruments, addressing much smaller distance scales than are possible without very long baseline X-ray interferometry, and using complementary techniques to address the geometry and dynamics of emission regions. A sky monitor (2-50 keV) acts as a trigger for pointed observations, providing high duty cycle, high time resolution monitoring of the X-ray sky with ~20 times the sensitivity of the RXTE All-Sky Monitor, enabling multi-wavelength and multi-messenger studies. A probe-class mission concept would employ lightweight collimator technology and large-area solid-state detectors, technologies which have been recently greatly advanced during the ESA M3 study. Given the large community interested in LOFT (>800 supporters, the scientific productivity of this mission is expected to be very high, similar to or greater than RXTE (~2000 refereed publications). We describe the results of a study, recently completed by the MSFC Advanced Concepts Office, that demonstrates that LOFT-P is feasible within a NASA probe-class mission budget., Comment: Proc. SPIE 9905, Space Telescopes and Instrumentation 2016: Ultraviolet to Gamma Ray, 99054Y (July 18, 2016)

Published
2016
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29. Nucleosynthesis in classical nova explosions

Author

Jordi José and Margarita Hernanz

Subjects
Physics, Nuclear and High Energy Physics, Nucleosynthesis, Astrophysics::High Energy Astrophysical Phenomena, Nuclear astrophysics, Astrophysics::Solar and Stellar Astrophysics, Astronomy, Astrophysics, Nova (laser), Astrophysics::Galaxy Astrophysics, Cosmochemistry
Abstract

Classical novae are fascinating stellar explosions at the crossroads of stellar astrophysics, nuclear physics, and cosmochemistry. In this review, we briefly summarize 30 years of nucleosynthesis studies, with special emphasis on recent advances in nova theory (including multidimensional models) as well as on experimental efforts to reduce nuclear uncertainties affecting critical reaction rates. Among the topics that are covered, we outline the interplay between nova outbursts and the galactic chemical abundances, the synthesis of radioactive nuclei of interest for γ-ray astronomy, such as 7Li, 22Na or 26Al, and the potential discovery of presolar meteoritic grains likely condensed in nova shells.

Published
2007
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30. The origin of presolar nova grains

Author

Margarita Hernanz and Jordi José

Subjects
Murchison meteorite, Physics, Interstellar medium, Supernova, Geophysics, Meteorite, Space and Planetary Science, Nucleosynthesis, Presolar grains, Astronomy, Astrophysics, Nova (laser)
Abstract

Infrared observations reveal that classical novae often form dust in their expanding shells ejected into the interstellar medium as a consequence of violent outbursts. Recent experimental efforts have led to the identification of presolar nova candidate grains from the Acfer 094 and Murchison meteorites. Recently, however, concerns have been raised about the stellar paternity of these grains by new measurements on another sample of SiC grains: these grains are characterized by 12C/13C and 14N/15N ratios similar to the ones reported for the nova grains, but a number of different imprints suggest that a possible supernova origin cannot be excluded. Here we review the predicted nucleosynthetic imprints accompanying nova explosions and discuss the chances to synthesize heavier species, such as titanium, in nova-like events.

Published
2007
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31. The First Nova Explosions

Author

Enrique García-Berro, Margarita Hernanz, Jordi José, and Pilar Gil-Pons

Subjects
Physics, Astrophysics and Astronomy, Presolar grains, Extinction (astronomy), Cataclysmic variable star, Astronomy, Astronomy and Astrophysics, Nova (laser), Astrophysics, Galaxy, Supernova, Space and Planetary Science, Nucleosynthesis, Circumstellar dust, Ejecta, Geology
Abstract

Classical novae are stellar explosions with an energy release that is only overcome by supernovae and γ-ray bursts. Theoretical and observational evidence suggests that these cataclysmic events are major sources of the Galactic 15N, 17O, and 13C, and contribute to the abundances of 7Li, and 26Al, with a likely nucleosynthetic endpoint around Ca. However, there are reasons to believe that these nuclear signatures have changed during the overall Galactic history. In this Letter, the first that addresses the nature of nova explosions in the most primitive, low-metallicity binaries, we show that primordial novae eject more massive envelopes and display a larger nuclear activity than classical novae, leading to a new type of explosion, halfway between a supernova and a nova. The ejected shells from the most violent, massive primordial novae yield large excesses of Ti and a likely nucleosynthetic endpoint around Cu-Zn, signatures never before associated with a nova-like explosion. We conclude that the chemical abundance pattern of the nova ejecta is strongly modified at low metallicities and suggest that primordial novae are a possible birthplace of a rare variety of presolar grains whose origin remains uncertain.

Published
2007
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32. A remarkable recurrent nova in M31:discovery and optical/UV observations of the predicted 2014 eruption

Author

M. J. Darnley, Pablo Rodríguez-Gil, A. S. Piascik, Martin Henze, Seiichiro Kiyota, Rebekah Hounsell, Hana Kučáková, Steven Williams, M. F. Bode, Marek Wolf, Iain A. Steele, Jan-Uwe Ness, Valério A. R. M. Ribeiro, Robert J. Smith, Mariko Kato, Hiroyuki Maehara, Izumi Hachisu, Gloria Sala, D. Baer, A. W. Shafter, Margarita Hernanz, K. Hornoch, I. Skillen, Universitat Politècnica de Catalunya. Departament de Física, and Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica

Subjects
Swift Gamma-Ray Burst Mission, Andromeda Galaxy, Red giant, Astronomy, FOS: Physical sciences, Astrophysics, CLASSICAL NOVAE, Photometry (optics), RS-OPHIUCHI, T-PYXIDIS, Ejecta, individual: M31 [galaxies], Solar and Stellar Astrophysics (astro-ph.SR), QB, Physics, novae, LIGHT CURVES, cataclysmic variables, 2006 OUTBURST, White dwarf, Astronomy and Astrophysics, WHITE-DWARF, Stars, X-RAY OBSERVATIONS, CURRENTLY FORMING STARS, Estels, Supernova, individual: M31N 2008-12a [stars], Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, High mass, LARGE-MAGELLANIC-CLOUD, LOCAL GROUP
Abstract

The Andromeda Galaxy recurrent nova M31N 2008-12a had been caught in eruption eight times. The inter-eruption period of M31N 2008-12a is ~1 year, making it the most rapidly recurring system known, and a strong single-degenerate Type Ia Supernova progenitor candidate. Following the 2013 eruption, a campaign was initiated to detect the predicted 2014 eruption and to then perform high cadence optical photometric and spectroscopic monitoring using ground-based telescopes, along with rapid UV and X-ray follow-up with the Swift satellite. Here we report the results of a high cadence multicolour optical monitoring campaign, the spectroscopic evolution, and the UV photometry. We also discuss tantalising evidence of a potentially related, vastly-extended, nebulosity. The 2014 eruption was discovered, before optical maximum, on October 2, 2014. We find that the optical properties of M31N 2008-12a evolve faster than all Galactic recurrent novae known, and all its eruptions show remarkable similarity both photometrically and spectroscopically. Optical spectra were obtained as early as 0.26 days post maximum, and again confirm the nova nature of the eruption. A significant deceleration of the inferred ejecta expansion velocity is observed which may be caused by interaction of the ejecta with surrounding material, possibly a red giant wind. We find a low ejected mass and low ejection velocity, which are consistent with high mass-accretion rate, high mass white dwarf, and short recurrence time models of novae. We encourage additional observations, especially around the predicted time of the next eruption, towards the end of 2015., 23 pages, 11 figures, 5 tables, accepted for publication in Astronomy & Astrophysics

Published
2015
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34. The Imprint of Nova Nucleosynthesis in Presolar Grains

Author

Sachiko Amari, Jordi José, Margarita Hernanz, Ernst Zinner, and Katharina Lodders

Subjects
Physics, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Presolar grains, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Nova (laser), Light curve, Interstellar medium, Meteorite, Space and Planetary Science, Nucleosynthesis, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Ejecta
Abstract

Infrared and ultraviolet observations of nova light curves have confirmed grain formation in their expanding shells that are ejected into the interstellar medium by a thermonuclear runaway. In this paper, we present isotopic ratios of intermediate-mass elements up to silicon for the ejecta of CO and ONe novae, based on 20 hydrodynamic models of nova explosions. These theoretical estimates will help to properly identify nova grains in primitive meteorites. In addition, equilibrium condensation calculations are used to predict the types of grains that can be expected in the nova ejecta, providing some hints on the puzzling formation of C-rich dust in O>C environments. These results show that SiC grains can condense in ONe novae, in concert with an inferred (ONe) nova origin for several presolar SiC grains., 42 pages. Accepted for publication in The Astrophysical Journal

Published
2004
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35. γ-rays from classical novae: expectations from present and future missions

Author

Jordi José and Margarita Hernanz

Subjects
Physics, Long lasting, Annihilation, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy, Astronomy and Astrophysics, Astrophysics, Electron, Supernova, Positron, Space and Planetary Science, Observatory, Nucleosynthesis
Abstract

A review of the main features of the γ-ray emission of individual classical novae is presented. We concentrate on the theoretical predictions of both the long lasting emission, produced by electron captures on 7 Be and β + -decay of 22 Na, and the prompt emission, produced by electron–positron annihilation (with positrons coming from 13 N and 18 F β + -decays). Special attention is paid to the observability of novae with the current INTEGRAL observatory and with future missions, like EXIST.

Published
2004
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36. The Impact of the Chemical Stratification of White Dwarfs on the Classification of Classical Novae

Author

Pilar Gil-Pons, Jordi José, Enrique García-Berro, and Margarita Hernanz

Subjects
Physics, Isotopes of neon, Space and Planetary Science, Nucleosynthesis, Astrophysics (astro-ph), FOS: Physical sciences, White dwarf, Stratification (water), Astronomy and Astrophysics, Astrophysics, Ejecta
Abstract

We analyse the impact of the initial abundances of the underlying white dwarf core on the nucleosynthesis accompanying classical nova outbursts, in the framework of hydrodynamic models of the explosion. Specifically, we take into account the chemical stratification of the white dwarf. It turns out that the presence of a thick CO-buffer on top of the ONe-rich core, as results from detailed calculations of previous evolution of the progenitor star, may lead to significant amounts of both 7Li and 26Al, after an outburst that, due to the lack of neon isotopes in the ejecta, would be misclassified as a non-neon nova (i.e., CO nova)., Accepted for publication in The Astrophysical Journal Letters

Published
2003
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37. The impact of the chemical stratification of white dwarfs on the nucleosynthesis from classical novae

Author

Enrique García–Berro, Margarita Hernanz, and Jordi José

Subjects
Physics, Nuclear and High Energy Physics, Isotopes of neon, Nucleosynthesis, White dwarf, Stratification (water), Astronomy, Astrophysics, Ejecta
Abstract

In the framework of hydrodynamic calculations of the nova outburst, we analyse the impact of the initial abundances on the composition of the ejecta, by taking into account the chemical stratification of the white dwarf. It turns out that the presence of a CO-buffer on top of an ONe core may lead to significant amounts of both 7 Li and 26 Al simultaneously in an explosionn that, due to the lack of neon isotopes, would be misclassified as a CO nova.

Published
2003
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38. Constraining Models of Classical Nova Outbursts with the Murchison Meteorite

Author

Sachiko Amari, Margarita Hernanz, Jordi José, and Ernst Zinner

Subjects
Murchison meteorite, Physics, Interstellar medium, Meteoroid, Meteorite, Space and Planetary Science, Nucleosynthesis, Presolar grains, Astronomy, Astronomy and Astrophysics, Nova (laser), Astrophysics, Light curve
Abstract

Infrared observations of nova light curves reveal that classical novae form grains in the expanding shells, ejected into the interstellar medium as a consequence of a violent outburst. Such grains contain nucleo-synthetic fingerprints of the nova explosion. In this paper, we analyse different isotopic signatures expected to be present in nova grains on the basis of detailed hydrodynamic calculations of CO and ONe novae and compare them with recent determinations of presolar nova grains from the Acfer 094 and Murchison meteorites.

Published
2003
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39. A false positive for clozapine using high-pressure liquid chromatography with ultraviolet detection

Author

Saioa Domingo Echaburu, Manuel Martinez, Unax Lertxundi, and Margarita Hernanz Manrique

Subjects
Psychiatry and Mental health, medicine.medical_specialty, Internal medicine, medicine, Test request, Pharmacology, Psychology, Gastroenterology, High-performance liquid chromatography, Biological Psychiatry, Clozapine, medicine.drug
Abstract

Background:We report a case of a false positive for clozapine, when analysing serum levels using a high-pressure liquid chromatography with ultraviolet (HPLC-UV) detection method.Methods:A patient not taking clozapine tested positive for clozapine three times in two different samples. This false positive was discovered by chance, because of an administrative error made in the first analytic test request.Results:The analysis of the first sample with a more specific method [HPLC-tandem mass spectrometry (LC-MS/MS)] showed that no clozapine was present.Conclusions:It is important to acknowledge that depending on the method employed, a false positive should not be ruled out as a possibility. Moreover, and even more worryingly, it should also be taken into account that clozapine serum levels could be tested erroneously high if the unknown interference is present and the HPLC-UV method is used. Although the interfering compound could not be identified, the possibility of a cross-reaction when analysing serum clozapine levels with the HPLC-UV method warrants urgent attention.

Published
2014

40. Galactic 1.275-MeV emission from ONe novae and its detectability by INTEGRAL/SPI

Author

J. Gómez-Gomar, Margarita Hernanz, Jordi José, and Pierre Jean

Subjects
Physics, Radionuclide, Photon, Spectrometer, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, White dwarf, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Nova (laser), Galaxy, Space and Planetary Science, Observatory, Astrophysics::Solar and Stellar Astrophysics, Radian, Astrophysics::Galaxy Astrophysics
Abstract

Models of Galactic 1.275-MeV emission produced by the decay of the radionuclide 22Na have been computed. Several frequency–spatial distributions of novae have been investigated using recent results of nova rates and spatial distributions of novae in our Galaxy. These models allow us to estimate the lower limit of the 22Na mass ejected per ONe nova detectable with the future spectrometer (SPI) of the INTEGRAL observatory as a function of the frequency–spatial distribution of ONe novae in the Galaxy. Calculations using recent estimations of the expected 22Na mass ejected per ONe nova show that the detection of the Galactic emission of 1.275-MeV photons will be difficult with the future spectrometer of the INTEGRAL observatory, whereas the cumulative emission around the Galactic Centre has some chance of being detected during the deep survey of the central radian of the Galaxy.

Published
2000
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41. Nuclear Uncertainties in the NeNa‐MgAl Cycles and Production of \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $^{22}$ \end{document} Na and \documentclass{aastex} \usepackage{amsbsy} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{bm} \usepackage{mathrsfs} \usepackage{pifont} \usepackage{stmaryrd} \usepackage{textcomp} \usepackage{portland,xspace} \usepackage{amsmath,amsxtra} \usepackage[OT2,OT1]{fontenc} \newcommand\cyr{ \renewcommand\rmdefault{wncyr} \renewcommand\sfdefault{wncyss} \renewcommand\encodingdefault{OT2} \normalfont \selectfont} \DeclareTextFontCommand{\textcyr}{\cyr} \pagestyle{empty} \DeclareMathSizes{10}{9}{7}{6} \begin{document} \landscape $^{26}$ \end{document} Al during Nova Outbursts

Author

Alain Coc, Margarita Hernanz, and Jordi José

Subjects
Physics, Nuclear reaction, Thermonuclear fusion, Accretion (meteorology), Isotope, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics, Nova (laser), 7. Clean energy, 01 natural sciences, Interstellar medium, 13. Climate action, Space and Planetary Science, 0103 physical sciences, 010303 astronomy & astrophysics
Abstract

Classical novae eject significant amounts of nuclear processed material into the interstellar medium. Among the isotopes synthesized during such explosions, two radioactive nuclei deserve a particular attention: 22Na and 26Al. In this paper, we investigate the nuclear paths leading to 22Na and 26Al production during nova outbursts by means of an implicit, hydrodynamic code that follows the course of the thermonuclear runaway from the onset of accretion up to the ejection stage. New evolutionary sequences of ONe novae have been computed, using updated nuclear reaction rates relevant to 22Na and 26Al production. Special attention is focused on the role played by nuclear uncertainties within the NeNa and MgAl cycles in the synthesis of such radioactive species. From the series of hydrodynamic models, which assume upper, recommended or lower estimates of the reaction rates, we derive limits on the production of both 22Na and 26Al. We outline a list of nuclear reactions which deserve new experimental investigations in order to reduce the wide dispersion introduced by nuclear uncertainties in the 22Na and 26Al yields.

Published
1999
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42. A lithium-rich stellar explosion

Author

Margarita Hernanz

Subjects
Physics, Multidisciplinary, chemistry, Milky Way, chemistry.chemical_element, Lithium, Astrophysics, Beryllium
Abstract

The contribution of explosions known as novae to the lithium content of the Milky Way is uncertain. Radioactive beryllium, which transforms into lithium, has been detected for the first time in one such explosion. See Letter p.381

Published
2015
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43. Gamma-ray emission from individual classical novae

Author

Jordi Isern, Margarita Hernanz, J. Gómez-Gomar, and Jordi José

Subjects
Physics, Annihilation, Photon, Spectrometer, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Gamma ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Electron, Light curve, Spectral line, Positron, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics
Abstract

Classical novae are important producers of radioactive nuclei, such as be7, n13, f18, na22 and al26. The disintegration of these nuclei produces positrons (except for be7) that through annihilation with electrons produce photons of energies 511 keV and below. Furthermore, be7 and na22 decay producing photons with energies of 478 keV and 1275 keV, respectively, well in the gamma-ray domain. Therefore, novae are potential sources of gamma-ray emission. The properties of gamma-ray spectra and gamma-ray light curves (for the continuum and for the lines at 511, 478 and 1275 keV) have been analyzed, with a special emphasis on the difference between carbon-oxygen and oxygen-neon novae. Predictions of detectability of individual novae by the future SPI spectrometer on board the INTEGRAL satellite are made., Accepted for publication in MNRAS, 9 pages, 9 figures. Revised version: only figure 2 has been changed

Published
1998
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44. Evolutionary calculations of carbon dredge-up in helium envelope white dwarfs

Author

James M. MacDonald, Jordi José, and Margarita Hernanz

Subjects
Physics, Opacity, Astrophysics (astro-ph), FOS: Physical sciences, White dwarf, chemistry.chemical_element, Astronomy and Astrophysics, Astrophysics, Effective temperature, Dredge-up, Atmosphere, chemistry, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Diffusion (business), Stellar evolution, Astrophysics::Galaxy Astrophysics, Helium
Abstract

We investigate the evolution of cooling helium atmosphere white dwarfs using a full evolutionary code, specifically developed for following the effects of element diffusion and gravitational settling on white dwarf cooling. The major difference between this work and previous work is that we use more recent opacity data from the OPAL project. Since, in general, these opacities are higher than those available ten years ago, at a given effective temperature, convection zones go deeper than in models with older opacity data. Thus convective dredge-up of observationally detectable carbon in helium atmosphere white dwarfs can occur for thicker helium layers than found by Pelletier et al (1986). We find that the range of observed C to He ratios in different DQ white dwarfs of similar effective temperature is well explained by a range of initial helium layer mass between $10^{-3}$ and $10^{-2} M_{\odot}$, in good agreement with stellar evolution theory, assuming a typical white dwarf mass of $0.6 M_{\odot}$. We also predict that oxygen will be present in DQ white dwarf atmospheres in detectable amounts if the helium layer mass is near the lower limit compatible with stellar evolution theory. Determination of the oxygen abundance has the potential of providing information on the profile of oxygen in the core and hence on the important $^{12}$C$(\alpha,\gamma)^{16}$O reaction rate., Comment: Accepted for publication in MNRAS, 8 pages, 6 figures

Published
1998
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45. The Large Observatory For x-ray Timing

Author

Antonios Manousakis, S. Boutloukos, F. Zwart, Jose M. Torrejon, C. Pittori, Alessandro Drago, Dieter H. Hartmann, Feryal Özel, T. J. L. Courvoisier, Tim Johannsen, Jordi José, M. Michalska, Christian Schmid, I. Rashevskaya, Gottfried Kanbach, V. Petracek, L. Bradley, Allan Hornstrup, M. H. Erkut, Sergio Campana, Rudy Wijnands, Andrew Cumming, Nils Andersson, Tomaso Belloni, M. C. Miller, Roman Wawrzaszek, Stefano Bianchi, Enrique García-Berro, Sandro Mereghetti, C. Guidorzi, C. Corral Van Damme, Søren Brandt, Francesco Tombesi, Felix Ryde, Didier Barret, Simon Vaughan, Marco Feroci, T. Di Salvo, C. van Baren, Angelo Antonelli, Marc Ribó, J. L. Atteia, P. Soleri, Alessio Trois, Silvia Zane, G. Mouret, Ersin Gogus, Emanuele Perinati, J. Coker, Piero Malcovati, V. Mangano, F. Jetter, P. Uter, P. Romano, M. Nowak, Roberto Turolla, Laura Tolos, Antonino D'Ai, Laura Alvarez, C. Amoros, Simone Scaringi, A. Possenti, David M. Smith, M. Falanga, A. Goldwurm, René Hudec, Ignacio Negueruela, M. van der Klis, Francesco Longo, José A. Pons, I. M. McHardy, R. Rohlfs, P. Cais, Luigi Stella, S. Di Cosimo, Antoine Rousseau, M. Ayre, M. Gschwender, D. Klochkov, Niels Lund, Chryssa Kouveliotou, P. Azzarello, F. Château, Michael Gabler, S. Vercellone, Martin Durant, I. Donnarumma, Giorgio Matt, Mauro Orlandini, P. Kaaret, Patrick Smith, P. T. O'Brien, A. Argan, M. Orienti, Marco Grassi, Claudio Labanti, Edward F. Brown, Christopher S. Reynolds, Gloria Sala, Y. Evangelista, Gabriel Török, José Braga, Riccardo Campana, Alan Smith, C. Gouiffes, Nevin N. Weinberg, Leonardo Gualtieri, Yannick Favre, P.G. Jonker, Gabriele Giovannini, D. de Martino, Irfan Kuvvetli, S. Motta, Teresa Mineo, Paul J. Groot, Pablo Reig, Martino Marisaldi, Andrea Sanna, Lorenzo Amati, G. L. Israel, D. Macera, K. S. Wood, Pablo Cerdá-Durán, F. Fuschino, Suvi Gezari, Mariano Mendez, Slawomir Suchy, Damien Rambaud, Nanda Rea, R. Artigue, J.-Y. Seyler, S. N. Shore, Frederick K. Lamb, Jörn Wilms, Mark G. Alford, Margarita Hernanz, Thomas M. Tauris, Luca Izzo, Tobias Boenke, J. J. M. in 't Zand, J. Mulačová, P. Binko, Daniel Maier, Jan Schee, Bruce Gendre, Enrico Bozzo, Paul S. Ray, Giuseppe Bertuccio, Simone Migliari, Ignazio Bombaci, Vladimir Karas, Nikolaos Stergioulas, P. P. Laubert, D. Karelin, A. C. Fabian, Giovanni Miniutti, Dacheng Lin, L. Guy, Martine Mouchet, Colleen A. Wilson-Hodge, Valeria Ferrari, Kai Hebeler, Mark H. Finger, Shigeto Watanabe, Pawel Haensel, H. Jacobs, Adrian Martindale, A. A. Zdziarski, Andrea Santangelo, Giuseppe Baldazzi, Piergiorgio Casella, Fabio Muleri, M. Hailey, Antonio Bianchini, Giuseppe Lodato, E. Del Monte, M. Rapisarda, Zdeněk Stuchlík, Alain Cros, V. Sochora, Laurens Keek, Jorge Casares, Andrew Melatos, Pere Blay, E. Rossi, A. P. Spencer, G. Stratta, Conrado Albertus, J. M. Paredes, M. Ahangarianabhari, Anna L. Watts, M. Del Santo, I. Kreykenbohm, Alessandro Patruno, G. A. Caliandro, C. Feldman, M. Pohl, Fabrizio Tamburini, G. Zampa, Marina Orio, Flemming Hansen, P. Ramon, Ruben Salvaterra, David H. Lumb, Edward M. Cackett, Andrew Shearer, Sharon M. Morsink, L. Pacciani, J.-M. Bonnet Bidaud, A. De Luca, Jérôme Chenevez, Sebastian Diebold, N. Zampa, Carole A. Haswell, Luciano Burderi, E. Cavazzuti, Adam Ingram, Dhiren Kataria, Berend Winter, A. Vacchi, W. Hermsen, P. Giommi, Dong Lai, N. A. Webb, P. Bodin, Dom Walton, Solen Balman, Benjamin Stappers, M. Burgay, Luca Zampieri, Carl Budtz-Jørgensen, Ralph A. M. J. Wijers, Giancarlo Cusumano, J. L. Galvez Sanchez, Raffaella Schneider, Luciano Rezzolla, Alexander Heger, S. Korpela, Dimitrios Emmanoulopoulos, Biswajit Paul, Diego Götz, B. Artigues, Paolo Soffitta, M. H. Finger, J. W. den Herder, Paolo Esposito, Kazushi Iwasawa, Poul Erik Holmdahl Olsen, J. Neilsen, Marco Barbera, Deepto Chakrabarty, R. A. Osten, M. Reina Aranda, A. J. Castro-Tirado, Andrea Tramacere, D. Haas, Johannes Dercksen, John A. Tomsick, A. V. Penacchioni, V. D'Elia, Alfonso Collura, Altan Baykal, P. Le Provost, S. Turriziani, Kostas D. Kokkotas, Duncan K. Galloway, Ron Remillard, Juhani Huovelin, Somak Bhattacharyya, Pavel Bakala, Phil Uttley, Richard E. Cole, Mahesh Prakash, L. Kuiper, T. Munoz-Darias, Diego F. Torres, S. Mahmoodifar, G. Ramsay, Andrew Norton, T. Kennedy, Achim Schwenk, L. Zdunik, A. B. Giles, Jerome Rodriguez, C. Motch, Ilya Mandel, Marcello Giroletti, Dimitrios Psaltis, J. Sandberg, Fiamma Capitanio, Remon Cornelisse, M. R. Gilfanov, Peggy Varniere, Franck Cadoux, Peter J. Wheatley, M. de Pasquale, Juri Poutanen, S. Maestre, A. Pellizzoni, Axel Schwope, Diego Altamirano, Piotr Orleanski, V. Vrba, Agata Różańska, Kateřina Goluchová, P. Rodríguez Gil, Niccolò Bucciantini, Stéphane Schanne, Carlo Ferrigno, Thomas J. Maccarone, H. Wende, Tod E. Strohmayer, Tadayuki Takahashi, Francois Lebrun, E. Kuulkers, Jeroen Homan, Maurizio Paolillo, M. A. Perez, J. P. Osborne, A. Alpar, Sanjay Reddy, G.W. Fraser, V. Sulemainov, D. Linder, L. Sabau-Graziati, A. Rachevski, Bing Zhang, Alessandro Papitto, C. Tenzer, Alex Markowitz, J. Portell, Roberto Mignani, Fabrizio Bocchino, Arnau Rios, R. de la Rie, M. Wille, A. de Rosa, Alessandro Riggio, M. Frericks, Andrew W. Steiner, Michal Bursa, Federico Bernardini, Jon M. Miller, W. Kluzniak, INAF - Osservatorio Astronomico di Roma ( OAR ), Istituto Nazionale di Astrofisica ( INAF ), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées ( LATT ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Variable Energy Cyclotron Centre, Institut Pasteur de Montevideo, Réseau International des Instituts Pasteur ( RIIP ) -Institut Pasteur de Montevideo, Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), FORMATION STELLAIRE 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux ( L3AB ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Interactions et dynamique des environnements de surface ( IDES ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Licryl Laboratory ( CNR-IPCF UOS Cosenza ), University of Calabria, Laboratori Nazionali di Frascati ( LNF ), National Institute for Nuclear Physics ( INFN ), PCAS, Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano ( IASF-MI ), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Canada's National Laboratory for Particle and Nuclear Physics ( TRIUMF ), NRC, Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] ( UNIBO ), Institut de recherches sur la catalyse et l'environnement de Lyon ( IRCELYON ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Spectrochimie Infrarouge et Raman - UMR 8516 ( LASIR ), Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Dipartimento di Scienze Fisiche [Naples], Università degli studi di Napoli Federico II, Energétique, propulsion, espace, environnement ( EPEE ), Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Physics and Astronomy [Hanover], Dartmouth College [Hanover], Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d’Optique Atmosphérique - UMR 8518 ( LOA ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), Institut de Biologie du Développement de Marseille ( IBDM ), Aix Marseille Université ( AMU ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Centre National de la Recherche Scientifique ( CNRS ), Universitat Politècnica de Catalunya [Barcelona] ( UPC ), INAF-IASF Milano, Climate and Environmental Physics [Bern], University of Bern, Centre National d'Etudes Spatiales ( CNES ), Institute of Geology, Eidgenössische Technische Hochschule [Zürich] ( ETH Zürich ), IEEC-CSIC, Universitat Autònoma de Barcelona [Barcelona] ( UAB ), MedisysResearch Lab ( Medisys ), Philips Research, European Space Astronomy Center ( ESAC ), European Space Agency ( ESA ), High Energy Astrophys. & Astropart. Phys (API, FNWI), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Astrophysique de l'Observatoire Midi-Pyrénées (LATT), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Réseau International des Instituts Pasteur (RIIP), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Licryl Laboratory (CNR-IPCF UOS Cosenza), Università della Calabria [Arcavacata di Rende] (Unical), Laboratori Nazionali di Frascati (LNF), Istituto Nazionale di Fisica Nucleare (INFN), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Canada's particle accelerator centre (TRIUMF), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Institut de recherches sur la catalyse et l'environnement de Lyon (IRCELYON), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Laboratoire Avancé de Spectroscopie pour les Intéractions la Réactivité et l'Environnement - UMR 8516 (LASIRE), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), University of Naples Federico II = Università degli studi di Napoli Federico II, Energétique, propulsion, espace, environnement (EPEE), Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Laboratoire d’Optique Atmosphérique - UMR 8518 (LOA), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Institut de Biologie du Développement de Marseille (IBDM), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS), Universitat Politècnica de Catalunya [Barcelona] (UPC), Climate and Environmental Physics [Bern] (CEP), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE)-Universität Bern [Bern] (UNIBE), Centre National d'Études Spatiales [Toulouse] (CNES), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Universitat Autònoma de Barcelona (UAB), MedisysResearch Lab (Medisys), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), SPIE, Takahashi, Tadayuki, Feroci M., Den Herder J.W., Bozzo E., Barret D., Brandt S., Hernanz M., Van Der Klis M., Pohl M., Santangelo A., Stella L., Watts A., Wilms J., Zane S., Ahangarianabhari M., Albertus C., Alford M., Alpar A., Altamirano D., Alvarez L., Amati L., Amoros C., Andersson N., Antonelli A., Argan A., Artigue R., Artigues B., Atteia J.-L., Azzarello P., Bakala P., Baldazzi G., Balman S., Barbera M., Van Baren C., Bhattacharyya S., Baykal A., Belloni T., Bernardini F., Bertuccio G., Bianchi S., Bianchini A., Binko P., Blay P., Bocchino F., Bodin P., Bombaci I., Bonnet Bidaud J.-M., Boutloukos S., Bradley L., Braga J., Brown E., Bucciantini N., Burderi L., Burgay M., Bursa M., Budtz-Jorgensen C., Cackett E., Cadoux F.R., Cais P., Caliandro G.A., Campana R., Campana S., Capitanio F., Casares J., Casella P., Castro-Tirado A.J., Cavazzuti E., Cerda-Duran P., Chakrabarty D., Chateau F., Chenevez J., Coker J., Cole R., Collura A., Cornelisse R., Courvoisier T., Cros A., Cumming A., Cusumano G., D'ai A., D'elia V., Del Monte E., De Luca A., De Martino D., Dercksen J.P.C., De Pasquale M., De Rosa A., Del Santo M., Di Cosimo S., Diebold S., Di Salvo T., Donnarumma I., Drago A., Durant M., Emmanoulopoulos D., Erkut M.H., Esposito P., Evangelista Y., Fabian A., Falanga M., Favre Y., Feldman C., Ferrari V., Ferrigno C., Finger M., Finger M.H., Fraser G.W., Frericks M., Fuschino F., Gabler M., Galloway D.K., Galvez Sanchez J.L., Garcia-Berro E., Gendre B., Gezari S., Giles A.B., Gilfanov M., Giommi P., Giovannini G., Giroletti M., Gogus E., Goldwurm A., Goluchova K., Gotz D., Gouiffes C., Grassi M., Groot P., Gschwender M., Gualtieri L., Guidorzi C., Guy L., Haas D., Haensel P., Hailey M., Hansen F., Hartmann D.H., Haswell C.A., Hebeler K., Heger A., Hermsen W., Homan J., Hornstrup A., Hudec R., Huovelin J., Ingram A., In't Zand J.J.M., Israel G., Iwasawa K., Izzo L., Jacobs H.M., Jetter F., Johannsen T., Jonker P., Jose J., Kaaret P., Kanbach G., Karas V., Karelin D., Kataria D., Keek L., Kennedy T., Klochkov D., Kluzniak W., Kokkotas K., Korpela S., Kouveliotou C., Kreykenbohm I., Kuiper L.M., Kuvvetli I., Labanti C., Lai D., Lamb F.K., Laubert P.P., Lebrun F., Lin D., Linder D., Lodato G., Longo F., Lund N., Maccarone T.J., Macera D., Maestre S., Mahmoodifar S., Maier D., Malcovati P., Mandel I., Mangano V., Manousakis A., Marisaldi M., Markowitz A., Martindale A., Matt G., Mchardy I.M., Melatos A., Mendez M., Mereghetti S., Michalska M., Migliari S., Mignani R., Miller M.C., Miller J.M., Mineo T., Miniutti G., Morsink S., Motch C., Motta S., Mouchet M., Mouret G., Mulaova J., Muleri F., Munoz-Darias T., Negueruela I., Neilsen J., Norton A.J., Nowak M., O'brien P., Olsen P.E.H., Orienti M., Orio M., Orlandini M., Orleaaski P., Osborne J.P., Osten R., Ozel F., Pacciani L., Paolillo M., Papitto A., Paredes J.M., Patruno A., Paul B., Perinati E., Pellizzoni A., Penacchioni A.V., Perez M.A., Petracek V., Pittori C., Pons J., Portell J., Possenti A., Poutanen J., Prakash M., Le Provost P., Psaltis D., Rambaud D., Ramon P., Ramsay G., Rapisarda M., Rachevski A., Rashevskaya I., Ray P.S., Rea N., Reddy S., Reig P., Reina Aranda M., Remillard R., Reynolds C., Rezzolla L., Ribo M., De La Rie R., Riggio A., Rios A., Rodriguez-Gil P., Rodriguez J., Rohlfs R., Romano P., Rossi E.M.R., Rozanska A., Rousseau A., Ryde F., Sabau-Graziati L., Sala G., Salvaterra R., Sanna A., Sandberg J., Scaringi S., Schanne S., Schee J., Schmid C., Shore S., Schneider R., Schwenk A., Schwope A.D., Seyler J.-Y., Shearer A., Smith A., Smith D.M., Smith P.J., Sochora V., Soffitta P., Soleri P., Spencer A., Stappers B., Steiner A.W., Stergioulas N., Stratta G., Strohmayer T.E., Stuchlik Z., Suchy S., Sulemainov V., Takahashi T., Tamburini F., Tauris T., Tenzer C., Tolos L., Tombesi F., Tomsick J., Torok G., Torrejon J.M., Torres D.F., Tramacere A., Trois A., Turolla R., Turriziani S., Uter P., Uttley P., Vacchi A., Varniere P., Vaughan S., Vercellone S., Vrba V., Walton D., Watanabe S., Wawrzaszek R., Webb N., Weinberg N., Wende H., Wheatley P., Wijers R., Wijnands R., Wille M., Wilson-Hodge C.A., Winter B., Wood K., Zampa G., Zampa N., Zampieri L., Zdunik L., Zdziarski A., Zhang B., Zwart F., Ayre M., Boenke T., Corral Van Damme C., Kuulkers E., Lumb D., Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de 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lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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Subjects
x-ray and γ-ray instrumentation, compact objects, microchannel plates, X-ray detectors, X-ray imaging, X-ray spectroscopy, X-ray timing, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, Electrical and Electronic Engineering, Vision, Observatories, Field of view, 01 natural sciences, 7. Clean energy, neutron stars, Observatory, 010303 astronomy & astrophysics, Physics, Equipment and services, Astrophysics::Instrumentation and Methods for Astrophysics, Steradian, [ SDU.ASTR.IM ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics - Instrumentation and Methods for Astrophysics, X-ray detector, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cosmic Vision, Spectral resolution, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, NO, microchannel plate, Settore FIS/05 - Astronomia e Astrofisica, X-rays, compact object, 0103 physical sciences, Electronic, Optical and Magnetic Materials, Instrumentation and Methods for Astrophysics (astro-ph.IM), dense hadronic matter, Sensors, 010308 nuclear & particles physics, Astronomy, Accretion (astrophysics), [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Neutron star, 13. Climate action, [ PHYS.ASTR.IM ] Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Gamma-ray burst, astro-ph.IM
Abstract

The Large Observatory For x-ray Timing (LOFT) was studied within ESA M3 Cosmic Vision framework and participated in the final down-selection for a launch slot in 2022-2024. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument, LOFT will study the behaviour of matter under extreme conditions, such as the strong gravitational field in the innermost regions of accretion flows close to black holes and neutron stars, and the supra-nuclear densities in the interior of neutron stars. The science payload is based on a Large Area Detector (LAD, 10 m 2 effective area, 2-30 keV, 240 eV spectral resolution, 1 deg collimated field of view) and a WideField Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g. GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the status of the mission at the end of its Phase A study., Proc. SPIE 9144, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, 91442T

Published
2014
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46. V2487 Oph 1998: a post nova in an intermediate polar

Author

Margarita Hernanz

Subjects
Physics, Supernova, Intermediate polar, Accretion disc, QC1-999, ROSAT, Astronomy, White dwarf, Cataclysmic variable star, Astrophysics, Binary system, Accretion (astrophysics)
Abstract

V2487 Oph (Nova Oph 1998) is a classical nova that exploded in 1998. XMM-Newton observations performed between 2 and 9 years after the explosion showed emission related to restablished accretion, and indicative of a magnetic white dwarf. The spectrum looks like that of a cataclysmic variable of the intermediate polar type. Anyway, we don't have yet a definitive confirmation of the intermediate polar character, through determination of spin and orbital periods. Although it is not the first nova exploding in a magnetic white dwarf, it is always challenging to reach explosive conditions when a stan- dard accretion disk can't be formed, because of the magnetic field. In addition, V2487 Oph has been the first nova where a detection of X-rays - in the host binary system - has been reported prior to its eruption, in 1990 with the ROSAT satellite. V2487 Oph has been also detected in hard X-rays with INTEGRAL/IBIS and RXTE/PCA. Last but not least, V2487 Oph has been identified as a recurrent nova in 2008, since a prior eruption in 1900 has been reported through analysis of Harvard photographic plates. Therefore, it is expected to host a massive white dwarf and be a candidate for a type Ia supernova explo- sion. In a recent study of the progenitors of galactic novae, it has been emphasized that V2487 Oph is an important and interesting object, "intermediate" between the "standard" classical novae and other historical and well-known recurrent novae with shorter recur- rence periods. It could be that in the end there's a continuous distribution of recurrence periods, instead of the common understanding up to now that "classical" and "recurrent" novae were quite apart (with recurrence periods of more than 10 4 years and less than 100 years - approximately - respectively). We present the results of our campaign of sev- eral observations with XMM-Newton. The consequences for the understanding of such a puzzling object are discussed.

Published
2014

47. The Cooling of CO White Dwarfs: Influence of the Internal Chemical Distribution

Author

Inmaculada Domínguez, Margarita Hernanz, Maurizio Salaris, Jordi Isern, Robert Mochkovitch, and Enrique García-Berro

Subjects
Physics, Astrophysics (astro-ph), FOS: Physical sciences, Stratification (water), White dwarf, Astronomy and Astrophysics, Chemical distribution, Astrophysics, Stars interiors, law.invention, Space and Planetary Science, law, Nuclear reactions, Abundances, Crystallization, Nucleosynthesis
Abstract

White dwarfs are the remnants of stars of low and intermediate masses on the main sequence. Since they have exhausted all of their nuclear fuel, their evolution is just a gravothermal process. The release of energy only depends on the detailed internal structure and chemical composition and on the properties of the envelope equation of state and opacity; its consequences on the cooling curve (i.e., the luminosity vs. time relationship) depend on the luminosity at which this energy is released. The internal chemical profile depends on the rate of the 12C(α, γ)16O reaction as well as on the treatment of convection. High reaction rates produce white dwarfs with oxygen-rich cores surrounded by carbon-rich mantles. This reduces the available gravothermal energy and decreases the lifetime of white dwarfs. In this paper we compute detailed evolutionary models providing chemical profiles for white dwarfs having progenitors in the mass range from 1.0 to 7 M☉, and we examine the influence of such profiles in the cooling process. The influence of the process of separation of carbon and oxygen during crystallization is decreased as a consequence of the initial stratification, but it is still important and cannot be neglected. As an example, the best fit to the luminosity functions of Liebert et al. and Oswalt et al. gives an age of the disk of 9.3 and 11.0 Gyr, respectively, when this effect is taken into account, and only 8.3 and 10.0 Gyr when it is neglected., This work has been supported by DGICYT grants PB 94-0111, PB 93-1162, and PB 94-0827-C02-02, the CIRIT grant GRQ 94-8001, the AIHF 335-B, the AIHI 94-082-A, and the C4 consortium. One of us (M. S.) thanks the EC for the “Human Capital and Mobility” fellowship ERBCHGECT920009.

Published
1997
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48. The Physics of Crystallizing White Dwarfs

Author

Robert Mochkovitch, Enrique García-Berro, Margarita Hernanz, and Jordi Isern

Subjects
Physics, Astrophysics (astro-ph), Theoretical models, FOS: Physical sciences, White dwarf, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Formalism (philosophy of mathematics), Cooling rate, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

White dwarfs can be used as galactic chronometers and, therefore, provide important information about galactic evolution if good theoretical models of their cooling are available. Consequently, it is natural to wonder if all the sources or sinks of energy are correctly taken into account. One of these sources is partial differentiation of the chemical components of the white dwarf upon crystallization. In this paper we use a new formalism to show that if there is a redistribution of the elements inside the star, there is a net release of energy that has to be radiated away and that slows down the cooling rate of the white dwarf., Accepted for publication in ApJ (16 pages, 1 figure, aasms4)

Published
1997
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49. New Results on [TSUP]26[/TSUP]A[CLC]l[/CLC] Production in Classical Novae

Author

Alain Coc, Margarita Hernanz, and Jordi José

Subjects
Physics, Nuclear reaction, Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 7. Clean energy, Galaxy, Reaction rate, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Envelope (waves)
Abstract

The production of 26Al by explosions of classical novae has been computed by means of a hydrodynamic code that follows both the accretion and the explosion stages. A special emphasis has been put on the analysis of the influence of the initial abundances of the accreted envelope, as well as on the nuclear reaction rates involved. With the most recent values of chemical composition and reaction rates available, 26Al production is lowered with respect to previous computations. According to our results, the final contribution of novae to the galactic 26Al is at most 0.4 M_sun, which is a small part of the estimated 26Al in the Galaxy derived from COMPTEL observations of the 1809 keV emission.

Published
1997
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50. Novel association of Neuregulin 1 gene with bipolar disorder but not with schizophrenia

Author

Ana González-Pinto, Amaia Ugarte, Aitor Palomino, Gixane González-García, Begoña Mendíbil, Arantza Gutiérrez-Fernández, Luis Pacheco, Carlos Matute, María Etxebeste, and Margarita Hernanz

Subjects
Adult, Male, Bipolar Disorder, biology, business.industry, Neuregulin-1, Middle Aged, Bioinformatics, medicine.disease, Polymorphism, Single Nucleotide, Cohort Studies, Psychiatry and Mental health, Psychotic Disorders, Schizophrenia, biology.protein, medicine, Humans, Female, Bipolar disorder, Neuregulin 1, Association (psychology), business, Gene, Biological Psychiatry
Published
2013

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