Author: "Margarita Hernanz" / Language: english - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Margarita Hernanz"' showing total 41 results

Start Over Author "Margarita Hernanz" Language english

41 results on '"Margarita Hernanz"'

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
Full Text: View/download PDF

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
Full Text: View/download PDF

3. 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
Full Text: View/download PDF

4. 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
Full Text: View/download PDF

5. 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

6. 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
Full Text: View/download PDF

7. 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
Full Text: View/download PDF

8. 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
Full Text: View/download PDF

9. The e-ASTROGAM mission: Exploring the extreme Universe with gamma rays in the MeV â 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

10. 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

11. 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
Full Text: View/download PDF

12. 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
Full Text: View/download PDF

13. 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
Full Text: View/download PDF

14. 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
Full Text: View/download PDF

15. 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 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), 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), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et 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), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Universität Bern [Bern]-Universität Bern [Bern], European Space Agency (ESA), Feroci, M., den Herder, J., 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., 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., Boutloukos, S., Bradley, L., Braga, J., Brown, E., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz Jørgensen, C., Cackett, E., Cadoux, F., Caïs, P., Caliandro, G., Campana, R., Campana, S., Capitanio, F., Casares, J., Casella, P., Castro Tirado, A., Cavazzuti, E., Cerda Duran, P., Chakrabarty, D., Château, 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., 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., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Ferrari, V., Ferrigno, C., Finger, M., Fraser, G., Frericks, M., Fuschino, F., Gabler, M., Galloway, D., Galvez Sanchez, J., Garcia Berro, E., Gendre, B., Gezari, S., Giles, A., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, 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., Haswell, C., Hebeler, K., Heger, A., Hermsen, W., Homan, J., Hornstrup, A., Hudec, R., Huovelin, J., Ingram, A., In't Zand, J., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H., Jetter, F., Johannsen, T., Jonker, P., Josè, 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., Kuvvetli, I., Labanti, C., Lai, D., Lamb, F., Laubert, P., Lebrun, F., Lin, D., Linder, D., Lodato, G., Longo, F., Lund, N., Maccarone, T., 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., Melatos, A., Mendez, M., Mereghetti, S., Michalska, M., Migliari, S., Mignani, R., Miller, M., Miller, J., Mineo, T., Miniutti, G., Morsink, S., Motch, C., Motta, S., Mouchet, M., Mouret, G., Mulačová, J., Muleri, F., Muñoz Darias, T., Negueruela, I., Neilsen, J., Norton, A., Nowak, M., O'Brien, P., Olsen, P., Orienti, M., Orio, M., Orlandini, M., Orleański, P., Osborne, J., Osten, R., Ozel, F., Pacciani, L., Paolillo, M., Papitto, A., Paredes, J., Patruno, A., Paul, B., Perinati, E., Pellizzoni, A., Penacchioni, A., Perez, M., 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., 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., Rodríguez Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E., 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., Seyler, J., Shearer, A., Smith, A., Smith, D., Smith, P., Sochora, V., Soffitta, P., Soleri, P., Spencer, A., Stappers, B., Steiner, A., Stergioulas, N., Stratta, G., Strohmayer, T., Stuchlik, Z., Suchy, S., Sulemainov, V., Takahashi, T., Tamburini, F., Tauris, T., Tenzer, C., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J., Torres, D., 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., 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-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), National Institute for Nuclear Physics (INFN), 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), Canada's National Laboratory for Particle and Nuclear Physics (TRIUMF), Università di Bologna [Bologna] (UNIBO), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Spectrochimie Infrarouge et Raman - UMR 8516 (LASIR), Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Lille, Aix Marseille Université (AMU)-Collège de France (CdF)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Universitat Autònoma de Barcelona [Barcelona] (UAB), Astronomy, den Herder, J. W., Atteia, J. L., Bonnet Bidaud, J. M., Cadoux, F. R., Cais, P., Caliandro, G. A., Castro Tirado, A. J., D'Aì, A., De Luca, A., De Martino, D., Dercksen, J. P. C., De Pasquale, M., Di Salvo, T., Erkut, M. H., Finger, M. H., Fraser, G. W., Galloway, D. K., Galvez Sanchez, J. L., Giles, A. B., Hartmann, D. H., Haswell, C. A., in't Zand, J. J. M., Jacobs, H. M., Kuiper, L. M., Lamb, F. K., Laubert, P. P., Maccarone, T. J., Mchardy, I. M., Miller, M. C., Miller, J. M., Norton, A. J., Olsen, P. E. H., Orleanski, P., Osborne, J. P., Paolillo, Maurizio, Paredes, J. M., Penacchioni, A. V., Perez, M. A., Ray, P. S., Rossi, E. M. R., Schwope, A. D., Seyler, J. Y., Smith, D. M., Smith, P. J., Steiner, A. W., Strohmayer, T. E., Torrejon, J. M., Torres, D. F., and Wilson Hodge, C. A.
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
Full Text: View/download PDF

16. 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

17. Novae in gamma-rays

Author: Margarita Hernanz
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Nuclear Experiment, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Classical novae produce radioactive nuclei which are emitters of gamma-rays in the MeV range. Some examples are the lines at 478 and 1275 keV (from 7Be and 22Na) and the positron-electron annihilation emission (511 keV line and a continuum below this energy, with a cut-off at 20-30 keV). The analysis of gamma-ray spectra and light curves is a potential unique and powerful tool both to trace the corresponding isotopes and to give insights on the properties of the expanding envelope determining its transparency. Another possible origin of gamma-rays is the acceleration of particles up to very high energies, so that either neutral pions or inverse Compton processes produce gamma-rays of energies larger than 100 MeV. MeV photons during nova explosions have not been detected yet, although several attempts have been made in the last decades; on the other hand, GeV photons from novae have been detected in some particular novae, in symbiotic binaries, where the companion is a red giant with a wind, instead of a main sequence star as in the cataclysmic variables hosting classical novae. Both mechanisms of gamma-ray production in novae are reviewed, with more emphasis on the one related to radioactivities., 16 pages, 4 figures, to appear in Bull. Astr. Soc. India (2012), 40, 337-391
Published: 2013

18. Accelerator experiments with soft protons and hyper-velocity dust particles: Application to ongoing projects of future X-ray missions

Author: Marco Feroci, E. Del Monte, N. Zampa, Lothar Strüder, A. Vacchi, J. Jochum, Silvia Zane, Alda Rubini, Margarita Hernanz, Søren Brandt, Caroline A. Kilbourne, Norbert Meidinger, George W. Fraser, Ralf Srama, D. Gotz, Maurice A. Leutenegger, J. P. Osborne, P. Azzarello, Michael Freyberg, R. L. Kelley, A. Rachevski, S. Bugiel, I. Rashevskaya, Emanuele Perinati, J. W. den Herder, C. Tenzer, Sebastian Diebold, Eckhard Kendziorra, Peter Friedrich, Konrad Dennerl, Gianluigi Zampa, Andrea Santangelo, B. Cordier, and Enrico Bozzo
Subjects: Physics - Instrumentation and Detectors, Proton, Instrumentation, Nuclear engineering, Hyper-velocity impacts, FOS: Physical sciences, Context (language use), Radiation, law.invention, Radiation damage, law, X-ray instrumentation, Van de Graaff generator, Electronic, Particle accelerators, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, Electrical and Electronic Engineering, Optical and Magnetic Materials, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Scattering, Detector, X-ray, Instrumentation and Detectors (physics.ins-det), Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We report on our activities, currently in progress, aimed at performing accelerator experiments with soft protons and hyper-velocity dust particles. They include tests of different types of X-ray detectors and related components (such as filters) and measurements of scattering of soft protons and hyper-velocity dust particles off X-ray mirror shells. These activities have been identified as a goal in the context of a number of ongoing space projects in order to assess the risk posed by environmental radiation and dust and qualify the adopted instrumentation with respect to possible damage or performance degradation. In this paper we focus on tests for the Silicon Drift Detectors (SDDs) used aboard the LOFT space mission. We use the Van de Graaff accelerators at the University of T\"ubingen and at the Max Planck Institute for Nuclear Physics (MPIK) in Heidelberg, for soft proton and hyper-velocity dust tests respectively. We present the experimental set-up adopted to perform the tests, status of the activities and some very preliminary results achieved at present time., Comment: Proceedings of SPIE, Vol. 8443, Paper No. 8443-24, 2012
Published: 2012

19. Classical and recurrent nova models

Author: Steven N. Shore, Enrique García–Berro, Alan C. Calder, Jordi Casanova, Margarita Hernanz, Jordi José, Universitat Politècnica de Catalunya. Departament de Física i Enginyeria Nuclear, Universitat Politècnica de Catalunya. Departament de Física Aplicada, and Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica
Subjects: Convection, Nuclear reaction, Astrofísica, Thermonuclear fusion, Física::Física de fluids [Àrees temàtiques de la UPC], Astrophysics, Photometry (optics), accretion, Nucleosynthesis, Ejecta, convection, nuclear reactions, white dwarfs, Physics, Energies::Energia nuclear [Àrees temàtiques de la UPC], cataclysmic variables, abundances, accretion disks, White dwarf, Astronomy, nucleosynthesis, Astronomy and Astrophysics, Interstellar medium, Space and Planetary Science, instabilities, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], hydrodynamics, novae [stars]
Abstract: Remarkable progress in the understanding of nova outbursts has been achieved through combined efforts in photometry, spectroscopy and numerical simulations. According to the thermonuclear runaway model, novae are powered by thermonuclear explosions in the hydrogen-rich envelopes transferred from a low-mass stellar companion onto a close white dwarf star. Extensive numerical simulations in 1-D have shown that the accreted envelopes attain peak temperatures ranging between 108 and 4 × 108 K, for about several hundred seconds, hence allowing extensive nuclear processing which eventually shows up in the form of nucleosynthetic fingerprints in the ejecta. Indeed, it has been claimed that novae can play a certain role in the enrichment of the interstellar medium through a number of intermediate-mass elements. This includes 17O, 15N, and 13C, systematically overproduced with respect to solar abundances, plus a lower contribution in a number of other species (A < 40), such as 7Li, 19F, or 26Al. At the turn of the XXI Century, classical novae have entered the era of multidimensional models, which provide a new insight into the physical mechanisms that drive mixing at the core-envelope interface.In this review, we will present hydrodynamic models of classical novae, from the onset of accretion up to the explosion and ejection stages, both for classical and recurrent novae, with special emphasis on their gross observational properties and their associated nucleosynthesis. The impact of nuclear uncertainties on the final yields will be discussed. Recent results from 2-D models of mixing during classical nova outbursts will also be presented.
Published: 2011

20. Binary systems and their nuclear explosions

Author: Jordi José, Margarita Hernanz, Jordi Isern, Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, and Universitat Politècnica de Catalunya. Departament de Física i Enginyeria Nuclear
Subjects: Physics, Equation of state, Thermonuclear fusion, Astrophysics::High Energy Astrophysical Phenomena, education, chemistry.chemical_element, Nuclear energy, Astrophysics, Iron peak, 01 natural sciences, Ideal gas, Nuclear physics, chemistry, Electron degeneracy pressure, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Energia nuclear, Neutron, Física nuclear, 010306 general physics, Gravitational binding energy, 010303 astronomy & astrophysics, Helium
Abstract: The nuclear energy supply of a typical star like the Sun would be ~ 1052 erg if all the hydrogen could be incinerated into iron peak elements. Since the gravitational binding energy is ~ 1049 erg, it is evident that the nuclear energy content is more than enough to blow up the Sun. However, stars are stable thanks to the fact that their matter obeys the equation of state of a classical ideal gas that acts as a thermostat: if some energy is released as a consequence of a thermal fluctuation, the gas expands, the temperature drops and the instability is quenched. The first researchers to discuss the scenario under which stars could explosively release their nuclear energy were Hoyle and Fowler (1960). They showed that this could occur under conditions of dynamic compression, as a consequence of collapse, or under electron degeneracy. They also pointed out in their seminal paper that hydrogen could only be responsible for mild explosions, like novae, as a consequence of the necessity to convert two protons into two neutrons, and that only the thermonuclear fusion of carbon could be energetic enough to feed a strong explosion. They did not consider helium because by this epoch the He-burning mechanism was not yet known.
Published: 2011

21. Research and development of a gamma-ray imaging spectrometer in the MeV range in Barcelona

Author: E. Cabruja, Manuel Lozano, José-Luis Galvez, Miguel Ullan, M. Chmeissani, Giulio Pellegrini, J. M. Álvarez, Jordi Isern, and Margarita Hernanz
Subjects: Physics, Spectrometer, business.industry, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Detector, Gamma ray, Imaging spectrometer, Astrophysics, Dot pitch, law.invention, Telescope, CdTe pixel detector, Optics, law, Laue Lens detector, business, Gamma-ray burst, Image resolution, Gamma-ray Astrophysics, Stacked detector
Abstract: Copyright 2010 Society of Photo-Optical Instrumentation Engineers (SPIE). One print or electronic copy may be made for personal use only. Systematic electronic or print reproduction and distribution, duplication of any material in this paper for a fee or for commercial purposes, or modification of the content of the paper are prohibited., Gamma-ray astrophysics in the MeV energy range plays an important role for the understanding of cosmic explosions and acceleration mechanisms in a variety of galactic and extragalactic sources, e.g., Supernovae, Classical Novae, Supernova Remnants (SNRs), Gamma-Ray Bursts (GRBs), Pulsars, Active Galactic Nuclei (AGN). Through the development of focusing telescopes in the MeV energy range, it will be possible to reach unprecedented sensitivities, compared with those of the currently operating gamma ray telescopes. In order to achieve the needed performance, a detector with mm spatial resolution and very high peak efficiency is required. It will be also desirable that the detector could detect polarization of the source. Our research and development activities in Barcelona aim to study a gamma-ray imaging spectrometer in the MeV range suited for the focal plane of a gamma-ray telescope mission, based on CdTe pixel detectors arranged in multiple layers with increasing thicknesses, to enhance gamma-ray absorption in the Compton regime. We have developed an initial prototype based on several CdTe module detectors, with 11x11 pixels, a pixel pitch of 1mm and a thickness of 2mm. Each pixel is stud-bump bonded to a fanout board and routed to a readout ASIC to measure pixel position, pulse height and rise time information for each incident gamma-ray photon. We will report on the results of an optimization study based on simulations, to select the optimal thickness of each CdTe detector within the module to get the best energy resolution of the spectrometer.
Published: 2010

22. Recent discoveries of supersoft X-ray sources in M 31

Author: Dieter H. Hartmann, Michael Freyberg, Gloria Sala, Holger Stiele, Arne Rau, Margarita Hernanz, Despina Hatzidimitriou, Frank Haberl, Wolfgang Pietsch, Marina Orio, Martin Henze, and Jochen Greiner
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Stars: individual: (M31N 2007-06b, M31N 2007-1 1a, M31N 2006-04a), individual: (M 31) [Galaxies], X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Orbital period, Light curve, Monitoring program, Galaxy, X-rays: binaries, Space and Planetary Science, Monitoring data, Globular cluster, Galaxies: individual: (M 31), Novae, cataclysmic variables, binaries [X-rays], individual: (M31N 2007-06b, M31N 2007-1 1a, M31N 2006-04a) [Stars], Astrophysics - High Energy Astrophysical Phenomena
Abstract: Classical novae (CNe) have recently been reported to represent the major class of supersoft X-ray sources (SSSs) in the central area of our neighbouring galaxy M 31. This paper presents a review of results from recent X-ray observations of M 31 with XMM-Newton and Chandra. We carried out a dedicated optical and X-ray monitoring program of CNe and SSSs in the central area of M 31. We discovered the first SSSs in M 31 globular clusters (GCs) and their connection to the very first discovered CN in a M 31 GC. This result may have an impact on the CN rate in GCs. Furthermore, in our optical and X-ray monitoring data we discovered the CN M31N 2007-11a, which shows a very short SSS phase of 29 - 52 days. Short SSS states (durations < 100 days) of CNe indicate massive white dwarfs (WDs) that are candidate progenitors of supernovae type Ia. In the case of M31N 2007-11a, the optical and X-ray light curves suggest a binary containing a WD with M_WD > 1.0 M_sun. Finally, we present the discovery of the SSS counterpart of the CN M31N 2006-04a. The X-ray light curve of M31N 2006-04a shows short-time variability, which might indicate an orbital period of about 2 hours., 4 pages, 1 figure; Proc. of workshop "Supersoft X-ray Sources - New Developments", ESAC, May 2009; accepted for publication in Astronomische Nachrichten
Published: 2009

23. X-ray observations of classical novae. Theoretical implications

Author: Margarita Hernanz and Gloria Sala
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Cataclysmic variable star, FOS: Physical sciences, Astrophysics, white dwarfs [Stars], X-rays: binaries, Astrophysics::Solar and Stellar Astrophysics, Ejecta, Solar and Stellar Astrophysics (astro-ph.SR), Envelope (waves), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Cataclysmic variables, Photosphere, Accretion (meteorology), White dwarf, Astronomy and Astrophysics, Stars: white dwarfs, Supernova, Nova (rocket), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, novae [Stars], binaries [X-rays], Stars: novae, Astrophysics - High Energy Astrophysical Phenomena
Abstract: 6 pages, 1 figure, 1 table.-- Pre-print archive.-- Refereed workshop proceedings will be published as a regular issue of "Astronomische Nachrichten (Astronomical Notes)"., Detection of X-rays from classical novae, both in outburst and post-outburst, provides unique and crucial information about the explosion mechanism. Soft X-rays reveal the hot white dwarf photosphere, whenever hydrogen (H) nuclear burning is still on and expanding envelope is transparent enough, whereas harder X-rays give information about the ejecta and/or the accretion flow in the reborn cataclysmic variable. The duration of the supersoft X-ray emission phase is related to the turn-off of the classical nova, i.e., of the H-burning on top of the white dwarf core. A review of X-ray observations is presented, with a special emphasis on the implications for the duration of post-outburst steady H-burning and its theoretical explanation. The particular case of recurrent novae (both the ”standard” objects and the recently discovered ones) will also be reviewed, in terms of theoretical feasibility of short recurrence periods, as well as regarding implications for scenarios of type Ia supernovae., This research has been funded by theMICINN projects AYA 2008-01839/ESP, AYA 2008-04211-C02-01 and AYA 2007-66256, the AGAUR project 2009 SGR 315 and by FEDER funds.
Published: 2009

24. The very short supersoft X-ray state of the classical nova M31N 2007-11a

Author: Dieter H. Hartmann, Michael Freyberg, M. Della Valle, Margarita Hernanz, Frank Haberl, Gloria Sala, Vadim Burwitz, Wolfgang Pietsch, Jochen Greiner, G. Grant Williams, Peter A. Milne, and Martin Henze
Subjects: Physics, Solar mass, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, White dwarf, Astronomy and Astrophysics, Nova (laser), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Light curve, Monitoring program, law.invention, Telescope, Supernova, Space and Planetary Science, law, Bulge, Astrophysics::Solar and Stellar Astrophysics
Abstract: Short supersoft X-ray source (SSS) states (durations < 100 days) of classical novae (CNe) indicate massive white dwarfs that are candidate progenitors of supernovae type Ia. We carry out a dedicated optical and X-ray monitoring program of CNe in the bulge of M 31. We discovered M31N 2007-11a and determined its optical and X-ray light curve. We used the robotic Super-LOTIS telescope to obtain the optical data and XMM-Newton and Chandra observations to discover an X-ray counterpart to that nova. Nova M31N 2007-11a is a very fast CN, exhibiting a very short SSS state with an appearance time of 6-16 days after outburst and a turn-off time of 45-58 days after outburst. The optical and X-ray light curves of M31N 2007-11a suggest a binary containing a white dwarf with a mass greater than one solar mass., 4 pages, 2 figures, 2 tables, submitted to A&A Letters; v2: accepted version
Published: 2008

25. Models for the soft X-ray emission of post-outburst classical novae

Author: Margarita Hernanz and Gloria Sala
Subjects: Physics, Soft x ray, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, White dwarf, Astronomy and Astrophysics, Observable, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Effective temperature, Luminosity, law.invention, Space and Planetary Science, law, Phase (matter), Astrophysics::Solar and Stellar Astrophysics, Hydrostatic equilibrium, Astrophysics::Galaxy Astrophysics, Envelope (waves)
Abstract: A hydrostatic and stationary white dwarf envelope model has been developed for the study of the post-outburst phases of classical novae and their soft X-ray emission. Several white dwarf masses and chemical compositions typical for classical novae have been considered. The results show that the luminosity, maximum effective temperature and envelope masses depend on the white dwarf mass and on the chemical composition. Envelope masses for which equilibrium solutions exist are pretty small ~10^{-7}-10^{-6} Msun, thus leading to a short duration of the soft X-ray emitting phase of classical novae, in agreement with most of the observations. The models presented provide a useful tool for the determination of the white dwarf properties from observable parameters in the X-ray range., 15 pages, 11 figures, 2 tables, accepted for publication in Astronomy & Astrophysics
Published: 2005

26. Future INTEGRAL observations of classical novae

Author: Pierre Jean, A. Giménez, Alain Coc, J. W. Truran, Gloria Sala, Jordi José, Jordi Isern, Sumner Starrfield, Margarita Hernanz, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), and 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)
Subjects: Physics, Thermonuclear fusion, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy, Astrophysics, 7. Clean energy, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 13. Climate action, Nucleosynthesis, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Gamma-ray burst, 010303 astronomy & astrophysics, Gamma ray detection
Abstract: The detection of gamma‐rays from classical novae would provide a unique proof of the thermonuclear runaway model for these explosions. There has been no positive detection of any nova in gamma‐rays up to date. The gamma rays emitted as a consequence of nova outbursts directly reflect the amount of radioactive nuclei synthesized during the explosion; in addition, they provide a direct insight of the dynamic properties of the expanding nova envelope, specially those emitted promptly, when the envelope is not yet completely transparent. The ESA INTEGRAL satellite (launch date October 17th, 2002), will offer an excellent opportunity to observe nearby classical novae, with unprecedented sensitivity and energetic resolution. Both our approved observation in the Guest Observer’s Programme, and the foreseen Core Programme observations, will hopefully be able to detect the gamma ray emission from classical nova explosions and to extract the maximum possible scientific results from them.
Published: 2002

27. The prompt gamma-ray emission of novae

Author: J. Gómez-Gomar, Jordi José, and Margarita Hernanz
Subjects: Physics, Positron, Isotope, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Gamma ray, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astronomy and Astrophysics, Astrophysics, Electron
Abstract: Classical novae are potential gamma-ray emitters, because of the disintegration of some radioactive nuclei synthesized during the explosion. Some short-lived isotopes (such as 13N and 18F), as well as the medium-lived 22Na, decay emitting positrons, which annihilate with electrons and thus are responsible for the prompt emission of gamma-rays from novae. This emission consists of a 511 keV line plus a continuum between 20 and 511 keV, and is released before the maximum in visual luminosity, i.e., before the discovery of the nova. The main characteristics of this prompt emission, together with the related uncertainties (both of nuclear and hydrodynamical origin, with a particular emphasis on the influence of the envelope properties) and prospects for detectability are analyzed in this paper., 6 pages, 3 figures (6 PS files), to appear in New Astronomy Reviews (Proceedings of the Ringberg Workshop "Astronomy with Radioactivities III")
Published: 2001

28. Gamma-ray signatures of classical novae

Author: Margarita Hernanz, J. Gómez-Gomar, and Jordi José
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Theoretical models, Gamma ray, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Nova (laser), Gamma-ray astronomy, Astrophysics, Interpretation (model theory), Gamma ray detection
Abstract: The role of classical novae as potential gamma-ray emitters is reviewed, on the basis of theoretical models of the gamma-ray emission from different nova types. The interpretation of the up to now negative results of the gamma-ray observations of novae, as well as the prospects for detectability with future instruments (specially onboard INTEGRAL) are also discussed., 10 pages, 7 figures. Invited talk at the "Gamma 2001" Symposium, April 4-6, 2001, Baltimore, Maryland. To be published by AIP
Published: 2001

29. Nucleosynthesis in classical novae

Author: Jordi José, Margarita Hernanz, Christian Iliadis, Girod, Dominique, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), and 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)
Subjects: Nuclear and High Energy Physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Natural abundance, Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Cosmochemistry, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Nucleosynthesis, 0103 physical sciences, Nuclear astrophysics, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, Ejecta, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy, Nova (laser), Galaxy, Chemical evolution, Supernova, Meteorite, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]
Abstract: A general review of the relevance of classical novae for the chemical evolution of the Galaxy, as well as for Galactic radioactivity is presented. A special emphasis is put on the pioneering work done by Jim Truran in this field of research. The impact of recent developments in nuclear astrophysics on nova nucleosynthesis, together with the prospects for observability of novae radioactivities with the INTEGRAL satellite are discussed., Comment: 6 pages, invited talk, to be published in Proceedings of the conference "Cosmic Evolution" in the honor of J. Audouze and J.W. Truran, held at Institut d'Astrophysique de Paris, November 2000
Published: 2001

30. The ages of very cool hydrogen-rich white dwarfs

Author: Enrique García-Berro, Didier Saumon, Maurizio Salaris, Margarita Hernanz, and Jordi Isern
Subjects: Physics, Equation of state, Hydrogen, Opacity, Astrophysics (astro-ph), Degenerate energy levels, FOS: Physical sciences, chemistry.chemical_element, Binary number, White dwarf, Astronomy and Astrophysics, Astrophysics, chemistry, Space and Planetary Science, Latent heat, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Physics::Atomic Physics, Envelope (waves)
Abstract: The evolution of white dwarfs is essentially a cooling process that depends primarily on the energy stored in their degenerate cores and on the transparency of their envelopes. In this paper we compute accurate cooling sequences for carbon-oxygen white dwarfs with hydrogen dominated atmospheres for the full range of masses of interest. For this purpose we use the most accurate available physical inputs for both the equation of state and opacities of the envelope and for the thermodynamic quantities of the degenerate core. We also investigate the role of the latent heat in the computed cooling sequences. We present separately cooling sequences in which the effects of phase separation of the carbon-oxygen binary mixture upon crystallization have been neglected, and the delay introduced in the cooling times when this mechanism is properly taken into account, in order to compare our results with other published cooling sequences which do not include a treatment of this phenomenon. We find that the cooling ages of very cool white dwarfs with pure hydrogen atmospheres have been systematically underestimated by roughly 1.5 Gyr at log(L/Lo)=-4.5 for an otherwise typical 0.6 Mo white dwarf, when phase separation is neglected. If phase separation of the binary mixture is included then the cooling ages are further increased by roughly 10%. Cooling tracks and cooling isochrones in several color-magnitude diagrams are presented as well., 8 Pages; ApJ, accepted for publication
Published: 2000

31. Update of nuclear reaction rates affecting nucleosynthesis in novae

Author: J. P. Thibaud, Margarita Hernanz, N. Smirnova, A. Coc, Jordi José, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), 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), J. Christensen-Dalsgaard, K. Langanke, and Lorgeril, Jocelyne
Subjects: Nuclear physics, Nuclear reaction, Physics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Nuclear and High Energy Physics, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 010308 nuclear & particles physics, Nucleosynthesis, 0103 physical sciences, 010306 general physics, 01 natural sciences
Published: 2000

32. New theoretical results concerning gamma-ray emission from classical novae

Author: Jordi José, Alain Coc, Jordi Isern, J. Gómez-Gomar, Margarita Hernanz, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), and 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)
Subjects: Nuclear reaction, Physics, Annihilation, Proton, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, 020206 networking & telecommunications, 02 engineering and technology, Nova (laser), Gamma-ray astronomy, Astrophysics, 7. Clean energy, Nuclear physics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Apparent magnitude, 13. Climate action, Nucleosynthesis, 0202 electrical engineering, electronic engineering, information engineering, Astrophysics::Solar and Stellar Astrophysics, 020201 artificial intelligence & image processing
Abstract: New results concerning the synthesis of radioactive nuclei in classical nova explosions are presented, together with their influence on the gamma-ray emission from these objects and the prospects for the detectability with present and future instruments. The isotopes involved in gamma-ray emission from classical novae are 13N, 18F, 7Be, 22Na and 26Al. Both 13N and 18F are crucial for the short duration annihilation emission, at 511 keV and below, that is emitted during the first hours after the outburst, before the nova maximum in visual magnitude. New recent results concerning the nuclear reaction rates involved in 18F destruction have been incorporated into our hydrodynamic code, which models the nova explosion with a detailed follow up of the associated nucleosynthesis. As a result of the larger rates of 18F destruction through proton captures, this isotope is produced in smaller quantities (typically by a factor of 10), leading to smaller fluxes in the 30–511 keV range. Concerning the medium and long ...
Published: 1999

33. The energetics of crystallizing white dwarfs revisited again

Author: Gilles Chabrier, Jordi Isern, Enrique García-Berro, and Margarita Hernanz
Subjects: Physics, Energetics, Astrophysics (astro-ph), White dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, law.invention, Space and Planetary Science, law, Astrophysics::Solar and Stellar Astrophysics, Redistribution (chemistry), Astrophysics::Earth and Planetary Astrophysics, Total energy, Crystallization, Chemical composition
Abstract: The evolution of white dwarfs is a cooling process that depends on the energy stored in the core and on the way in which it is transferred through the envelope. In this paper we show that despite some (erroneous) claims, the redistribution of chemical elements ensuing the crystallization of C/O white dwarfs provides between the 10% and the 20% of the total energy released during the crystallization process, depending on the internal chemical composition, which is not negligible at all, given the present state of the art of the white dwarf cooling theory., 16 pages, 2 figures, accepted for publication in Astrophysical Journal
Published: 1999

34. Gamma-ray emission from novae related to positron annihilation: constraints on its observability posed by new experimental nuclear data

Author: Jordi José, Jordi Isern, Alain Coc, Margarita Hernanz, J. Gómez-Gomar, Centre de Spectrométrie Nucléaire et de Spectrométrie de Masse (CSNSM), 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), and Lorgeril, Jocelyne
Subjects: Physics, Range (particle radiation), [PHYS.NEXP] Physics [physics]/Nuclear Experiment [nucl-ex], 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Gamma ray, FOS: Physical sciences, Nuclear data, Astronomy and Astrophysics, Astrophysics, Nova (laser), Radiation, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 01 natural sciences, Luminosity, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Moment (physics), 010303 astronomy & astrophysics, Envelope (waves)
Abstract: Classical novae emit gamma-ray radiation at 511 keV and below, with a cut-off at around (20-30) keV, related to positron annihilation and its Comptonization in the expanding envelope. This emission has been elusive up to now, because it occurs at epochs well before the maximum in optical luminosity, but it could be detected by some sensitive intrument on board a satellite, provided that the nova is close enough and that it is observed at the right moment. The detection of this emission, which is a challenge for the now available and for the future gamma-ray instruments, would shed light into the physical processes occurring in the early phases of the explosion, which are invisible in other lower energy ranges. A good prediction of the emitted fluxes and of the corresponding detectability distances with different instruments relies critically on a good knowledge of reaction rates relevant to f18 destruction, which have been subject to a strong revision after recent nuclear spectroscopy measurements. With respect to previous results, smaller ejected masses of f18 are predicted, leading to smaller emitted fluxes in the (20-511) keV range and shorter detectability distances., 9 pages, 2 figures, accepted for publication in Astrophys. J. Letters
Published: 1999

35. The halo white dwarf population

Author: Enrique García-Berro, Santiago Torres, R. Mochkovitch, Margarita Hernanz, and Jordi Isern
Subjects: Physics, education.field_of_study, Astrophysics (astro-ph), Population, Dark matter, FOS: Physical sciences, White dwarf, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Luminosity, Galactic halo, Apparent magnitude, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Halo, education, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy)
Abstract: Halo white dwarfs can provide important information about the properties and evolution of the galactic halo. In this paper we compute, assuming a standard IMF and updated models of white dwarf cooling, the expected luminosity function, both in luminosity and in visual magnitude, for different star formation rates. We show that a deep enough survey (limiting magnitude > 20) could provide important information about the halo age and the duration of the formation stage. We also show that the number of white dwarfs produced using the recently proposed biased IMFs cannot represent a large fraction of the halo dark matter if they are constrained by the presently observed luminosity function. Furthermore, we show that a robust determination of the bright portion of the luminosity function can provide strong constraints on the allowable IMF shapes., 29 pages (AASTeX), 7 eps figures included, accepted for publication in ApJ
Published: 1998

36. Highlights of Spanish Astrophysics IV : Proceedings of the Seventh Scientific Meeting of the Spanish Astronomical Society (SEA) Held in Barcelona, Spain, September 12-15, 2006

Author: Francesca Figueras, Josep Miquel Girart, Margarita Hernanz, Carme Jordi, Francesca Figueras, Josep Miquel Girart, Margarita Hernanz, and Carme Jordi
Subjects: Astronomy--Research--Spain--Congresses, Astrophysics, Astrophysics--Research--Spain--Congresses, Astrophysics--Congresses, Astronomy--Congresses
Abstract: This volume documents the contributions presented at the Seventh Scientific Meeting of the Spanish Astronomical Society (Sociedad Española de Astronomía, SEA). The event bought together 301 participants who presented 161 contributed talks and 120 posters, the greatest numbers up to now. The fact that most exciting items of the current astronomical research were addressed in the meeting proofs the good health of the SEA, a consolidated organization founded fifteen years ago in Barcelona. Two plenary sessions of the meeting were devoted to the approved entrance of Spain as a full member of the European Southern Observatory (ESO) and to the imminent first light of the greatest telescope in the world, the GTC (Gran Telescopio de Canarias), milestones that will certainly lead the Spanish Astronomy in the next future.
Published: 2007

37. Nucleosynthesis in classical nova explosions.

Author: Jordi Jos, é and, and Margarita Hernanz
Subjects: COSMOCHEMISTRY, CHEMICAL elements, NUCLEAR physics, PHYSICAL sciences
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 g-ray astronomy, such as 7Li, 22Na or 26Al, and the potential discovery of presolar meteoritic grains likely condensed in nova shells. [ABSTRACT FROM AUTHOR]
Published: 2007
Full Text: View/download PDF

38. X-Ray Flashes in Recurrent Novae: M31N 2008-12a and the Implications of the Swift Non-detection

Author: Allen W. Shafter, Michael F. Bode, Jan-Uwe Ness, J. A. Kennea, Mariko Kato, Izumi Hachisu, M. J. Darnley, K. L. Page, Martin Henze, J. P. Osborne, Hideyuki Saio, Neil Gehrels, and Margarita Hernanz
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, White dwarf, Astronomy and Astrophysics, Context (language use), Astrophysics, Nova (laser), Light curve, 01 natural sciences, Stars, Flash (photography), Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Binary star, Variable star, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, QB
Abstract: Models of nova outbursts suggest that an X-ray flash should occur just after hydrogen ignition. However, this X-ray flash has never been observationally confirmed. We present four theoretical light curves of the X-ray flash for two very massive white dwarfs (WDs) of 1.380 and 1.385 M_sun and for two recurrence periods of 0.5 and 1 years. The duration of the X-ray flash is shorter for a more massive WD and for a longer recurrence period. The shortest duration of 14 hours (0.6 days) among the four cases is obtained for the 1.385 M_sun WD with one year recurrence period. In general, a nova explosion is relatively weak for a very short recurrence period, which results in a rather slow evolution toward the optical peak. This slow timescale and the predictability of very short recurrence period novae give us a chance to observe X-ray flashes of recurrent novae. In this context, we report the first attempt, using the Swift observatory, to detect an X-ray flash of the recurrent nova M31N 2008-12a (0.5 or 1 year recurrence period), which resulted in the non-detection of X-ray emission during the period of 8 days before the optical detection. We discuss the impact of these observations on nova outburst theory. The X-ray flash is one of the last frontiers of nova studies and its detection is essentially important to understand the pre-optical-maximum phase. We encourage further observations., Comment: 12 pages, including 9 figures and 3 tables. To appear in the Astrophysical Journal

39. X-RAY FLASHES IN RECURRENT NOVAE: M31N 2008-12a AND THE IMPLICATIONS OF THE SWIFT NONDETECTION.

Author: Mariko Kato, Hideyuki Saio, Martin Henze, Jan-Uwe Ness, Julian P. Osborne, Kim L. Page, Matthew J. Darnley, Michael F. Bode, Allen W. Shafter, Margarita Hernanz, Neil Gehrels, Jamie Kennea, and Izumi Hachisu
Subjects: X-ray astronomy, WHITE dwarf stars, NOVAE (Astronomy), SPACE astronomy, ASTRONOMY
Abstract: Models of nova outbursts suggest that an X-ray flash should occur just after hydrogen ignition. However, this X-ray flash has never been observationally confirmed. We present four theoretical light curves of the X-ray flash for two very massive white dwarfs (WDs) of 1.380 and 1.385 and for two recurrence periods of 0.5 and 1 yr. The duration of the X-ray flash is shorter for a more massive WD and for a longer recurrence period. The shortest duration of 14 hr (0.6 days) among the four cases is obtained for the WD with a 1 yr recurrence period. In general, a nova explosion is relatively weak for a very short recurrence period, which results in a rather slow evolution toward the optical peak. This slow timescale and the predictability of very short recurrence period novae give us a chance to observe X-ray flashes of recurrent novae. In this context, we report the first attempt, using the Swift observatory, to detect an X-ray flash of the recurrent nova M31N 2008-12a (0.5 or 1 yr recurrence period), which resulted in the nondetection of X-ray emission during the period of 8 days before the optical detection. We discuss the impact of these observations on nova outburst theory. The X-ray flash is one of the last frontiers of nova studies, and its detection is essential for understanding the pre-optical-maximum phase. We encourage further observations. [ABSTRACT FROM AUTHOR]
Published: 2016
Full Text: View/download PDF

40. 10 Gyr of classical nova explosions.

Author: Jordi Jos, é and, and Margarita Hernanz
Subjects: NOVAE (Astronomy), STELLAR activity, DWARF stars, NUCLEOSYNTHESIS
Abstract: Classical novae are stellar explosions in cataclysmic binary systems, consisting of a compact white dwarf star (CO or ONe-rich) and a low-mass, main-sequence companion (typically, a K or M dwarf of solar composition). The system is close enough (orbital periods ranging between 1 and 15 h), hence allowing mass transfer episodes driven by overflows of the companion star. This matter flow forms an accretion disk that surrounds the white dwarf, and ultimately accumulates on its surface (at a rate M = 10[?]9-10[?]10 M[?] yr[?]1), building up an envelope under semi-degenerate conditions until a violent thermonuclear runaway ensues. Classical novae are believed to be major sources of the Galactic 15N, 17O and 13C, with a minor contribution on a number of additional species, mainly 7Li and 26Al. But there are reasons to believe that these nucleosynthetic features have varied during the overall 10 Gyr of Galactic history. In this paper, we review recent progress on the characterization of primordial novae, that is, novae exploding in primordial cataclysmic binaries, and will compare their expected nucleosynthetic pattern with that of classical novae. Emphasis is made on the dominant nuclear paths during the explosion and on a thorough comparison with other explosive sites, such as type-I x-ray bursts. [ABSTRACT FROM AUTHOR]
Published: 2008
Full Text: View/download PDF

41. WSO/UV: World Space Observatory/Ultraviolet

Author: Solheim, Jan Erik, Hernanza, M., González-Riestra, R., Wamsteker, W., Shustov, B., Barstow, M., Brosch, N., Fu-Zhen, C., Dennefeld, M., Dopita, M., Gómez de Castro, A.I., Kappelmannc, N.l., Pagano, I., Sahade, J., Haubold, H., Solheim, J.-E., Martínezc, P., arXiv, Import, Margarita Hernanz and Jordi José, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, 020301 aerospace & aeronautics, 010504 meteorology & atmospheric sciences, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy, 02 engineering and technology, Astrophysics, medicine.disease_cause, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], VDP::Mathematics and natural science: 400::Physics: 430::Astrophysics, astronomy: 438, 0203 mechanical engineering, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Observatory, medicine, Ultraviolet, World space, 0105 earth and related environmental sciences
Abstract: We summarize the capabilities of the World Space Observatory (UV) Project (WSO/UV). An example of the importance of this project (with a planned launch date of 2007/8) for the study of Classical Novae is given., Comment: 4 pages, To appear in the proceeedings of the "Classical Nova Explosions" conference, eds. M. Hernanz and J. Jose, AIP
Published: 2002

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Category

Publication Type

Journal

Database

Publisher

41 results on '"Margarita Hernanz"'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources