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43 results on '"di Salvo, Tiziana"'

1. First detection of X-ray polarization from the accreting neutron star 4U 1820-303

Author: Di Marco, Alessandro, La Monaca, Fabio, Poutanen, Juri, Russell, Thomas D., Anitra, Alessio, Farinelli, Ruben, Mastroserio, Guglielmo, Muleri, Fabio, Xie, Fei, Bachetti, Matteo, Burderi, Luciano, Carotenuto, Francesco, Del Santo, Melania, Di Salvo, Tiziana, Dovciak, Michal, Gnarini, Andrea, Iaria, Rosario, Kajava, Jari J. E., Liu, Kuan, Middei, Riccardo, O'Dell, Stephen L., Pilia, Maura, Rankin, John, Sanna, Andrea, Eijnden, Jakob van den, Weisskopf, Martin C., Bobrikova, Anna, Capitanio, Fiamma, Costa, Enrico, Kaaret, Philip, Marino, Alessio, Soffitta, Paolo, Ursini, Francesco, Ambrosino, Filippo, Cocchi, Massimo, Fabiani, Sergio, Marshall, Herman L., Matt, Giorgio, Motta, Sara Elisa, Papitto, Alessandro, Stella, Luigi, Tarana, Antonella, Zane, Silvia, Agudo, Ivan, Antonelli, Lucio A., Baldini, Luca, Baumgartner, Wayne H., Bellazzini, Ronaldo, Bianchi, Stefano, Bongiorno, Stephen D., Bonino, Raffaella, Brez, Alessandro, Bucciantini, Niccolo, Castellano, Simone, Cavazzuti, Elisabetta, Chen, Chien-Ting, Ciprini, Stefano, De Rosa, Alessandra, Del Monte, Ettore, Di Gesu, Laura, Di Lalla, Niccolo, Donnarumma, Immacolata, Doroshenko, Victor, Ehlert, Steven R., Enoto, Teruaki, Evangelista, Yuri, Ferrazzoli, Riccardo, Garcia, Javier A., Gunji, Shuichi, Hayashida, Kiyoshi, Heyl, Jeremy, Iwakiri, Wataru, Jorstad, Svetlana G., Karas, Vladimir, Kislat, Fabian, Kitaguchi, Takao, Kolodziejczak, Jeffery J., Krawczynski, Henric, Latronico, Luca, Liodakis, Ioannis, Maldera, Simone, Manfreda, Alberto, Marin, Frederic, Marinucci, Andrea, Marscher, Alan P., Massaro, Francesco, Mitsuishi, Ikuyuki, Mizuno, Tsunefumi, Negro, Michela, Ng, Chi-Yung, Omodei, Nicola, Oppedisano, Chiara, Pavlov, George G., Peirson, Abel L., Perri, Matteo, Pesce-Rollins, Melissa, Petrucci, Pierre-Olivier, Possenti, Andrea, Puccetti, Simonetta, Ramsey, Brian D., Ratheesh, Ajay, Roberts, Oliver J., Romani, Roger W., Sgrò, Carmelo, Slane, Patrick, Spandre, Gloria, Swartz, Douglas A., Tamagawa, Toru, Tavecchio, Fabrizio, Taverna, Roberto, Tawara, Yuzuru, Tennant, Allyn F., Thomas, Nicholas E., Tombesi, Francesco, Trois, Alessio, Tsygankov, Sergey S., Turolla, Roberto, Vink, Jacco, and Wu, Kinwah
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract: This paper reports the first detection of polarization in the X-rays for atoll-source 4U 1820-303, obtained with the Imaging X-ray Polarimetry Explorer (IXPE) at 99.999% confidence level (CL). Simultaneous polarimetric measurements were also performed in the radio with the Australia Telescope Compact Array (ATCA). The IXPE observations of 4U 1820-303 were coordinated with Swift-XRT, NICER, and NuSTAR aiming to obtain an accurate X-ray spectral model covering a broad energy interval. The source shows a significant polarization above 4 keV, with a polarization degree of 2.0(0.5)% and a polarization angle of -55(7) deg in the 4-7 keV energy range, and a polarization degree of 10(2)% and a polarization angle of -67(7) deg in the 7-8 keV energy bin. This polarization also shows a clear energy trend with polarization degree increasing with energy and a hint for a position-angle change of about 90 deg at 96% CL around 4 keV. The spectro-polarimetric fit indicates that the accretion disk is polarized orthogonally to the hard spectral component, which is presumably produced in the boundary/spreading layer. We do not detect linear polarization from the radio counterpart, with a 99.97% upper limit of 50% at 7.25 GHz.
Published: 2023
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2. Timing Analysis of the 2022 Outburst of SAX J1808.4-3658: Hints of Orbital Decay

Author: ILLIANO, GIULIA, PAPITTO, ALESSANDRO, SANNA, ANDREA, Bult, Peter, AMBROSINO, Filippo, MIRAVAL ZANON, ARIANNA, Coti Zelati, Francesco, STELLA, Luigi, Altamirano, Diego, Baglio, Maria Cristina, BOZZO , ENRICO, BURDERI, LUCIANO, DE MARTINO, Domitilla, DI MARCO, ALESSANDRO, Di Salvo, Tiziana, Ferrigno, Carlo, Loktev, Vladislav, MARINO, ALESSIO, Ng, Mason, PILIA, Maura, Poutanen, Juri, Salmi, Tuomo, and ITA
Abstract: We present a pulse timing analysis of NICER observations of the accreting millisecond X-ray pulsar SAX J1808.4−3658 during the outburst that started on 2022 August 19. Similar to previous outbursts, after decaying from a peak luminosity of ≃1 × 1036 erg s−1 in about a week, the pulsar entered a ∼1 month long reflaring stage. Comparison of the average pulsar spin frequency during the outburst with those previously measured confirmed the long-term spin derivative of ${\dot{\nu }}_{\mathrm{SD}}=-(1.15\,\pm \,0.06)\times \,{10}^{-15}$ Hz s−1, compatible with the spin-down torque of a ≈1026 G cm3 rotating magnetic dipole. For the first time in the last twenty years, the orbital phase evolution shows evidence for a decrease of the orbital period. The long-term behavior of the orbit is dominated by an ∼11 s modulation of the orbital phase epoch consistent with a ∼21 yr period. We discuss the observed evolution in terms of a coupling between the orbit and variations in the mass quadrupole of the companion star.
Published: 2023

3. Fe Kα and Fe Kβ line detection in the NuSTAR spectrum of the ultra-bright Z-source Scorpius X-1

Author: Mazzola, Simona Michela, Iaria, Rosario, Di Salvo, Tiziana, Sanna, Andrea, Gambino, Angelo Francesco, Marino, Alessio, Bozzo, Enrico, Ferrigno, Carlo, Riggio, Alessandro, Anitra, Alessio, and Burderi, Luciano
Subjects: Astrophysics::High Energy Astrophysical Phenomena, stars: neutron – stars: individual: Scorpius X-1 — X-rays: binaries — Xrays:general — accretion, accretion disks, Astrophysics::Galaxy Astrophysics
Abstract: Low-mass X-ray binaries hosting a low-magnetised neutron star, which accretes matter via Roche-lobe overflow, are generally grouped in two classes, named Atoll and Z sources after the path described in their X-ray colour-colour diagrams. Scorpius X-1 is the brightest persistent low-mass X-ray binary known so far, and it isthe prototype of the Z sources. We analysed the first NuSTAR observation of this source to study its spectral emission exploiting the high statistics data collected by this satellite. Examining the colour-colour diagram, the source was probably observed during the lower normal and flaring branches of its Z-track. We separated the data from the two branches in order to investigate the evolution of the source along the track. We fitted the 3-60 keV NuSTAR spectra using the same models for both the branches. We adopted two description for the continuum: in the first case we used a blackbody and a thermal Comptonisation with seed photons originating in the accretiondisc; in the second one, we adopted a disc-blackbody and a Comptonisation with a blackbody-shaped spectrum of the incoming seed photons. A power-law fitting the high energy emission above 20 keV was also required in both cases. The two models provide the same physical scenario for the source in both the branches: a blackbody temperature between 0.8 and 1.5 keV, a disc-blackbody with temperature between 0.4 and 0.6 keV, and an optically thick Comptonising corona with optical depth between 6 and 10 and temperature about 3 keV. Furthermore, two lines related to the Kα and Kβ transitions of the He-like Fe XXVions were detected at 6.6 keV and 7.8 keV, respectively. A hard tail modelled by a power law with a photon index between 2 and 3 was also required for both the models.
Published: 2021
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4. Accretion in strong field gravity with eXTP

Author: De Rosa, Alessandra, Uttley, Phil, Gou, Lijun, Liu, Yuan, Bambi, Cosimo, Barret, Didier, Belloni, Tomaso, Berti, Emanuele, Bianchi, Stefano, Caiazzo, Ilaria, Casella, Piergiorgio, Feroci, Marco, Ferrari, Valeria, Gualtieri, Leonardo, Heyl, Jeremy, Ingram, Adam, Karas, Vladimir, Lu, Fangjun, Luo, Bin, Matt, Giorgio, Motta, Sara, Neilsen, Joseph, Pani, Paolo, Santangelo, Andrea, Shu, Xinwen, Wang, Junfeng, Wang, Jian-Min, Xue, Yongquan, Xu, Yupeng, Yuan, Weimin, Yuan, Yefei, Zhang, Shuang-Nan, Zhang, Shu, Agudo, Ivan, Amati, Lorenzo, Andersson, Nils, Baglio, Cristina, Bakala, Pavel, Baykal, Altan, Bhattacharyya, Sudip, Bombaci, Ignazio, Bucciantini, Niccolò, Capitanio, Fiamma, Ciolfi, Riccardo, Cui, Wei K., D'Ammando, Filippo, Dauser, Thomas, Del Santo, Melania, De Marco, Barbara, Di Salvo, Tiziana, Done, Chris, Dovčiak, Michal, Fabian, Andrew C., Falanga, Maurizio, Gambino, Angelo Francesco, Gendre, Bruce, Grinberg, Victoria, Heger, Alexander, Homan, Jeroen, Iaria, Rosario, Jiang, Jiachen, Jin, Chichuan, Koerding, Elmar, Linares, Manu, Liu, Zhu, Maccarone, Thomas J., Malzac, Julien, Manousakis, Antonios, Marin, Frédéric, Marinucci, Andrea, Mehdipour, Missagh, Méndez, Mariano, Migliari, Simone, Miller, Cole, Miniutti, Giovanni, Nardini, Emanuele, O'Brien, Paul T., Osborne, Julian P., Petrucci, Pierre Olivier, Possenti, Andrea, Riggio, Alessandro, Rodriguez, Jerome, Sanna, Andrea, Shao, Lijing, Sobolewska, Malgosia, Sramkova, Eva, Stevens, Abigail L., Stiele, Holger, Stratta, Giulia, Stuchlik, Zdenek, Svoboda, Jiri, Tamburini, Fabrizio, Tauris, Thomas M., Tombesi, Francesco, Török, Gabriel, Urbanec, Martin, Vincent, Frederic, Wu, Qingwen, Yuan, Feng, in't Zand, Jean J. M., Zdziarski, Andrzej A., Zhou, Xinlin, Rosa, Alessandra De, Cui, Wei, D’Ammando, Filippo, Fabian, Andrew, Maccarone, Thomas, O’Brien, Paul, Osborne, Julian, Stevens, Abigail, Tauris, Thomas, in’ t Zand, Jean, Zdziarski, Andrzej, School of Physics and Astronomy [Southampton], University of Southampton, Sécurité des Données et des Systèmes (SDS), Laboratoire d'Informatique Fondamentale d'Orléans (LIFO), Université d'Orléans (UO)-Institut National des Sciences Appliquées - Centre Val de Loire (INSA CVL), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université d'Orléans (UO)-Institut National des Sciences Appliquées - Centre Val de Loire (INSA CVL), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Fudan University [Shanghai], 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), Osservatorio Astronomico di Brera, Istituto Nazionale di Astrofisica (INAF), Department of Physics and Astronomy [U Mississippi], The University of Mississippi [Oxford], IASF, Area di Ricerca di Tor Vergata, Astronomical Institute of the Czech Academy of Sciences, Czech Academy of Sciences [Prague] (ASCR), Key Laboratory of Western China's Environmental Systems (Ministry of Education), Lanzhou University, Dipartimento de Fisica Roma Tre (DF-Roma3), Università degli Studi Roma Tre, Sichuan University, U.S. Department of Energy (DOE), Medical School (University of Nanjing), Nanjing University (NJU), Faculty of Philosophy and Science, Silesian University in Opava, INAF - Osservatorio Astrofisico di Arcetri (OAA), Instituto di Astrofisica (IASF), Consiglio Nazionale delle Ricerche (CNR), Istituto di Radioastronomia (IRA), Department of Physics, Durham University, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Eberhard Karls Universität Tübingen, State Key Laboratory of Magnetic Resonance and Atomic and Molecular Physics, Wuhan Institute of Physics and Mathematics, Chinese Academy of Sciences, Wuhan, 430071 China, Chinese Academy of Sciences [Wuhan Branch], Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), Biogéosciences [UMR 6282] [Dijon] (BGS), Centre National de la Recherche Scientifique (CNRS)-Université de Bourgogne (UB)-AgroSup Dijon - Institut National Supérieur des Sciences Agronomiques, de l'Alimentation et de l'Environnement, European Space Astronomy Centre (ESAC), European Space Agency (ESA), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Cagliari (OAC), 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), Ethoikos, Radicondoli, ASI Science Data Center (ASDC), Italian Space Agency, Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Technologie de Belfort-Montbeliard (UTBM), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Department of Applied Biology and Chemical Technology, The Hong Kong Polytechnic University [Hong Kong] (POLYU), Max-Planck-Institut für Radioastronomie (MPIFR), Centre National de la Recherche Scientifique (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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), eXTP, Institut National des Sciences Appliquées - Centre Val de Loire (INSA CVL), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université d'Orléans (UO), Université de Bourgogne (UB)-AgroSup Dijon - Institut National Supérieur des Sciences Agronomiques, de l'Alimentation et de l'Environnement-Centre National de la Recherche Scientifique (CNRS), 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), Institute of High Energy Physics [Beijing], 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), INAF - Osservatorio Astronomico di Brera (OAB), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Università degli Studi Roma Tre = Roma Tre University (ROMA TRE), Sichuan University [Chengdu] (SCU), U.S. Department of Energy [Washington] (DOE), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Istituto di Radioastronomia [Bologna] (IRA), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Eberhard Karls Universität Tübingen = Eberhard Karls University of Tuebingen, Biogéosciences [UMR 6282] (BGS), Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS), Agence Spatiale Européenne = European Space Agency (ESA), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), De Rosa, Alessandra, Uttley, Phil, Gou, LiJun, Liu, Yuan, Bambi, Cosimo, Barret, Didier, Belloni, Tomaso, Berti, Emanuele, Bianchi, Stefano, Caiazzo, Ilaria, Casella, Piergiorgio, Feroci, Marco, Ferrari, Valeria, Gualtieri, Leonardo, Heyl, Jeremy, Ingram, Adam, Karas, Vladimir, Lu, FangJun, Luo, Bin, Matt, Giorgio, Motta, Sara, Neilsen, Joseph, Pani, Paolo, Santangelo, Andrea, Shu, XinWen, Wang, JunFeng, Wang, Jian-Min, Xue, YongQuan, Xu, YuPeng, Yuan, WeiMin, Yuan, YeFei, Zhang, Shuang-Nan, Zhang, Shu, Agudo, Ivan, Amati, Lorenzo, Andersson, Nil, Baglio, Cristina, Bakala, Pavel, Baykal, Altan, Bhattacharyya, Sudip, Bombaci, Ignazio, Bucciantini, Niccoló, Capitanio, Fiamma, Ciolfi, Riccardo, Cui, Wei K., D’Ammando, Filippo, Dauser, Thoma, Del Santo, Melania, De Marco, Barbara, Di Salvo, Tiziana, Done, Chri, Dovčiak, Michal, Fabian, Andrew C., Falanga, Maurizio, Gambino, Angelo Francesco, Gendre, Bruce, Grinberg, Victoria, Heger, Alexander, Homan, Jeroen, Iaria, Rosario, Jiang, JiaChen, Jin, ChiChuan, Koerding, Elmar, Linares, Manu, Liu, Zhu, Maccarone, Thomas J., Malzac, Julien, Manousakis, Antonio, Marin, Frédéric, Marinucci, Andrea, Mehdipour, Missagh, Méndez, Mariano, Migliari, Simone, Miller, Cole, Miniutti, Giovanni, Nardini, Emanuele, O’Brien, Paul T., Osborne, Julian P., Petrucci, Pierre Olivier, Possenti, Andrea, Riggio, Alessandro, Rodriguez, Jerome, Sanna, Andrea, Shao, LiJing, Sobolewska, Malgosia, Sramkova, Eva, Stevens, Abigail L., Stiele, Holger, Stratta, Giulia, Stuchlik, Zdenek, Svoboda, Jiri, Tamburini, Fabrizio, Tauris, Thomas M., Tombesi, Francesco, Torok, Gabriel, Urbanec, Martin, Vincent, Frederic, Wu, QingWen, Yuan, Feng, in’ t Zand, Jean J. M., Zdziarski, Andrzej A., Zhou, XinLin, ITA, USA, GBR, FRA, DEU, 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), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Chinese Academy of Sciences (CAS), National Science Centre, Poland (NCN), High Energy Astrophys. & Astropart. Phys (API, FNWI), Rosa, Alessandra De, Gou, Lijun, Lu, Fangjun, Shu, Xinwen, Wang, Junfeng, Xue, Yongquan, Xu, Yupeng, Yuan, Weimin, Yuan, Yefei, Jiang, Jiachen, Jin, Chichuan, Shao, Lijing, Wu, Qingwen, and Zhou, Xinlin
Subjects: ACTIVE GALACTIC NUCLEI, Accretion, accretion, black holes physics, X-ray, Physics and Astronomy (all), black holes physic, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Black holes physics, Polarimetry, FOS: Physical sciences, BLACK-HOLE SPIN, General Physics and Astronomy, Strong field, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, ELECTROMAGNETIC EMISSION, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), XMM-NEWTON, Physics, LENS-THIRRING PRECESSION, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], QUASI-PERIODIC OSCILLATIONS, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], IRON K, Accretion (astrophysics), X ray, [SDU]Sciences of the Universe [physics], ULTRA-FAST OUTFLOWS, Astrophysics::Earth and Planetary Astrophysics, SPECTRAL FEATURES, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], X-RAY BINARIES
Abstract: In this paper we describe the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to accretion flows in the strong field gravity regime around both stellar-mass and supermassive black-holes. eXTP has the unique capability of using advanced 'spectral-timing-polarimetry' techniques to analyze the rapid variations with three orthogonal diagnostics of the flow and its geometry, yielding unprecedented insight into the inner accreting regions, the effects of strong field gravity on the material within them and the powerful outflows which are driven by the accretion process., Accepted for publication on Sci. China Phys. Mech. Astron. (2019)
Published: 2019
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5. Observatory science with eXTP

Author: in't Zand, Jean J. M., Bozzo, Enrico, Qu, Jinlu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, De Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, Xuefeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, Joao, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, Chichuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D'Aì, Antonino, Dai, Zi-Gao, D'Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D'Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, Xilong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, Mingyu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Laurens, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, Fangjun, Lutovinov, Alexander A., Malyshev, Denys, Malzac, Julien, Manousakis, Antonios, McHardy, Ian, Mehdipour, Missagh, Men, Yunpeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joonas, Nardini, Emanuele, Neubert, Torsten, O'Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuomas, Schanne, Stéphane, Schatz, Hendrik, Shao, Lijing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jir̆í, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, Junfeng, Watts, Anna L., Weng, Shanshan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, Shaolin, Xu, Yupeng, Yan, Zhen, Younes, George, Yu, Wenfei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, Zingale, Michael, in ’t Zand, Jean, Drake, Stephen, Jenke, Peter, Maccarone, Thomas, Rossi, Elena, Tauris, Thomas, Andersson, Nils, Ballantyne, David, Brown, Edward, Cackett, Edward, D’Aì, Antonino, D’Ammando, Filippo, D’Elia, Valerio, Ferdman, Robert, Galloway, Duncan, Gambino, Angelo, Heinke, Craig, Jonker, Peter, Kaastra, Jelle, Lutovinov, Alexander, Mignani, Roberto, O’Brien, Paul, Osborne, Julian, Papadakis, Iossif, Pérez Torres, Miguel, Shore, Steven, Stappers, Ben, Strohmayer, Tod, Suleimanov, Valery, Torres, Diego, Watts, Anna, Weinberg, Nevin, Wheatley, Peter, Woods, Tyrone, Woosley, Stan, Zdziarski, Andrzej, in ’t Zand, Jean J. M., Bozzo, Enrico, Qu, JinLu, Li, Xiang-Dong, Amati, Lorenzo, Chen, Yang, Donnarumma, Immacolata, Doroshenko, Victor, Drake, Stephen A., Hernanz, Margarita, Jenke, Peter A., Maccarone, Thomas J., Mahmoodifar, Simin, de Martino, Domitilla, De Rosa, Alessandra, Rossi, Elena M., Rowlinson, Antonia, Sala, Gloria, Stratta, Giulia, Tauris, Thomas M., Wilms, Joern, Wu, XueFeng, Zhou, Ping, Agudo, Iván, Altamirano, Diego, Atteia, Jean-Luc, Andersson, Nils A., Baglio, M. Cristina, Ballantyne, David R., Baykal, Altan, Behar, Ehud, Belloni, Tomaso, Bhattacharyya, Sudip, Bianchi, Stefano, Bilous, Anna, Blay, Pere, Braga, João, Brandt, Søren, Brown, Edward F., Bucciantini, Niccolò, Burderi, Luciano, Cackett, Edward M., Campana, Riccardo, Campana, Sergio, Casella, Piergiorgio, Cavecchi, Yuri, Chambers, Frank, Chen, Liang, Chen, Yu-Peng, Chenevez, Jérôme, Chernyakova, Maria, Jin, ChiChuan, Ciolfi, Riccardo, Costantini, Elisa, Cumming, Andrew, D’Aì, Antonino, Dai, Zi-Gao, D’Ammando, Filippo, De Pasquale, Massimiliano, Degenaar, Nathalie, Del Santo, Melania, D’Elia, Valerio, Di Salvo, Tiziana, Doyle, Gerry, Falanga, Maurizio, Fan, XiLong, Ferdman, Robert D., Feroci, Marco, Fraschetti, Federico, Galloway, Duncan K., Gambino, Angelo F., Gandhi, Poshak, Ge, MingYu, Gendre, Bruce, Gill, Ramandeep, Götz, Diego, Gouiffès, Christian, Grandi, Paola, Granot, Jonathan, Güdel, Manuel, Heger, Alexander, Heinke, Craig O., Homan, Jeroen, Iaria, Rosario, Iwasawa, Kazushi, Izzo, Luca, Ji, Long, Jonker, Peter G., José, Jordi, Kaastra, Jelle S., Kalemci, Emrah, Kargaltsev, Oleg, Kawai, Nobuyuki, Keek, Lauren, Komossa, Stefanie, Kreykenbohm, Ingo, Kuiper, Lucien, Kunneriath, Devaky, Li, Gang, Liang, En-Wei, Linares, Manuel, Longo, Francesco, Lu, FangJun, Lutovinov, Alexander A., Malyshev, Deny, Malzac, Julien, Manousakis, Antonio, McHardy, Ian, Mehdipour, Missagh, Men, YunPeng, Méndez, Mariano, Mignani, Roberto P., Mikusincova, Romana, Miller, M. Coleman, Miniutti, Giovanni, Motch, Christian, Nättilä, Joona, Nardini, Emanuele, Neubert, Torsten, O’Brien, Paul T., Orlandini, Mauro, Osborne, Julian P., Pacciani, Luigi, Paltani, Stéphane, Paolillo, Maurizio, Papadakis, Iossif E., Paul, Biswajit, Pellizzoni, Alberto, Peretz, Uria, Pérez Torres, Miguel A., Perinati, Emanuele, Prescod-Weinstein, Chanda, Reig, Pablo, Riggio, Alessandro, Rodriguez, Jerome, Rodríguez-Gil, Pablo, Romano, Patrizia, Różańska, Agata, Sakamoto, Takanori, Salmi, Tuomo, Salvaterra, Ruben, Sanna, Andrea, Santangelo, Andrea, Savolainen, Tuoma, Schanne, Stéphane, Schatz, Hendrik, Shao, LiJing, Shearer, Andy, Shore, Steven N., Stappers, Ben W., Strohmayer, Tod E., Suleimanov, Valery F., Svoboda, Jirí, Thielemann, F.-K., Tombesi, Francesco, Torres, Diego F., Torresi, Eleonora, Turriziani, Sara, Vacchi, Andrea, Vercellone, Stefano, Vink, Jacco, Wang, Jian-Min, Wang, JunFeng, Watts, Anna L., Weng, ShanShan, Weinberg, Nevin N., Wheatley, Peter J., Wijnands, Rudy, Woods, Tyrone E., Woosley, Stan E., Xiong, ShaoLin, Xu, YuPeng, Yan, Zhen, Younes, George, Yu, WenFei, Yuan, Feng, Zampieri, Luca, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Shuang-Nan, Zhang, Shu, Zhang, Shuo, Zhang, Xiao, Zingale, Michael, Institut de recherche en astrophysique et planétologie (IRAP), 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), 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), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), eXTP, Centre National de la Recherche Scientifique (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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), 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 de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre de Recherche en Information Biomédicale sino-français (CRIBS), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Southeast University [Jiangsu]-Institut National de la Santé et de la Recherche Médicale (INSERM), Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), ASI Science Data Center (ASDC), Italian Space Agency, INAF - Osservatorio Astronomico di Brera (OAB), Istituto Nazionale di Astrofisica (INAF), Laboratoire d'Anthropobiologie (LA), École des hautes études en sciences sociales (EHESS)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), SRON Netherlands Institute for Space Research (SRON), Istituto di Radioastronomia [Bologna] (IRA), KAUST Catalysis Center (KCC), King Abdullah University of Sciences & Technologie, IASF, Area di Ricerca di Tor Vergata, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-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), School of Physics and Astronomy [Southampton], University of Southampton, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut für Astrophysik [Wien], Universität Wien, Sabanci University [Istanbul], The George Washington University (GW), Department of Physics, Tokyo Institute of Technology [Tokyo] (TITECH), Deakin University [Burwood], Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), University of New Hampshire (UNH), Department of Mechanical and Industrial Engineering [Trondheim] (MTP NTNU), Norwegian University of Science and Technology [Trondheim] (NTNU), Norwegian University of Science and Technology (NTNU)-Norwegian University of Science and Technology (NTNU), Ethoikos, Radicondoli, Jodrell Bank Centre for Astrophysics, University of Manchester [Manchester], Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Sichuan University [Chengdu] (SCU), University of Warwick [Coventry], U.S. Department of Energy [Washington] (DOE), University College of London [London] (UCL), Medical School (University of Nanjing), Nanjing University (NJU), Beijing Municipal Climate Center, Max-Planck-Institut für Radioastronomie (MPIFR), Laboratorio de Investigación y Formación en Informática Avanzada [La Plata] (LIFIA), Facultad de Informática [La Plata], Universidad Nacional de la Plata [Argentine] (UNLP)-Universidad Nacional de la Plata [Argentine] (UNLP), NLD, Unidad de Excelencia Científica María de Maeztu Instituto de Ciencias del Cosmos (ICCUB), MDM-2014-0369, National Natural Science Foundation of China (NSFC), European Research Council (ERC), National Aeronautics and Space Administration (NASA), Agencia Estatal de Investigación (AEI), Royal Society, Strategic Priority Research Program of the Chinese Academy of Sciences, National Science Centre, Poland (NCN), 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), Royal Society (UK), European Research Council, European Commission, National Natural Science Foundation of China, National Basic Research Program (China), National Science Foundation (US), Ministerio de Economía y Competitividad (España), Polish Academy of Sciences, Astronomy, Discrete Technology and Production Automation, in't Zand, Jean J. M., Qu, Jinlu, Tauris, Thomas M., Wilm, Joern, Wu, Xuefeng, Jin, Chichuan, D'Aì, Antonino, D'Ammando, Filippo, D'Elia, Valerio, Fan, Xilong, Ge, Mingyu, Lu, Fangjun, Mchardy, Ian, Men, Yunpeng, O'Brien, Paul T., Shao, Lijing, Svoboda, Jir̆í, Thielemann, F. -K., Wang, Junfeng, Weng, Shanshan, Xiong, Shaolin, Xu, Yupeng, Yu, Wenfei, Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, Institut de Mathématiques de Toulouse UMR5219 (IMT), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse 1 Capitole (UT1)-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Osservatorio Astronomico di Brera, Istituto di Radioastronomia (IRA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), George Washington University (GW), Department of Mechanical and Industrial Engineering [Trondheim], Sichuan University, U.S. Department of Energy (DOE), Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Météo France-Université Toulouse III - Paul Sabatier (UT3), SRON Netherlands Institute for Space Research, University of Geneva, CAS - Institute of High Energy Physics, Nanjing University, INAF/IASF Bologna, National Institute for Astrophysics, University of Tübingen, NASA Goddard Space Flight Center, ICREA, University of Alabama in Huntsville, Texas Tech University, Osservatorio Astronomico di Capodimonte, Leiden University, University of Amsterdam, Polytechnic University of Catalonia, University of Urbino, Max Planck Institute for Radio Astronomy, Friedrich-Alexander University Erlangen-Nürnberg, CAS - Purple Mountain Observatory, CSIC, IRAP, New York University Abu Dhabi, Georgia Institute of Technology, Middle East Technical University, Technion-Israel Institute of Technology, Tata Institute of Fundamental Research, Roma Tre University, Instituto de Astrofísica de Canarias, Instituto Nacional de Pesquisas Espaciais, Danmarks Tekniske Universitet, Michigan State University, Osservatorio Astrofisico Di Arcetri, Florence, University of Cagliari, Wayne State University, Osservatorio Astronomico Roma, CAS - Shanghai Astronomical Observatory, Department of Electronics and Nanoengineering, Aalto-yliopisto, and Aalto University
Subjects: cataclysmic binaries, Astronomy, FIELD CAMERAS OBSERVATIONS, space research instruments nuclear astrophysics flare stars accretion and accretion disks mass loss and stellar winds cataclysmic binaries X-ray binaries supernova remnants active galactic nuclei X-ray bursts gamma-ray bursts gravitational waves, General Physics and Astronomy, gamma-ray burst, space research instrument, 01 natural sciences, Gamma ray bursts, Observatory, Accretion and accretion disks, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, gravitational wave, accretion and accretion disk, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), supernova remnants, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], flare stars, gamma-ray bursts, Astrophysics::Instrumentation and Methods for Astrophysics, accretion and accretion disks, active galactic nuclei, gravitational waves, mass loss and stellar winds, nuclear astrophysics, space research instruments, X-ray binaries, X-ray bursts, Physics and Astronomy (all), Space research instruments, X ray burst, Supernova, QUIET, High mass, X-ray binarie, Mass loss and stellar winds, Nuclear astrophysics, Gamma-ray bursts, Astrophysics - High Energy Astrophysical Phenomena, PULSAR-WIND NEBULAE, FAST RADIO-BURSTS, Astrofísica nuclear, Active galactic nucleus, TIDAL DISRUPTION, Supernova remnants, Astrophysics::High Energy Astrophysical Phenomena, Polarimetry, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, ACCRETING NEUTRON-STARS, Gravitational waves, cataclysmic binarie, Settore FIS/05 - Astronomia e Astrofisica, SUPERMASSIVE BLACK-HOLES, 0103 physical sciences, 010306 general physics, X-ray burst, Astrophysics::Galaxy Astrophysics, Cataclysmic binaries, Active galactic nuclei, flare star, White dwarf, Flare stars, Stars, supernova remnant, QB460-466 Astrophysics, [SDU]Sciences of the Universe [physics], mass loss and stellar wind, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], X-RAY, Supernova remmants, X ray binaries, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SEYFERT 1 GALAXY, nuclear astrophysic
Abstract: Disponible preprint en: arXiv:1812.04023v1 [astro-ph.HE] [v1] Mon, 10 Dec 2018 19:00:52 UTC (4,376 KB), In this White Paper we present the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to Observatory Science targets. These include flaring stars, supernova remnants, accreting white dwarfs, low and high mass X-ray binaries, radio quiet and radio loud active galactic nuclei, tidal disruption events, and gamma-ray bursts. eXTP will be excellently suited to study one common aspect of these objects: their often transient nature. Developed by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s.© 2018, Science China Press and Springer-Verlag GmbH Germany, part of Springer Nature., This work was supported by the Royal Society, ERC Starting (Grant No. 639217), the European Union Horizon 2020 Research and Innovation Programme under the Marie Sklodowska-Curie Global Fellowship (Grant No. 703916), the National Natural Science Foundation of China (Grant Nos. 11233001, 11773014, 11633007, 11403074, 11333005, 11503008, and 11590781), the National Basic Research Program of China (Grant No. 2015CB857100), NASA (Grant No. NNX13AD28A), an ARC Future Fellowship (Grant No. FT120100363), the National Science Foundation (Grant No. PHY-1430152), the Spanish MINECO (Grant No. AYA2016-76012-C3-1-P), the ICCUB (Unidad de Excelencia 'Maria de Maeztu') (Grant No. MDM-2014-0369), EU's Horizon Programme through a Marie Sklodowska-Curie Fellowship (Grant No. 702638), the Polish National Science Center (Grant Nos. 2015/17/B/ST9/03422, 2015/18/M/ST9/00541, 2013/10/M/ST9/00729, and 2015/18/A/ST9/00746), the Strategic Priority Research Program of the Chinese Academy of Sciences (Grant No. XDA15020100), and the NWO Veni Fellowship (Grant No. 639.041.647).
Published: 2019

6. Accretion powered X-ray millisecond pulsars

Author: Di Salvo, Tiziana and Sanna, Andrea
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Neutron Stars are among the most exotic objects in the Universe. A neutron star, with a mass of 1.4-2 Solar masses within a radius of about 10-15 km, is the most compact stable configuration of matter in which degeneracy pressure can still balance gravity, since further compression would lead to gravitational collapse and formation of a black hole. As gravity is extreme, rotation is extreme: neutron stars are the fastest rotating stars known, with periods as short as a millisecond. The presence of a magnetic field not aligned with the rotation axis of the star is the origin of pulsating emission from these sources, which for this reason are dubbed pulsars. The discovery in 1998 of the first Accreting Millisecond X-ray Pulsar, started an exciting season of continuing discoveries. In the last 20 years, thanks to the extraordinary performance of astronomical detectors in the radio, optical, X-ray, and Gamma-ray bands, astrophysicists had the opportunity to thoroughly investigate the so-called Recycling Scenario: the evolutionary path leading to the formation of a Millisecond-spinning Pulsar. In this chapter we review the general properties of Accreting Millisecond X-ray Pulsars, which provide the first evidence that neutron stars are spun up to millisecond periods by accretion of matter and angular momentum from a (low-mass) companion star. We describe the general characteristics of this class of systems with particular attention to their spin and orbital parameters, their short-term and long-term evolution, as well as the information that can be drawn from their X-ray spectra., 26 pages, 5 figures, 2 tables
Published: 2020

7. Neutron Star Radius-to-mass Ratio from Partial Accretion Disc Occultation as Measured through Fe K$��$ Line Profiles

Author: La Placa, Riccardo, Stella, Luigi, Papitto, Alessando, Bakala, Pavel, Di Salvo, Tiziana, Falanga, Maurizio, De Falco, Vittorio, and De Rosa, Alessandra
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics
Abstract: We present a new method to measure the radius-to-mass ratio (R/M) of weakly magnetic, disc-accreting neutron stars by exploiting the occultation of parts of the inner disc by the star itself. This occultation imprints characteristic features on the X-ray line profile that are unique and are expected to be present in low mass X-ray binary systems seen under inclinations higher than ~65 degrees. We analyse a NuSTAR observation of a good candidate system, 4U 1636-53, and find that X-ray spectra from current instrumentation are unlikely to single out the occultation features owing to insufficient signal-to-noise. Based on an extensive set of simulations we show that large-area X-ray detectors of the future generation could measure R/M to ~2��3% precision over a range of inclinations. Such is the precision in radius determination required to derive tight constraints on the equation of state of ultradense matter and it represents the goal that other methods too aim to achieve in the future., 17 pages, 8 figures; this is a pre-print edition of an article that has been accepted for publication in the Astrophysical Journal
Published: 2020
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8. Dense matter with eXTP

Author: Watts, Anna L., Yu, Wen Fei, Poutanen, Juri, Zhang, Shu, Bhattacharyya, Sudip, Bogdanov, Slavko, Ji, Long, Patruno, Alessandro, Riley, Thomas E., Bakala, Pavel, Baykal, Altan, Bernardini, Federico, Bombaci, Ignazio, Brown, Edward, Cavecchi, Yuri, Chakrabarty, Deepto, Chenevez, Jérôme, Degenaar, Nathalie, Del Santo, Melania, Di Salvo, Tiziana, Doroshenko, Victor, Falanga, Maurizio, Ferdman, Robert D., Feroci, Marco, Gambino, Angelo F., Ge, Ming Yu, Greif, Svenja K., Guillot, Sebastien, Gungor, Can, Hartmann, Dieter H., Hebeler, Kai, Heger, Alexander, Homan, Jeroen, Iaria, Rosario, Zand, Jean in’t, Kargaltsev, Oleg, Kurkela, Aleksi, Lai, Xiao Yu, Li, Ang, Li, Xiang Dong, Li, Zhao Sheng, Linares, Manuel, Lu, Fang Jun, Mahmoodifar, Simin, Méndez, Mariano, Coleman Miller, M., Morsink, Sharon, Nättilä, Joonas, Possenti, Andrea, and Tsang, David
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract: In this White Paper we present the potential of the Enhanced X-ray Timing and Polarimetry (eXTP) mission for determining the nature of dense matter; neutron star cores host an extreme density regime which cannot be replicated in a terrestrial laboratory. The tightest statistical constraints on the dense matter equation of state will come from pulse profile modelling of accretion-powered pulsars, burst oscillation sources, and rotation-powered pulsars. Additional constraints will derive from spin measurements, burst spectra, and properties of the accretion flows in the vicinity of the neutron star. Under development by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Sciences, the eXTP mission is expected to be launched in the mid 2020s.
Published: 2019

9. Accretion in strong field gravity with eXTP

Author: De Rosa, Alessandra, Uttley, Phil, Gou, Li Jun, Liu, Yuan, Bambi, Cosimo, Barret, Didier, Belloni, Tomaso, Berti, Emanuele, Bianchi, Stefano, Caiazzo, Ilaria, Casella, Piergiorgio, Feroci, Marco, Ferrari, Valeria, Gualtieri, Leonardo, Heyl, Jeremy, Ingram, Adam, Karas, Vladimir, Lu, Fang Jun, Luo, Bin, Matt, Giorgio, Motta, Sara, Neilsen, Joseph, Pani, Paolo, Santangelo, Andrea, Shu, Xin Wen, Wang, Jun Feng, Wang, Jian Min, Xue, Yong Quan, Xu, Yu Peng, Yuan, Wei Min, Yuan, Ye Fei, Zhang, Shuang Nan, Zhang, Shu, Agudo, Ivan, Amati, Lorenzo, Andersson, Nils, Baglio, Cristina, Bakala, Pavel, Baykal, Altan, Bhattacharyya, Sudip, Bombaci, Ignazio, Bucciantini, Niccoló, Capitanio, Fiamma, Ciolfi, Riccardo, Cui, Wei K., D’Ammando, Filippo, Dauser, Thomas, Del Santo, Melania, De Marco, Barbara, Di Salvo, Tiziana, Done, Chris, Dovčiak, Michal, Fabian, Andrew C., Falanga, Maurizio, Gambino, Angelo Francesco, Gendre, Bruce, Grinberg, Victoria, Heger, Alexander, Homan, Jeroen, Iaria, Rosario, Jiang, Jia Chen, Jin, Chi Chuan, Koerding, Elmar, Linares, Manu, Liu, Zhu, Maccarone, Thomas J., Malzac, Julien, Manousakis, Antonios, Marin, Frédéric, Marinucci, Andrea, Mehdipour, Missagh, Méndez, Mariano, Migliari, Simone, Miller, Cole, Miniutti, Giovanni, Nardini, Emanuele, O’Brien, Paul T., Osborne, Julian P., Petrucci, Pierre Olivier, Possenti, Andrea, Riggio, Alessandro, Rodriguez, Jerome, Sanna, Andrea, Shao, Li Jing, Sobolewska, Malgosia, Sramkova, Eva, Stevens, Abigail L., Stiele, Holger, Stratta, Giulia, Stuchlik, Zdenek, Svoboda, Jiri, Tamburini, Fabrizio, Tauris, Thomas M., Tombesi, Francesco, Torok, Gabriel, Urbanec, Martin, Vincent, Frederic, Wu, Qing Wen, Yuan, Feng, in’ t Zand, Jean J.M., Zdziarski, Andrzej A., and Zhou, Xin Lin
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: In this paper we describe the potential of the enhanced X-ray Timing and Polarimetry (eXTP) mission for studies related to accretion flows in the strong field gravity regime around both stellar-mass and supermassive black-holes. eXTP has the unique capability of using advanced “spectral-timing-polarimetry” techniques to analyze the rapid variations with three orthogonal diagnostics of the flow and its geometry, yielding unprecedented insight into the inner accreting regions, the effects of strong field gravity on the material within them and the powerful outflows which are driven by the accretion process. X-spinmeasurements.
Published: 2019

10. Accreting pulsars: mixing-up accretion phases in transitional systems

Author: Campana, Sergio and Di Salvo, Tiziana
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: In the last 20 years our understanding of the millisecond pulsar (MSP) population changed dramatically. Thanks to RXTE, we discovered that neutron stars in LMXBs spins at 200-750 Hz frequencies, and indirectly confirmed the recycling scenario, according to which neutron stars are spun up to ms periods during the LMXB-phase. In the meantime, the continuous discovery of rotation-powered MSPs in binary systems in the radio and gamma-ray band (mainly with the Fermi LAT) allowed us to classify these sources into two "spiders" populations, depending on the mass of their companion stars: Black Widow, with very low-mass companion stars, and Redbacks, with larger companions possibly filling their Roche lobes but without accretion. It was soon regained that MSPs in short orbital period LMXBs are the progenitors of the spider populations of rotation-powered MSPs, although a direct link between accretion- and rotation-powered MSPs was still missing. In 2013 XMM-Newton spotted the X-ray outburst of a new accreting MSP (IGR J18245-2452) in a source that was previously classified as a radio MSP. Follow up observations of the source when it went back to X-ray quiescence showed that it was able to swing between accretion- to rotation-powered pulsations in a relatively short timescale (few days), promoting this source as the direct link between the LMXB and the radio MSP phases. Following discoveries showed that there exists a bunch of sources, which alternates X-ray activity phases, showing X-ray pulsations, to radio-loud phases, showing radio pulsations, establishing a new class of MSPs: the Transitional MSP. In this review we describe these exciting discoveries and the properties of accreting and transitional MSPs, highlighting what we know and what we have still to learn about in order to fully understand the (sometime puzzling) behavior of these systems and their evolutive connection (abridged)., 34 pages, 5 figures, invited review to the White Book of "NewCompStar" European COST Action MP1304
Published: 2018

11. The Hot and Energetic Universe: A White Paper presenting the science theme motivating the Athena+ mission

Author: Nandra, Kirpal, Barret, Didier, Barcons, Xavier, Fabian, Andy, Den Herder, Jan-Willem, Piro, Luigi, Watson, Mike, Adami, Christophe, Aird, James, Afonso, Jose Manuel, Alexander, Dave, Argiroffi, Costanza, Amati, Lorenzo, Arnaud, Monique, Atteia, Jean-Luc, Audard, Marc, Badenes, Carles, Ballet, Jean, Ballo, Lucia, Bamba, Aya, Bhardwaj, Anil, Stefano Battistelli, Elia, Becker, Werner, Becker, Michaël, Behar, Ehud, Bianchi, Stefano, Biffi, Veronica, Bîrzan, Laura, Bocchino, Fabrizio, Bogdanov, Slavko, Boirin, Laurence, Boller, Thomas, Borgani, Stefano, Borm, Katharina, Bouché, Nicolas, Bourdin, Hervé, Bower, Richard, Braito, Valentina, Branchini, Enzo, Branduardi-Raymont, Graziella, Bregman, Joel, Brenneman, Laura, Brightman, Murray, Brüggen, Marcus, Buchner, Johannes, Bulbul, Esra, Brusa, Marcella, Bursa, Michal, Caccianiga, Alessandro, Cackett, Ed, Campana, Sergio, Cappelluti, Nico, Cappi, Massimo, Carrera, Francisco, Ceballos, Maite, Christensen, Finn, Chu, You-Hua, Churazov, Eugene, Clerc, Nicolas, Corbel, Stephane, Corral, Amalia, Comastri, Andrea, Costantini, Elisa, Croston, Judith, Dadina, Mauro, D Ai, Antonino, Decourchelle, Anne, Della Ceca, Roberto, Dennerl, Konrad, Dolag, Klaus, Done, Chris, Dovciak, Michal, Drake, Jeremy, Eckert, Dominique, Edge, Alastair, Ettori, Stefano, Ezoe, Yuichiro, Feigelson, Eric, Fender, Rob, Feruglio, Chiara, Finoguenov, Alexis, Fiore, Fabrizio, Galeazzi, Massimiliano, Gallagher, Sarah, Gandhi, Poshak, Gaspari, Massimo, Gastaldello, Fabio, Georgakakis, Antonis, Georgantopoulos, Ioannis, Gilfanov, Marat, Gitti, Myriam, Gladstone, Randy, Goosmann, Rene, Gosset, Eric, Grosso, Nicolas, Guedel, Manuel, Guerrero, Martin, Haberl, Frank, Hardcastle, Martin, Heinz, Sebastian, Alonso Herrero, Almudena, Hervé, Anthony, Holmstrom, Mats, Iwasawa, Kazushi, Jonker, Peter, Kaastra, Jelle, Kara, Erin, Karas, Vladimir, Kastner, Joel, King, Andrew, Kosenko, Daria, Koutroumpa, Dimita, Kraft, Ralph, Kreykenbohm, Ingo, Lallement, Rosine, Lanzuisi, Giorgio, Lee, J., Lemoine-Goumard, Marianne, Lobban, Andrew, Lodato, Giuseppe, Lovisari, Lorenzo, Lotti, Simone, Mccharthy, Ian, Mcnamara, Brian, Maggio, Antonio, Maiolino, Roberto, Marco, Barbara, Martino, Domitilla, Mateos, Silvia, Matt, Giorgio, Maughan, Ben, Mazzotta, Pasquale, Mendez, Mariano, Merloni, Andrea, Micela, Giuseppina, Miceli, Marco, Mignani, Robert, Miller, Jon, Miniutti, Giovanni, Molendi, Silvano, Montez, Rodolfo, Moretti, Alberto, Motch, Christian, Nazé, Yaël, Nevalainen, Jukka, Nicastro, Fabrizio, Nulsen, Paul, Ohashi, Takaya, O Brien, Paul, Osborne, Julian, Oskinova, Lida, Pacaud, Florian, Paerels, Frederik, Page, Mat, Papadakis, Iossif, Pareschi, Giovanni, Petre, Robert, Petrucci, Pierre-Olivier, Piconcelli, Enrico, Pillitteri, Ignazio, Pinto, C., Plaa, Jelle, Pointecouteau, Etienne, Ponman, Trevor, Ponti, Gabriele, Porquet, Delphine, Pounds, Ken, Pratt, Gabriel, Predehl, Peter, Proga, Daniel, Psaltis, Dimitrios, Rafferty, David, Ramos-Ceja, Miriam, Ranalli, Piero, Rasia, Elena, Rau, Arne, Rauw, Gregor, Rea, Nanda, Read, Andy, Reeves, James, Reiprich, Thomas, Renaud, Matthieu, Reynolds, Chris, Risaliti, Guido, Rodriguez, Jerome, Rodriguez Hidalgo, Paola, Roncarelli, Mauro, Rosario, David, Rossetti, Mariachiara, Rozanska, Agata, Rovilos, Emmanouil, Salvaterra, Ruben, Salvato, Mara, Di Salvo, Tiziana, Jeremy Sanders, Sanz-Forcada, Jorge, Schawinski, Kevin, Schaye, Joop, Schwope, Axel, Sciortino, Salvatore, Severgnini, Paola, Shankar, Francesco, Sijacki, Debora, Sim, Stuart, Schmid, Christian, Smith, Randall, Steiner, Andrew, Stelzer, Beate, Stewart, Gordon, Strohmayer, Tod, Strüder, Lothar, Sun, Ming, Takei, Yoh, Tatischeff, V., Tiengo, Andreas, Tombesi, Francesco, Trinchieri, Ginevra, Tsuru, T. G., Ud-Doula, Asif, Ursino, Eugenio, Valencic, Lynne, Vanzella, Eros, Vaughan, Simon, Vignali, Cristian, Vink, Jacco, Vito, Fabio, Volonteri, Marta, Wang, Daniel, Webb, Natalie, Willingale, Richard, Wilms, Joern, Wise, Michael, Worrall, Diana, Young, Andrew, Zampieri, Luca, In T Zand, Jean, Zane, Silvia, Zezas, Andreas, Zhang, Yuying, Zhuravleva, Irina, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Dipartimento di Fisica e Chimica (DiFC), Università degli studi di Palermo - University of Palermo, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de recherche en astrophysique et planétologie (IRAP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Columbia Astrophysics Laboratory (CAL), Columbia University [New York], Department of Astrophysical Sciences [Princeton], Princeton University, Département d'Astrophysique (ex SAP) (DAP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institute for Computational Cosmology (ICC), Durham University, Dipartimento de Fisica Roma Tre (DF-Roma3), Università degli Studi Roma Tre, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Technische Universität München [München] (TUM), National Space Institute [Lyngby] (DTU Space), Technical University of Denmark [Lyngby] (DTU), 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), SRON Netherlands Institute for Space Research (SRON), Max-Planck-Institut für Extraterrestrische Physik (MPE), Department of Physics [Durham University], Ecole Polytechnique Fédérale de Lausanne (EPFL), Tokyo Metropolitan University [Tokyo], Department of Astronomy and Astrophysics [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Physics [Coral Gables], University of Miami [Coral Gables], Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Swedish Institute of Space Physics [Kiruna] (IRF), Astronomical Institute of the Czech Academy of Sciences, Czech Academy of Sciences [Prague] (ASCR), HEPPI - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Cavendish Laboratory, University of Cambridge [UK] (CAM), Università degli Studi di Roma Tor Vergata [Roma], Max-Planck-Institut für Astrophysik (MPA), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, PSL Research University (PSL), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], School of Physics and Astronomy [Southampton], University of Southampton, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Department of Computer Science, Penn State System, Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lawrence Livermore National Laboratory (LLNL), Max Plank Institute for Extraterrestial Life, 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), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fisica e Chimica [Palermo] (DiFC), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi Roma Tre = Roma Tre University (ROMA TRE), Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), 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), Tokyo Metropolitan University [Tokyo] (TMU), 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), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), HELIOS - LATMOS, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Harvard University-Smithsonian Institution, Université Paris sciences et lettres (PSL), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universiteit Leiden, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Astronomy, Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-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 Diderot - Paris 7 (UPD7), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Smithsonian Institution-Harvard University [Cambridge], Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Maiolino, Roberto [0000-0002-4985-3819], Reynolds, Christopher [0000-0002-1510-4860], Sijacki, Debora [0000-0002-3459-0438], Apollo - University of Cambridge Repository, 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Earth and Planetary Astrophysics (astro-ph.EP), astro-ph.SR, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics - Cosmology and Extragalactic Astrophysics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], astro-ph.EP, astro-ph.CO, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), astro-ph.IM, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: This White Paper, submitted to the recent ESA call for science themes to define its future large missions, advocates the need for a transformational leap in our understanding of two key questions in astrophysics: 1) How does ordinary matter assemble into the large scale structures that we see today? 2) How do black holes grow and shape the Universe? Hot gas in clusters, groups and the intergalactic medium dominates the baryonic content of the local Universe. To understand the astrophysical processes responsible for the formation and assembly of these large structures, it is necessary to measure their physical properties and evolution. This requires spatially resolved X-ray spectroscopy with a factor 10 increase in both telescope throughput and spatial resolving power compared to currently planned facilities. Feedback from supermassive black holes is an essential ingredient in this process and in most galaxy evolution models, but it is not well understood. X-ray observations can uniquely reveal the mechanisms launching winds close to black holes and determine the coupling of the energy and matter flows on larger scales. Due to the effects of feedback, a complete understanding of galaxy evolution requires knowledge of the obscured growth of supermassive black holes through cosmic time, out to the redshifts where the first galaxies form. X-ray emission is the most reliable way to reveal accreting black holes, but deep survey speed must improve by a factor ~100 over current facilities to perform a full census into the early Universe. The Advanced Telescope for High Energy Astrophysics (Athena+) mission provides the necessary performance (e.g. angular resolution, spectral resolution, survey grasp) to address these questions and revolutionize our understanding of the Hot and Energetic Universe. These capabilities will also provide a powerful observatory to be used in all areas of astrophysics., Submitted in response to the call for White Papers for the definition of the L2 and L3 missions in the ESA Science program. More information: http://www.the-athena-x-ray-observatory.eu/. 19 pages, 12 figures, 4 tables
Published: 2013

12. The Hot and Energetic Universe: The close environments of supermassive black holes

Author: Dovciak, Michal, Matt, Giorgio, Bianchi, Stefano, Boller, Thomas, Brenneman, Laura, Bursa, Michal, D Ai, Antonino, Di Salvo, Tiziana, Marco, Barbara, Goosmann, Rene, Karas, Vladimir, Iwasawa, Kazushi, Kara, Erin, Miller, Jon, Miniutti, Giovanni, Papadakis, Iossif, Petrucci, Pierre-Olivier, Ponti, Gabriele, Porquet, Delphine, Reynolds, Chris, Risaliti, Guido, Rozanska, Agata, Luca Zampieri, Zezas, Andreas, Young, Andrew, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Porquet, Delphine
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), [SDU.ASTR.CO] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.HE] Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: Most of the action in Active Galactic Nuclei (AGN) occurs within a few tens of gravitational radii from the supermassive black hole, where matter in the accretion disk may lose up to almost half of its energy with a copious production of X-rays, emitted via Comptonization of the disk photons by hot electrons in a corona and partly reflected by the accretion disk. Thanks to its large effective area and excellent energy resolution, Athena+ contributions in the understanding of the physics of accretion in AGN will be fundamental - and unique - in many respects. It will allow us to map the disk-corona system - which is crucial to understand the mechanism of energy extraction and the relation of the corona with winds and jets - by studying the time lags between reflected and primary photons. These lags have been recently discovered by XMM-Newton, but only Athena+ will have the sensitivity required to fully exploit this technique. Athena+ will also be able e.g. to determine robustly the spin of the black hole in nearby sources (and to extend these measurements beyond the local Universe), to establish the nature of the soft X-ray components, and to map the circumnuclear matter within the AGN inner parsec with unprecedented details., Supporting paper for the science theme "The Hot and Energetic Universe" to be implemented by the Athena+ X-ray observatory (http://www.the-athena-x-ray-observatory.eu). 9 pages, 8 figures
Published: 2013

13. On Low Mass X-ray Binaries and Millisecond Pulsar

Author: Burderi, L., DI SALVO, Tiziana, Burderi, L., and Di Salvo, T.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Settore FIS/05 - Astronomia E Astrofisica, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Stars: neutron, Stars: magnetic fields, Pulsars: general, X-rays: binaries, X-rays: pulsars, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The detection, in 1998, of the first Accreting Millisecond Pulsar, started an exciting season of continuing discoveries in the fashinating field of compact binary systems harbouring a neutron star. Indeed, in these last three lustres, thanks to the extraordinary performances of astronomical detectors, on ground as well as on board of satellites, mainly in the Radio, Optical, X-ray, and Gamma-ray bands, astrophysicists had the opportunity to thoroughly investigate the so-called Recycling Scenario: the evolutionary path leading to the formation of a Millisecond Radio Pulsar. The most intriguing phase is certainly the spin-up stage during which, because of the accretion of matter and angular momentum, the neutron star accumulates an extraordinary amount of mechanical rotational energy, up to one percent of its whole rest-mass energy. These millisecond spinning neutron stars are truly extreme physical objects: General and Special Relativity are fully in action, since their surfaces, attaining speeds close to one fifth of the speed of light, are located just beyond their Schwartzscild Radius, and electrodynamical forces, caused by the presence of huge surface magnetic fields of several hundred million Gauss, display their spectacular properties accelerating electrons up to such energies to promote pair creation in a cascade process responsible for the emission in Radio and Gamma-ray. The rotational energy is swiftly converted and released into electromagnetic power which, in some cases, causes the neutron star to outshine with a luminosity of one hundred Suns. In this paper I will review some of the most recent discoveries on (accreting) millisecond pulsars., Comment: 7 pages, 1 table, proceedings of the conference: "Reading the book of Globular Clusters with the lens of stellar evolution", Rome Astronomical Observatory, 26-28 November 2012
Published: 2013
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14. The pulse profile and spin evolution of the accreting pulsar in Terzan 5, IGR J17480-2446, during its 2010 outburst

Author: Papitto, A, Burderi, L, Belloni, TM, Stella, L, Bozzo, E, D'Aì, A, Ferrigno, C, Motta, S, Riggio, A, Tramacere, A., DI SALVO, Tiziana, IARIA, Rosario, Papitto, A, Di Salvo, T, Burderi, L, Belloni, TM, Stella, L, Bozzo, E, D'Aì, A, Ferrigno, C, Iaria, R, Motta, S, Riggio, A, and Tramacere, A
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Settore FIS/05 - Astronomia E Astrofisica, Astrophysics::High Energy Astrophysical Phenomena, neutron, pulsars: individual: IGR J17480-2446, X-rays: binaries [accretion, accretion discs, stars], FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, accretion, accretion discs, stars: neutron, pulsars: individual: IGR J17480-2446, X-rays: binaries, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: (abridged) We analyse the spectral and pulse properties of the 11 Hz transient accreting pulsar, IGR J17480-2446, in the globular cluster Terzan 5, considering all the available RXTE, Swift and INTEGRAL observations performed between October and November, 2010. By measuring the pulse phase evolution we conclude that the NS spun up at an average rate of =1.48(2)E-12 Hz/s, compatible with the accretion of the Keplerian angular momentum of matter at the inner disc boundary. Similar to other accreting pulsars, the stability of the pulse phases determined by using the second harmonic component is higher than that of the phases based on the fundamental frequency. Under the assumption that the second harmonic is a good tracer of the neutron star spin frequency, we successfully model its evolution in terms of a luminosity dependent accretion torque. If the NS accretes the specific Keplerian angular momentum of the in-flowing matter, we estimate the inner disc radius to lie between 47 and 93 km when the luminosity attains its peak value. Smaller values are obtained if the interaction between the magnetic field lines and the plasma in the disc is considered. The phase-averaged spectrum is described by thermal Comptonization of photons with energy of ~1 keV. A hard to soft state transition is observed during the outburst rise. The Comptonized spectrum evolves from a Comptonizing cloud at an electron temperature of ~20 keV towards an optically denser cloud at kT_e~3 keV. At the same time, the pulse amplitude decreases from 27% to few per cent and becomes strongly energy dependent. We discuss various possibilities to explain such a behaviour, proposing that at large accretion luminosities a significant fraction of the in-falling matter is not channelled towards the magnetic poles, but rather accretes more evenly onto the NS surface., Comment: To appear in MNRAS
Published: 2012

15. The X-ray spectrum of the newly discovered accreting millisecond pulsar IGR J17511-3057

Author: Papitto, A., Riggio, A., Burderi, L., D'Aì, A., Bozzo, E., Menna, M. T., DI SALVO, Tiziana, IARIA, Rosario, Papitto, A., Riggio, A., di Salvo, T., Burderi, L., D'Aì, A., Iaria, R., Bozzo, E., and Menna, M. T.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Settore FIS/05 - Astronomia E Astrofisica, stars neutron, X-rays binaries, X-rays individual IGR J17511-3057, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: We report on an XMM-Newton observation of the accreting millisecond pulsar, IGR J17511-3057. Pulsations at 244.8339512(1) Hz are observed with an RMS pulsed fraction of 14.4(3)%. A precise solution for the P_orb=12487.51(2)s binary system is derived. The measured mass function indicates a main sequence companion with a mass between 0.15 and 0.44 Msun. The XMM-Newton spectrum of the source can be modelled by at least three components, multicoloured disc emission, thermal emission from the NS surface and thermal Comptonization emission. Spectral fit of the XMM-Newton data and of the RXTE data, taken in a simultaneous temporal window, constrain the Comptonization parameters: the electron temperature, kT_e=51(+6,-4) keV, is rather high, while the optical depth (tau=1.34(+0.03,-0.06)) is moderate. The energy dependence of the pulsed fraction supports the interpretation of the cooler thermal component as coming from the accretion disc, and indicates that the Comptonizing plasma surrounds the hot spots on the NS surface, which provide the seed photons. Signatures of reflection, such as a broadened iron K-alpha emission line and a Compton hump at 30 keV ca., are also detected. We derive from the smearing of the reflection component an inner disc radius of ~> 40 km for a 1.4 Msun neutron star, and an inclination between 38{\deg} and 68{\deg}. XMM-Newton also observed two type-I X-ray bursts, probably ignited in a nearly pure helium environment. No photospheric radius expansion is observed, thus leading to an upper limit on the distance to the source of 10 kpc. A lower limit of 6.5 kpc can be also set if it is assumed that emission during the decaying part of the burst involves the whole neutron star surface. Pulsations observed during the burst decay are compatible with being phase locked, and have a similar amplitude, than pre-burst pulsations., Comment: 16 pages, 10 figures, 4 tables, accepted for publication in MNRAS
Published: 2010
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16. A Spectral Insight into the Physics of Accreting ms Pulsars

Author: Papitto, A, Riggio, A, Burderi, L, Menna, MT, Bozzo, E., DI SALVO, Tiziana, D'AI', Antonino, IARIA, Rosario, Papitto, A, Riggio, A, Burderi, L, Di Salvo, T, D'Ai, A, Iaria, R, Menna, MT, and Bozzo, E
Subjects: X-rays: binaries, Settore FIS/05 - Astronomia E Astrofisica, line: profile, profiles, X-rays: binaries [accretion, accretion disks, line], accretion, accretion disk
Abstract: The broadened iron lines observed from accreting compact objects are most easily interpreted in terms of reflection onto the accretion disc of the hard X-ray photons emitted by the central source. In this context, such a broadness is due to the relativistic motion of the reflecting plasma, in the deep gravitational well of the compact object, and can thus serve as a probe of the inner radius of the disc. Here we report about the discovery of such features from a couple of accreting millisecond pulsars, and discuss the constraints which can be derived on the magnetospheric radius.
Published: 2010

17. Linking Jet Emission, X-ray States and Hard X-ray Tails in the Neutron Star X-ray Binary GX 17+2

Author: MIGLIARI S, MILLER JONES J. C. A, FENDER R. P, HOMAN J, ROTHSCHILD R. E, RUPEN M. P, TOMSICK J. A, WIJNANDS R, VAN DER KLIS M., DI SALVO, Tiziana, High Energy Astrophys. & Astropart. Phys (API, FNWI), MIGLIARI S, MILLER-JONES J C A, FENDER R P, HOMAN J, DI SALVO T, ROTHSCHILD R E, RUPEN M P, TOMSICK J A, WIJNANDS R, and VAN DER KLIS M
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We present the results from simultaneous radio (Very Large Array) and X-ray (Rossi-X-ray Timing Explorer) observations of the Z-type neutron star X-ray binary GX~17+2. The aim is to assess the coupling between X-ray and radio properties throughout its three rapidly variable X-ray states and during the time-resolved transitions. These observations allow us, for the first time, to investigate quantitatively the possible relations between the radio emission and the presence of the hard X-ray tails and the X-ray state of the source. The observations show: 1) a coupling between the radio jet emission and the X-ray state of the source, i.e. the position in the X-ray hardness-intensity diagram (HID); 2) a coupling between the presence of a hard X-ray tail and the position in the HID, qualitatively similar to that found for the radio emission; 3) an indication for a quantitative positive correlation between the radio flux density and the X-ray flux in the hard-tail power law component; 4) evidence for the formation of a radio jet associated with the Flaring Branch-to-Normal Branch X-ray state transition; 5) that the radio flux density of the newly-formed jet stabilizes when also the normal-branch oscillation (NBO) in the X-ray power spectrum stabilizes its characteristic frequency, suggesting a possible relation between X-ray variability associated to the NBO and the jet formation. We discuss our results in the context of jet models., Accepted by ApJ
Published: 2007

18. Improved orbital parameters of accreting millisecond pulsar SAX J1808.4-3658

Author: MENNA M. T, PAPITTO A, BURDERI L, D, ANTONA F, DI SALVO, Tiziana, ROBBA, Natale, MENNA M T, PAPITTO A, BURDERI L, DI SALVO T, ANTONA F, and ROBBA N R
Published: 2006

19. Spectral evolution of Scorpius X-1 along its Color-Color Diagram

Author: D'AI', Antonino, DI SALVO, Tiziana, ROBBA, Natale, IARIA, Rosario, LAVAGETTO, Giuseppe, ZYCKI P., D'AI' A, DI SALVO T, ROBBA N R, IARIA R, LAVAGETTO G, and ZYCKI P
Published: 2006

20. Radio Ejection and Bump-related Orbital Period Gap of Millisecond Binary Pulsars

Author: D'ANTONA, Fabio, DI SALVO, Tiziana, LAVAGETTO, Giuseppe, VENTURA P, BURDERI L, POSSENTI A, TEODORESCU A., D'ANTONA F, VENTURA P, BURDERI L, DI SALVO T, LAVAGETTO G, POSSENTI A, and TEODORESCU A
Published: 2006

21. Improved orbital parameters of accreting millisecond pulsar SAX J1808.4-3658

Author: MENNA MT, PAPITTO A, BURDERI L, DI SALVO, Tiziana, D'ANTONA, Fabio, ROBBA, Natale, MENNA MT, PAPITTO A, BURDERI L, DI SALVO T, DANTONA F, and ROBBA NR
Published: 2006

22. Spectral changes during six years of Scorpius X-1 monitoring with BeppoSAX Wide Field Cameras

Author: Burderi, Luciano, Di Salvo, Tiziana, Santolamazza, Patrizia, Fiore, Fabrizio, P SANTOLAMAZZA, F FIORE, L BURDERI, and DI SALVO T
Subjects: Accretion (meteorology), Track (disk drive), Astrophysics (astro-ph), X-ray binary, FOS: Physical sciences, Astrophysics, X-ray, neutron stars, accreting millisecond, Wide field, Spectral line, Accretion rate, Neutron star, Spectral fitting, Geology
Abstract: We analyse a sample of fifty-five observations of Scorpius X-1 available in the BeppoSAX Wide Field Camera public archive and spanning over the six years of BeppoSAX mission life. Spectral changes are initially analysed by inspection of colour-colour and colour-intensity diagrams, we also discuss the shift of the Z tracks in these diagrams. Then we select two long observations for spectral fitting analysis, a secular shift is evident between the tracks in these observations. We finally extract spectra along the tracks and discuss the best fit model, the parameter variations along the track and between tracks, and their link to the accretion rate., 6 pages, 11 postscrpt figures.To appear in the conference proceedings of `Interacting Binaries: Accretion, Evolution & Outcomes' (Cefalu', July 4-10 2004)
Published: 2005

23. Constraints on the neutron star magnetic fields in Low Mass X-ray Binaries

Author: DI SALVO, Tiziana, L. BURDERI, AND N. R. ROBBA, DI SALVO T, L BURDERI, and AND N R ROBBA
Published: 2005

24. Accretion and Magneto-Dipole Emission in Fast-Rotating Neutron Stars: New Spin-Equilibrium Lines

Author: DI SALVO, Tiziana, D'ANTONA, Fabio, ROBBA, Natale, L. BURDERI, DI SALVO T, L BURDERI, F D'ANTONA, and N ROBBA
Published: 2005

25. Constraining the Equation of State of Neutron Stars with Genral Relativity

Author: LAVAGETTO, Giuseppe, D'ANTONA, Fabio, DI SALVO, Tiziana, IARIA, Rosario, ROBBA, Natale, BURDERI L, LAVAGETTO G, BURDERI L, D'ANTONA F, DI SALVO T, IARIA R, and ROBBA N R
Subjects: Neutron stars, Relativity and gravitation, Thermodynamic processes conduction convection equations of state
Abstract: When a radio pulsar breakes down by virtue of magnetodipole emission, its gravitational mass decreases accordingly. If the pulsar in hosted in a binary system, this mass loss will increase the orbital period of the system. We show that this relativistic effect can be indeed observable if the NS is fast and magnetized enough and that, if observed, it will help to put tight constraints on the equation of state of ultradense matter.
Published: 2005

26. BeppoSAX discovery of a new X-ray pulsar

Author: G. AUGELLO, L. BURDERI, L. STELLA, IARIA, Rosario, ROBBA, Natale, DI SALVO, Tiziana, LAVAGETTO, Giuseppe, G AUGELLO, R IARIA, ROBBA NR, T DI SALVO, L BURDERI, G LAVAGETTO, and L STELLA
Published: 2004

27. 'The discovery of serendipitous X-ray pulsar SAX J1802.7-2017 from a BeppoSAX observation of GX 9+1'

Author: G. AUGELLO, L. BURDERI, L. STELLA, IARIA, Rosario, ROBBA, Natale, DI SALVO, Tiziana, LAVAGETTO, Giuseppe, G AUGELLO, R IARIA, ROBBA NR, T DI SALVO, L BURDERI, G LAVAGETTO, and L STELLA
Published: 2004

28. To accrete or not to accrete: the dilemma of the recycling scenario

Author: BURDERI L, D'ANTONA, Fabio, DI SALVO, Tiziana, LAVAGETTO, Giuseppe, IARIA, Rosario, ROBBA, Natale, BURDERI L, D'ANTONA F, DI SALVO T, LAVAGETTO G, IARIA R, and ROBBA NR
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: We study the evolution of a low-mass X-ray binary by coupling a binary stellar evolution code with a general relativistic code that describes the behaviour of the neutron star. We find that non-conservative mass transfer scenarios are required to prevent the formation of submillisecond pulsars and/or the collapse to a black hole. We discuss the sweeping effects of an active magneto-dipole rotator on the transferred matter as a promising mechanism to obtain highly non-conservative evolutions., Comment: 7 pages, including 2 figures. To appear in proceedings of Aspen Center for Physics Conference on ``Binary Radio Pulsars'' Eds. F. Rasio and I. Stairs
Published: 2004
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29. Radio ejection in the evolution of X-ray binaries: the bridge between low mass X-ray binaries and millisecond pulsars

Author: Burderi, Luciano, D'Antona, Francesca, Di Salvo, Tiziana, and Burgay, Marta
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present a scenario for the spin-up and evolution of binary millisecond pulsars. This can explain the observational properties of the recently discovered binary millisecond pulsar PSR J1740-5340, with orbital period 32.5 hrs, in the Globular Cluster NGC 6397. The optical counterpart of this system is a star as luminous as the cluster turnoff stars, but with a lower Teff (a larger radius) which we model with a star of initial mass compatible with the masses evolving in the cluster (~0.85 Msun). This star has suffered Roche lobe overflow while evolving off the main sequence, spinning up the neutron star to the present period of 3.65 ms. There are evidences that at present, Roche lobe overflow is still going on. Indeed Roche lobe deformation of the mass losing component is necessary to be compatible with the optical light curve. The presence of matter around the system is also consistent with the long lasting irregular radio eclipses seen in the system. We propose that this system is presently in a phase of `radio-ejection' mass loss. The radio-ejection phase can be initiated only if the system is subject to intermittency in the mass transfer during the spin-up phase. In fact, when the system is detached the pulsar radio emission is not quenched, and may be able to prevent further mass accretion due to the action of the pulsar pressure at the inner Lagrangian point., 6 pages, including 3 figures. To appear in the proceedings of the XXII Moriond Astrophysics Meeting "The Gamma-Ray Universe" (Les Arcs, March 9-16, 2002), eds. A. Goldwurm, D. Neumann, and J. Tran Thanh Van, The Gioi Publishers (Vietnam)
Published: 2002

30. Broad iron lines from accreting millisecond pulsars

Author: Papitto, Alessandro, Di Salvo, Tiziana, Ai, Antonino D., Burderi, Luciano, Iaria, Rosario, Egron, Elise, and Alessandro Riggio

31. X-ray Spectroscopy of MXB 1728-34 with XMM-Newton

Author: Egron, Elise, Di Salvo, Tiziana, Burderi, Luciano, Papitto, Alessandro, Barragán, Laura, Dauser, Thomas, Joern Wilms, D Aí, Antonino, and Riggio, Alessandro

32. Interacting Binaries: Accretion, Evolution, Outcomes

Author: Burderi, Luciano, Lucio Angelo Antonelli, D Antona, Francesca, Di Salvo, Tiziana, Israel, Gian Luca, Piersanti, Luciano, Tornambè, Amedeo, and Straniero, Oscar

33. Quantum correlations beyond entanglement in a classical-channel model of gravity

Author: Federico Roccati, Benedetto Militello, Emilio Fiordilino, Rosario Iaria, Luciano Burderi, Tiziana Di Salvo, Francesco Ciccarello, Roccati, Federico, Militello, Benedetto, Fiordilino, Emilio, Iaria, Rosario, Burderi, Luciano, Di Salvo, Tiziana, and Ciccarello, Francesco
Subjects: Quantum Physics, Multidisciplinary, Quantum gravity, open quantum systems, quantum correlations, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Quantum Physics (quant-ph), Settore FIS/03 - Fisica Della Materia, General Relativity and Quantum Cosmology
Abstract: A direct quantization of the Newtonian interaction between two masses is known to establish entanglement, which if detected would witness the quantum nature of the gravitational field. Gravitational interaction is yet compatible also with gravitational decoherence models relying on classical channels, hence unable to create entanglement. Here, we show in paradigmatic cases that, despite the absence of entanglement, a classical-channel model of gravity can still establish quantum correlations in the form of quantum discord between two masses. This is demonstrated for the Kafri-Taylor-Milburn (KTM) model and a recently proposed dissipative extension of this. In both cases, starting from an uncorrelated state, a significant amount of discord is generally created. This eventually decays in the KTM model, while it converges to a small stationary value in its dissipative extension. We also find that initial local squeezing on the state of the masses can significanlty enhance the generated discord., 8 pages, 5 figures
Published: 2022

34. Imperfect accretion: ejecting matter in X-ray binaries

Author: MARINO, ALESSIO, DI SALVO, Tiziana, and PALMA, Gioacchino Massimo
Subjects: Settore FIS/05 - Astronomia E Astrofisica, accretion, X-ray binarie, black hole, neutron star, accretion disk
Abstract: X-ray binaries are binary stars composed of a compact object (a black hole, a neutron star) accreting matter from a companion star. These sources can be considered perfect astrophysical laboratories to test our knowledge of, e.g., General Relativity and Magneto-Hydrodynamics. Accretion is the key phenomenon characterizing these systems, but it is not always completely efficient. In many systems, ejections of matter are also observed, e.g. in the form of jets and winds, or also suggested, e.g. to explain the observed strong orbital expansion of a number of systems. Furthermore accretion and ejection seems to be somehow interconnected but the nature of this correlation is not completely clear. The purpose of this thesis is the study of a number of cases where the accretion is imperfect and mass losses have to be taken into account to correctly model the physical properties of the binaries. In the first of the featured projects, I focus on the spectral study of the accretion flow in the Neutron Star (NS) Low Mass X-ray Binary (LMXB) 1RXS J180408.9-342058, an intriguing system which in the past exhibited “very faint” phases of activity. I performed a spectral analysis of data collected by different X-ray telescopes, i.e. INTEGRAL, Swift and NuSTAR, The study led to several interesting results, in particular the observation of the intermediate spectral state, hard to catch in NS LMXBs because very short-lived, and new constraints on the nature of the companion star, which exclude the hypothesis of a helium dwarf companion as suggested in the past. The second project presents a systematic study of (almost) all known Accreting Millisecond X-ray Pulsars (AMXPs), i.e. LMXBs hosting an X-ray pulsar spinning at millisecond periods, with the aim of looking for indications of non-conservative mass-transfer in this class. Comparing this observed luminosity averaged over twenty years with the one expected from the theory in a conservative scenario, I found that over a sample of 19 sources, around one half of it shows indications for mass losses. The third project in this thesis is dedicated to jets, the most known form of mass ejection in X-ray binaries. Jets are characterized by flat radio-to-mid-IR spectra, which have been modelled in the last few decades using the Internal Shocks model ISHEM. The basic idea of this model consists in using the observed X-ray variability as a proxy for the fluctuations of the Lorentz factor in the ejected shells along the jet. I applied the model on the multi-wavelength data set of the NS LMXB 4U 0614+091. I found that ISHEM describes satisfactorily the data only in two cases: using the X-ray variability but in non-conical geometry or either in conical geometry but using flicker noise instead of the X-ray variability. The final project of my thesis aims at testing a unified accretion-ejection model to the Black Hole LMXB MAXI J1820+070. The model considers the accretion flow in X-ray binaries as two-fold, comprising a truncated geometrically thin disk far from the Black Hole and a so-called jet emitting disk serving as the base of the jet close to the Black Hole. Interestingly, the model allows not only to describe the X-rays data, but also to predict the radio power emitted by the jet. In order to test the model, I used X-rays data from Swift and NuSTAR. The preliminary results of the spectral fitting suggest that the model is indeed effective in describing the observed X-ray spectra. Furthermore, the analysis reveals the need for describing the reflection spectrum with two reflection components instead of one: the origin of such intriguing component, if confirmed, will be object of future investigations.
Published: 2021

35. Dense matter with eXTP

Author: Xiang-Dong Li, Jean in 't Zand, B. W. Stappers, Sudip Bhattacharyya, Slavko Bogdanov, Holger Stiele, Sharon M. Morsink, Tiziana Di Salvo, Zhaosheng Li, Robert D. Ferdman, Alessandro Riggio, Jin-Lu Qu, Wenfei Yu, Oleg Kargaltsev, R. Iaria, Xia Zhou, Joonas Nättilä, Gabriel Török, David Tsang, Aleksi Kurkela, Laura Tolos, Achim Schwenk, Ingo Tews, Ypeng Xu, Andrea Vacchi, Martin Urbanec, Andrea Santangelo, Xiao Yu Lai, Manuel Linares, Pavel Bakala, Altan Baykal, Anna L. Watts, Alexander Heger, Eva Šrámková, Andrea Sanna, Maurizio Falanga, Ang Li, M. Coleman Miller, Federico Bernardini, Edward F. Brown, Yuri Cavecchi, Jérôme Chenevez, Long Ji, Dieter H. Hartmann, Hendrik Schatz, Ignazio Bombaci, Shuang-Nan Zhang, Silvia Zane, Chanda Prescod-Weinstein, Victor Doroshenko, Kai Hebeler, Guobao Zhang, Tuomo Salmi, Fangjun Lu, Ming-Yu Ge, Melania Del Santo, Deepto Chakrabarty, Mariano Mendez, ShiJie Zheng, Wenda Zhang, S. K. Greif, Alessandro Patruno, Angelo Gambino, Nathalie Degenaar, Simin Mahmoodifar, Juri Poutanen, Marco Feroci, Thomas E. Riley, Shu Zhang, Andrea Possenti, Sebastien Guillot, Tod E. Strohmayer, Jeroen Homan, Can Güngör, Li-Ming Song, Renxin Xu, Universitat Politècnica de Catalunya. Departament de Física, Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica, High Energy Astrophys. & Astropart. Phys (API, FNWI), Astronomy, Watts, Anna L., Yu, WenFei, Poutanen, Juri, Zhang, Shu, Bhattacharyya, Sudip, Bogdanov, Slavko, Ji, Long, Patruno, Alessandro, Riley, Thomas E., Bakala, Pavel, Baykal, Altan, Bernardini, Federico, Bombaci, Ignazio, Brown, Edward, Cavecchi, Yuri, Chakrabarty, Deepto, Chenevez, Jérôme, Degenaar, Nathalie, Del Santo, Melania, Di Salvo, Tiziana, Doroshenko, Victor, Falanga, Maurizio, Ferdman, Robert D., Feroci, Marco, Gambino, Angelo F., Ge, MingYu, Greif, Svenja K., Guillot, Sebastien, Gungor, Can, Hartmann, Dieter H., Hebeler, Kai, Heger, Alexander, Homan, Jeroen, Iaria, Rosario, Zand, Jean in’t, Kargaltsev, Oleg, Kurkela, Aleksi, Lai, XiaoYu, Li, Ang, Li, XiangDong, Li, ZhaoSheng, Linares, Manuel, Lu, FangJun, Mahmoodifar, Simin, Méndez, Mariano, Coleman Miller, M., Morsink, Sharon, Nättilä, Joona, Possenti, Andrea, Prescod-Weinstein, Chanda, Qu, JinLu, Riggio, Alessandro, Salmi, Tuomo, Sanna, Andrea, Santangelo, Andrea, Schatz, Hendrik, Schwenk, Achim, Song, LiMing, Šrámková, Eva, Stappers, Benjamin, Stiele, Holger, Strohmayer, Tod, Tews, Ingo, Tolos, Laura, Török, Gabriel, Tsang, David, Urbanec, Martin, Vacchi, Andrea, Xu, RenXin, Xu, YuPeng, Zane, Silvia, Zhang, GuoBao, Zhang, ShuangNan, Zhang, WenDa, Zheng, ShiJie, and Zhou, Xia
Subjects: GAMMA-RAY PULSARS, dense matter, Astrophysics::High Energy Astrophysical Phenomena, Polarimetry, General Physics and Astronomy, FOS: Physical sciences, Astrophysics, Neutron, BRIGHTNESS OSCILLATIONS, 7. Clean energy, 01 natural sciences, INNER ACCRETION DISKS, Spectral line, X-ray, equation of state, neutron, X-rays, Physics and Astronomy (all), Equacions d'estat, Pulsar, 0103 physical sciences, MILLISECOND PULSARS, NEUTRON-STAR, RADIUS CONSTRAINTS, 010306 general physics, 010303 astronomy & astrophysics, RELATIVISTIC IRON LINE, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), LIGHT CURVES, Neutrons, Equation of state, QUASI-PERIODIC OSCILLATIONS, X-Rays, Starke Wechselwirkung und exotische Kerne – Abteilung Blaum, Astrophysics::Instrumentation and Methods for Astrophysics, EQUATION-OF-STATE, Accretion (astrophysics), Neutron star, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], Raigs X, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Dense matter
Abstract: In this White Paper we present the potential of the Enhanced X-ray Timing and Polarimetry (eXTP) mission for determining the nature of dense matter; neutron star cores host an extreme density regime which cannot be replicated in a terrestrial laboratory. The tightest statistical constraints on the dense matter equation of state will come from pulse profile modelling of accretion-powered pulsars, burst oscillation sources, and rotation-powered pulsars. Additional constraints will derive from spin measurements, burst spectra, and properties of the accretion flows in the vicinity of the neutron star. Under development by an international Consortium led by the Institute of High Energy Physics of the Chinese Academy of Science, the eXTP mission is expected to be launched in the mid 2020s., Comment: Accepted for publication on Sci. China Phys. Mech. Astron. (2019)
Published: 2019

36. Accreting Pulsars: Mixing-up Accretion Phases in Transitional Systems

Author: Tiziana Di Salvo, Sergio Campana, Rezzolla, Luciano, Pizzocchero, Pierre, Jones, David Ian, Rea, Nanda, Vidana, Isaac, Campana, Sergio, Di Salvo, Tiziana, and ITA
Subjects: Physics, education.field_of_study, Millisecond, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Population, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Orbital period, 01 natural sciences, Neutron star, Stars, Settore FIS/05 - Astronomia E Astrofisica, Pulsar, Millisecond pulsar, millisecond pulsars, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, education, neutron star, 010303 astronomy & astrophysics, Fermi Gamma-ray Space Telescope, pulsar
Abstract: In the last 20 years our understanding of the millisecond pulsar population changed dramatically. Thanks to the large effective area and good time resolution of the NASA X-ray observatory Rossi X-ray Timing Explorer, we discovered that neutron stars in Low Mass X-ray Binaries (LMXBs) spins at frequencies between 200 and 750 Hz, and indirectly confirmed the recycling scenario, according to which neutron stars are spun up to millisecond periods during the LMXB-phase. In the meantime, the continuous discovery of rotation-powered millisecond pulsars in binary systems in the radio and gamma-ray band (mainly with the Fermi Large Area Telescope) allowed us to classify these sources into two "spiders" populations, depending on the mass of their companion stars: Black Widow pulsars, with very low-mass companion stars, and Redbacks, with larger mass companion stars possibly filling their Roche lobes without accretion of matter onto the neutron star. It was soon regained that millisecond pulsars in short orbital period LMXBs are the progenitors of the spider populations of rotation-powered millisecond pulsars, although a direct link between accretion-powered and rotation-powered millisecond pulsars was still missing. In 2013 the ESA X-ray observatory XMM-Newton spotted the X-ray outburst of a new accreting millisecond pulsar (IGR J18245-2452) in a source that was previously classified as a radio millisecond pulsar, probably of the Redback type. Follow up observations of the source when it went back to X-ray quiescence showed that it was able to swing between accretion-powered to rotation-powered pulsations in a relatively short timescale (few days), promoting this source as the direct link between the LMXB and the radio millisecond pulsar phases. Following discoveries showed that there exists a bunch of sources which alternates X-ray activity phases, showing X-ray coherent pulsations, to radio-loud phases, showing radio pulsations, establishing a new class of millisecond pulsars, the so-called transitional millisecond pulsars. In this review we describe these exciting discoveries and the properties of accreting and transitional millisecond pulsars, highlighting what we know and what we have still to learn about in order to fully understand the (sometime puzzling) behaviour of these systems and their evolutive connection.
Published: 2018

37. Type I X-ray Bursts at Low Accretion Rates

Author: Peng, Fang, Brown, Edward F., Truran, James W., Antonelli, L. Angelo, Israel, Gian Luca, Piersanti, Luciano, Tornambe, Amedeo, Burderi, Luciano, Di Salvo, Tiziana, Fiore, Fabrizio, Matt, Giorgio, and Menna, Maria Teresa
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Caltech Library Services
Abstract: Neutron stars, with their strong surface gravity, have interestingly short timescales for the sedimentation of heavy elements. Recent observations of unstable thermonuclear burning (observed as X-ray bursts) on the surfaces of slowly accreting neutron stars (< 0.01 of the Eddington rate) motivate us to examine how sedimentation of CNO isotopes affects the ignition of these bursts. We further estimate the burst development using a simple one-zone model with a full reaction network. We report a region of mass accretion rates for weak H flashes. Such flashes can lead to a large reservoir of He, the unstable burning of which may explain some observed long bursts (duration ~ 1000 s).
Published: 2007

38. Type Ia Supernovae: Energetics, Neutronization and Nucleosynthesis

Author: Fang Peng, Ivo R. Seitenzahl, Natalia Vladimirova, D. Q. Lamb, Alan C. Calder, James W. Truran, Dean M. Townsley, Edward F. Brown, Antonelli, L. Angelo, Israel, Gian Luca, Piersanti, Luciano, Tornambe, Amedeo, Burderi, Luciano, Di Salvo, Tiziana, Fiore, Fabrizio, Matt, Giorgio, and Menna, Maria Teresa
Subjects: Physics, Thermonuclear fusion, Astrophysics::High Energy Astrophysical Phenomena, Energetics, Dark matter, Astronomy, White dwarf, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Supernova, Nucleosynthesis, Dark energy, Deflagration, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Caltech Library Services
Abstract: The utility of Type Ia supernovae, not simply as probes of the distance scale but also as a means of constraining the properties of dark energy, demands a significant improvement in theoretical predictions of their properties in outburst. To this end, we have given substantial effort to quantifying the energetics and nucleosynthesis properties of deflagration fronts in the interiors of the putative carbon-oxygen white dwarf progenitors of Type Ia thermonuclear supernovae. We briefly review some essential features of our flame model and its properties in this paper and discuss its implications both for our multidimensional numerical simulations of SNe Ia and for nucleosynthesis (specifically 56Ni production) in SNe Ia and Galactic chemical evolution.
Published: 2007

39. Radio Observations of Supernovae

Author: Kurt W. Weiler, Nino Panagia, Schuyler D. Van Dyk, Richard A. Sramek, Chris Stockdale, Antonelli, L. Angelo, Israel, Gian Luca, Piersanti, Luciano, Tornambe, Amedeo, Burderi, Luciano, Di Salvo, Tiziana, Fiore, Fabrizio, Matt, Giorgio, and Menna, Maria Teresa
Subjects: Physics, Supernova, Line-of-sight, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Binary number, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Caltech Library Services, Astrophysics::Galaxy Astrophysics
Abstract: Study of radio supernovae over the past 25 years includes two dozen detected objects and more than 100 upper limits. From this work it is possible to identify classes of radio properties, demonstrate conformance to and deviations from existing models, estimate the density and structure of the circumstellar material and, by inference, the evolution of the presupernova stellar wind. It is also possible to detect ionized hydrogen along the line of sight, to demonstrate binary properties of the stellar system, to detect clumpiness of the circumstellar material, and to put useful constraints on the progenitors of undetected Type Ia supernovae., Comment: 8 pages, 4 figures. Invited talk at `The Multicoloured Landscape of Compact Objects and their Explosive Origins', Cefalu', 2006 June 11-24 (AIP Conf. Proc.), eds. L. Burderi et al., in press
Published: 2007
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40. Which Stars Form Black Holes and Neutron Stars?

Author: Michael P. Muno, Antonelli, L. Angelo, Israel, Gian Luca, Piersanti, Luciano, Tornambe, Amedeo, Burderi, Luciano, Di Salvo, Tiziana, Fiore, Fabrizio, Matt, Giorgio, and Menna, Maria Teresa
Subjects: Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Binary number, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Neutron star, Stars, Supernova, Star cluster, High mass, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Caltech Library Services, Astrophysics::Galaxy Astrophysics
Abstract: I describe the current state of our knowledge of the mapping between the initial masses of stars and the compact objects -- particularly neutron stars and black holes -- that they produce. Most of that knowledge is theoretical in nature, and relies on uncertain assumptions about mass loss through winds, binary mass transfer, and the amount of mass ejected during a supernovae. Observational constraints on the initial masses of stars that produce neutron stars and black holes is scarce. They fall into three general categories: (1) models of the stars that produced the supernova remnants associated with known compact objects, (2) scenarios through with high mass X-ray binaries were produced, and (3) associations between compact objects and coeval clusters of stars for which the minimum masses of stars that have undergone supernovae are known. I focus on the last category as the most promising in the near term. I describe three highly-magnetized neutron stars that have been associated with progenitors that had initial masses of $>$30\msun, and evaluate the prospects of finding further associations between star clusters and compact objects., 8 pages, 3 figures. Uses aipproc.cls. To appear in the proceedings of the conference``The Multicoloured Landscape of Compact Objects and their Explosive Origins'', 2006 June 11--24, Cefalu, Sicily, to be published by AIP
Published: 2006

41. GrailQuest and HERMES: hunting for gravitational wave electromagnetic counterparts and probing space-time quantum foam

Author: F. Scala, Silvia Piranomonte, Yupeng Xu, Piero Malcovati, Samuel Pliego-Caballero, Angelo Francesco Gambino, Chiara Ferruglio, Fabrizio Fiore, M. Rapisarda, Giovanni Della Casa, G. Zanotti, Andrea Vacchi, Stefano Silvestrini, Lorenzo Amati, Simone Pirrotta, Giuseppe Bertuccio, Alessandro Maselli, András Pál, M. Fiorini, Salvatore Capozziello, D. Milankovich, Mile Karlica, Irina Rashevskaya, A. Anitra, Marco Grassi, Barbara Negri, Filippo Frontera, Margherita Piccinin, Alexander Rashevsky, Daniele Ottolina, Simonetta Puccetti, N. Zampa, Claudio Labanti, A. Guzmán, Borja Lopez Fernandez, Luciano Burderi, E. Demenev, Ugo Lo Cicero, G. Dilillo, C. Guidorzi, Andrea Santangelo, P. Nogara, Giovanni La Rosa, A. Pasquale, Masanori Ohno, Marco Barbera, Roberto Bertaccin, Alessandro Riggio, Norbert Werner, Melania Del Santo, Raffaele Piazzolla, Jakub Ripa, F. Mele, Filippo Ambrosino, Massimo Della Valle, Michele Bechini, Ivan Troisi, J. Prinetto, Tian-Xiang Chen, Marco Feroci, Jiewei Cao, C. Tenzer, Lingjun Wang, M. Citossi, Giancarlo Ghirlanda, Lara Nava, Pierluigi Bellutti, David Selcan, Francesco Russo, A. Monge, Pavel Efremov, Silvia Zane, F. Ceraudo, Uros Kostic, Giuseppe Sottile, Andrea Sanna, Fabrizio Ferrandi, M. Perri, A. Gomboc, R. Iaria, G. Sciarrone, Marco Cinelli, Y. Evangelista, Giuseppe Pucacco, Na Gao, Tiziana Di Salvo, M. Gandola, Tomaz Rotovnik, Enrico Costa, Dejan Gacnik, Gábor Galgóczi, Gianluigi Zampa, Mariafelicia De Laurentis, Paolo Lunghi, Michele Fiorito, Arianna Manca, Riccardo Campana, F. Fuschino, Andrea Colagrossi, Aurora Clerici, S. Curzel, Alessandro Papitto, Fabrizio Amarilli, E. Virgilli, Gianluca Morgante, Giovanni Amelino-Camelia, Burderi, Luciano, Di Salvo, Tiziana, Riggio, Alessandro, Gambino, Angelo Francesco, Sanna, Andrea, Fiore, Fabrizio, Amarilli, Fabrizio, Amati, Lorenzo, Ambrosino, Filippo, Amelino-Camelia, Giovanni, Anitra, Alessio, Barbera, Marco, Bechini, Michele, Bellutti, Paolo, Bertaccin, Roberto, Bertuccio, Giuseppe, Campana, Riccardo, Cao, Jiewei, Capozziello, Salvatore, Ceraudo, Francesco, Chen, Tianxiang, Cinelli, Marco, Citossi, Marco, Clerici, Aurora, Colagrossi, Andrea, Costa, Enrico, Curzel, Serena, De Laurentis, Mariafelicia, Della Casa, Giovanni, Della Valle, Massimo, Demenev, Evgeny, Del Santo, Melania, Dilillo, Giuseppe, Efremov, Pavel, Evangelista, Yuri, Feroci, Marco, Ferruglio, Chiara, Ferrandi, Fabrizio, Fiorini, Mauro, Fiorito, Michele, Frontera, Filippo, Fuschino, Fabio, Gacnik, Dejan, Galgoczi, Gabor, Gao, Na, Gandola, Massimo, Ghirlanda, Giancarlo, Gamboc, Andreja, Grassi, Marco, Guidorzi, Cristiano, Guzman, Alejandro, Iaria, Rosario, Karlica, Mile, Kostic, Uro, Labanti, Claudio, La Rosa, Giovanni, Lo Cicero, Ugo, Lopez Fernandez, Borja, Lunghi, Paolo, Malcovati, Piero, Maselli, Alessandro, Manca, Arianna, Mele, Filippo, Milankovich, Dorottya, Monge, Angel, Morgante, Gianluca, Nava, Lara, Negri, Barbara, Nogara, Paolo, Ohno, Masanori, Ottolina, Daniele, Pasquale, Andrea, Pal, Andra, Perri, Matteo, Piccinin, Margherita, Piazzolla, Raffaele, Pirrotta, Simone, Pliego-Caballero, Samuel, Prinetto, Jacopo, Pucacco, Giuseppe, Puccetti, Simonetta, Rapisarda, Massimo, Rashevskaya, Irina, Rashevsky, Alexander, Ripa, Jakub, Russo, Francesco, Papitto, Alessandro, Piranomonte, Silvia, Santangelo, Andrea, Scala, Francesca, Sciarrone, Giulia, Selcan, David, Silvestrini, Stefano, Sottile, Giuseppe, Rotovnik, Tomaz, Tenzer, Christoph, Troisi, Ivan, Vacchi, Andrea, Virgilli, Enrico, Werner, Norbert, Wang, Lingjun, Xu, Yupeng, Zampa, Gianluigi, Zampa, Nicola, Zane, Silvia, Zanotti, Giovanni, ITA, GBR, DEU, ESP, CZE, CHN, SVN, HUN, den Herder J-WA, Nikzad, S, Nakazawa, K, Burderi L., Di Salvo T., Sanna A., Fiore F., Riggio A., Gambino A.F., Amarilli F., Amati L., Ambrosino F., Amelino-Camelia G., Anitra A., Barbera M., Bechini M., Bellutti P., Bertacin R., Bertuccio G., Campana R., Cao J., Capozziello S., Ceraudo F., Chen T., Cinelli M., Citossi M., Clerici A., Colagrossi A., Costa E., Curzel S., De Laurentis M., Della Casa G., Demenev E., Del Santo M., Della Valle M., Dilillo G., Efremov P., Evangelista Y., Feroci M., Feruglio C., Ferrandi F., Fiorini M., Fiorito M., Frontera F., Fuschino F., Gacnik D., Galgoczi G., Gao N., Gandola M., Ghirlanda G., Gomboc A., Grassi M., Guidorzi C., Guzman A., Iaria R., Karlica M., Kostic U., Labanti C., La Rosa G., Lo Cicero U., Lopez Fernandez B., Lunghi P., Malcovati P., Maselli A., Manca A., Mele F., Milankovich D., Monge A., Morgante G., Nava L., Negri B., Nogara P., Ohno M., Ottolina D., Pasquale A., Pal A., Perri M., Piccinin M., Piazzolla R., Pirrotta S., Pliego-Caballero S., Prinetto J., Pucacco G., Puccetti S., Rapisarda M., Rashevskaya I., Rashevski A., Ripa J., Russo F., Papitto A., Piranomonte S., Santangelo A., Scala F., Sciarrone G., Selcan D., Silvestrini S., Sottile G., Rotovnik T., Tenzer C., Troisi I., Vacchi A., Virgilli E., Werner N., Wang L., Xu Y., Zampa G., Zampa N., Zane S., and Zanotti G.
Subjects: Physics, CubeSats, Gamma-Ray Bursts, Photon, Gravitational Wave counterparts, 010308 nuclear & particles physics, Gravitational wave, Space time, Quantum gravity, Astronomy, Triangulation (social science), 01 natural sciences, Settore FIS/05 - Astronomia E Astrofisica, All-sky monitor, Observatory, X-rays, 0103 physical sciences, Nano-satellites, Temporal triangulation, Gamma-ray burst, Quantum foam, 010303 astronomy & astrophysics
Abstract: GrailQuest (Gamma-ray Astronomy International Laboratory for Quantum Exploration of Space-Time) is an ambitious astrophysical mission concept that uses a fleet of small satellites whose main objective is to search for a dispersion law for light propagation in vacuo. Within Quantum Gravity theories, different models for space-time quantization predict relative discrepancies of the speed of photons w.r.t. the speed of light that depend on the ratio of the photon energy to the Planck energy. This ratio is as small as 10-23 for photons in the γ- ray band (100 keV). Therefore, to detect this effect, light must propagate over enormous distances and the experiment must have extraordinary sensitivity. Gamma-Ray Bursts, occurring at cosmological distances, could be used to detect this tiny signature of space-time granularity. This can be obtained by coherently combine a huge number of small instruments distributed in space to act as a single detector of unprecedented effective area. This is the first example of high-energy distributed astronomy: a new concept of modular observatory of huge overall collecting area consisting in a fleet of small satellites in low orbits, with sub-microsecond time resolution and wide energy band (keV-MeV). The enormous number of collected photons will allow to effectively search these energy dependent delays. Moreover, GrailQuest will allow to perform temporal triangulation of impulsive events with arc-second positional accuracies: an extraordinary sensitive X-ray/Gamma all-sky monitor crucial for hunting the elusive electromagnetic counterparts of Gravitational Waves, that will play a paramount role in the future of Multi-messenger Astronomy. A pathfinder of GrailQuest is already under development through the HERMES (High Energy Rapid Modular Ensemble of Satellites) project: a fleet of six 3U cube-sats to be launched by the end of 2022.
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42. Spectral analysis and orbital evolution of Low Mass X-ray Binaries at high inclination

Author: GALIANO, Carmela, Galiano, C., DI SALVO, Tiziana, and CUPANE, Antonio
Subjects: Low Mass X-Ray Binary, X1822-371, XB1916-053, spectral analysis, orbital evolution, Settore FIS/05 - Astronomia E Astrofisica
Abstract: X-Ray binaries are gravitationally bound systems consisting of a compact object that accretes matter from a companion star; they are the most interesting objects of the sky, infact they allow to study the physics of matter in very extreme conditions of density, temperature or magnetic eld. So the determination of spectral and temporal properties of X-ray binaries plays an important role in understanding the processes involved in these systems. This project aims to understand the properties of binary systems, at high inclination (dipping and eclips- ing sources), containing neutron stars weakly magnetized. In the light curves of these systems it is possible to identify a variety of modulations with orbital periodicity that are caused by the high inclination of the orbital plane with respect to the line of sight. Using data from several X-ray satellites such as Chandra, XMMNewton and Suzaku, we analized the spectral properties of the source X1822-371 and temporal evolution of the source XB1916-053. A short introduction about X-ray binary systems and basics about accretion is presented in chapter 1, while in chapter 2 I describe brie y the formation and evolution of binary systems. The results we obtained analizing the source X1822-371 are described in chapter 3. Our aim was to understand the nature of the residuals between 0.6 and 0.8 keV previously observed in the XMM/EPIC-pn data by Iaria et al. (2013). We interpreted the Gaussian feature in absorption as a cyclotron resonant scattering feature (CRSF) produced close to the neutron star surface and derive the magnetic eld strength at the surface of the neutron star. If our interpretation is correct this is the very rst detection of a CRSF below 1 keV in a LMXB. In the source XB 1916-053 the known orbital period derivative is extremely large and can be explained by invoking an extreme, non-conservative mass transfer rate that is not easily justiable. The results of our analysis of a large sample of data are presented in chapter 4. We had found that both in a conservative and non-conservative mass transfer scenario we have to invoke the presence of a third body to explain the observed sinusoidal modulation. We proposed that XB 1916-053 forms a hierarchical triple system.

43. BROAD BAND SPECTRAL ANALYSIS AND X-RAY SPECTROSCOPY OF NEUTRON STAR LOW MASS X-RAY BINARIES

Author: Matranga, Marco, Matranga, M., DI SALVO, Tiziana, and PALMA, Gioacchino Massimo
Subjects: X-ray Spectoscopy, X-ray Spectroscopy

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