STUDIES OF THE ORIGIN OF HIGH-FREQUENCY QUASI-PERIODIC OSCILLATIONS OF MASS-ACCRETING BLACK HOLES IN X-RAY BINARIES WITH NEXT-GENERATION X-RAY TELESCOPES-猫眼课题宝

用下一代X射线望远镜研究X射线双星中吸质黑洞高频准周期振荡的起源

DOI：

发表时间：

2016

期刊：

影响因子：

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作者：

B. Beheshtipour;J. Hoormann;H. Krawczynski

RXTE（罗西X射线计时探测器）的观测揭示了来自几个吸积恒星质量黑洞的X射线通量的高频准周期振荡（HFQPO）。 HFQPO（及其较低频率的对应物）可能使我们能够在强引力状态下研究广义相对论。然而，今天的观察证据尚不允许我们区分不同的 HFQPO 模型。在本文中，我们使用广义相对论射线追踪代码来研究轨道热点模型中 HFQPO 的 X 射线定时光谱和偏振特性。我们研究了银河双星 GRS 1915+105 中 166 Hz 准周期振荡 (QPO) 特殊情况的观测特征。最后，我们讨论了使用定时光谱实验（例如 LOFT（X 射线定时大型天文台））的光谱特征的可观测性，以及使用星载 X 射线偏振计（例如 IXPE（成像 X 射线偏振测量探测器）、PolSTAR（偏振光谱望远镜阵列）、PRAXyS（相对论 X 射线源的偏振测量）或 XIPE）的偏振特征的可观测性。（X 射线成像偏振测定探测器）。 LOFT 等高计数率任务将能够获得每个光子的 QPO 相位，从而能够研究 QPO 相位分辨光谱形状及其与通量水平之间的相关性。由于 HFQPO 的周期较短，第一代 X 射线偏振计无法为每个光子分配 QPO 相位。因此，QPO 相位分辨偏振能谱的研究需要使用第一代 X 射线偏振计和 LOFT 型任务同时进行观测。

Observations with RXTE (Rossi X-ray Timing Explorer) revealed the presence of high-frequency quasi-periodic oscillations (HFQPOs) of the X-ray flux from several accreting stellar-mass black holes. HFQPOs (and their counterparts at lower frequencies) may allow us to study general relativity in the regime of strong gravity. However, the observational evidence today does not yet allow us to distinguish between different HFQPO models. In this paper we use a general-relativistic ray-tracing code to investigate X-ray timing spectroscopy and polarization properties of HFQPOs in the orbiting Hotspot model. We study observational signatures for the particular case of the 166 Hz quasi-periodic oscillation (QPO) in the galactic binary GRS 1915+105. We conclude with a discussion of the observability of spectral signatures with a timing-spectroscopy experiment such as the LOFT (Large Observatory for X-ray Timing) and polarization signatures with space-borne X-ray polarimeters such as IXPE (Imaging X-ray Polarimetry Explorer), PolSTAR (Polarization Spectroscopic Telescope Array), PRAXyS(Polarimetry of Relativistic X-ray Sources), or XIPE (X-ray Imaging Polarimetry Explorer). A mission with high count rate such as LOFT would make it possible to get a QPO phase for each photon, enabling the study of the QPO-phase-resolved spectral shape and the correlation between this and the flux level. Owing to the short periods of the HFQPOs, first-generation X-ray polarimeters would not be able to assign a QPO phase to each photon. The study of QPO-phase-resolved polarization energy spectra would thus require simultaneous observations with a first-generation X-ray polarimeter and a LOFT-type mission.

The Large Observatory for X-ray Timing (LOFT)

DOI： 10.1117/12.925156

发表时间： 2011-07

期刊：

Experimental Astronomy

影响因子： 3

作者：

M. Feroci;L. Stella;M. Klis;T. Courvoisier;M. Hernanz;R. Hudec;A. Santangelo;D. Walton;A. Zdziarski;D. Barret;T. Belloni;J. Braga;S. Brandt;C. Budtz-Jørgensen;S. Campana;J. Herder;J. Huovelin;G. Israel;M. Pohl;P. Ray;A. Vacchi;S. Zane;A. Argan;P. Attinà;G. Bertuccio;E. Bozzo;R. Campana;D. Chakrabarty;E. Costa;A. De Rosa;E. Del Monte;S. Di Cosimo;I. Donnarumma;Y. Evangelista;D. Haas;P. Jonker;S. Korpela;C. Labanti;P. Malcovati;R. Mignani;F. Muleri;M. Rapisarda;A. Rashevsky;N. Rea;A. Rubini;C. Tenzer;C. Wilson-Hodge;B. Winter;K. Wood;G. Zampa;N. Zampa;M. Abramowicz;M. Alpar;D. Altamirano;J. Alvarez;L. Amati;C. Amoros;L. A. Antonelli;R. Artigue;P. Azzarello;M. Bachetti;G. Baldazzi;M. Barbera;C. Barbieri;S. Basa;A. Baykal;R. Belmont;L. Boirin;V. Bonvicini;L. Burderi;M. Bursa;C. Cabanac;E. Cackett;G. A. Caliandro;P. Casella;S. Chaty;J. Chenevez;M. Coe;A. Collura;A. Corongiu;S. Covino;G. Cusumano;F. D’Amico;S. Dall’Osso;D. de Martino;G. De Paris;G. Di Persio;T. di Salvo;C. Done;M. Dovc̆iak;A. Drago;U. Ertan;S. Fabiani;M. Falanga;R. Fender;P. Ferrando;D. Della Monica Ferreira;G. Fraser;F. Frontera;F. Fuschino;J. Galvez;P. Gandhi;P. Giommi;O. Godet;E. Göğüş;A. Goldwurm;D. Götz;M. Grassi;P. Guttridge;P. Hakala;G. Henri;W. Hermsen;J. Horák;A. Hornstrup;J. I. in’t Zand;J. Isern;E. Kalemci;G. Kanbach;V. Karas;D. Kataria;T. Kennedy;D. Klochkov;W. Kluźniak;K. Kokkotas;I. Kreykenbohm;J. Krolik;L. Kuiper;I. Kuvvetli;N. Kylafis;J. Lattimer;Francesco Lazzarotto;D. Leahy;F. Lebrun;D. Lin;N. Lund;T. Maccarone;J. Malzac;M. Marisaldi;A. Martindale;M. Mastropietro;J. McClintock;I. McHardy;M. Méndez;S. Mereghetti;M. Miller;T. Mineo;E. Morelli;S. Morsink;C. Motch;S. Motta;T. Muñoz-Darias;G. Naletto;V. Neustroev;J. Nevalainen;J. Olive;M. Orio;M. Orlandini;P. Orleanski;F. Ozel;L. Pacciani;S. Paltani;I. Papadakis;A. Papitto;A. Patruno;A. Pellizzoni;V. Petráček;J. Pétri;P. Petrucci;B. Phlips;L. Picolli;A. Possenti;D. Psaltis;D. Rambaud;P. Reig;R. Remillard;J. Rodriguez;P. Romano;M. Romanova;T. Schanz;C. Schmid;A. Segreto;A. Shearer;A. Smith;P. Smith;P. Soffitta;N. Stergioulas;M. Stolarski;Z. Stuchlík;A. Tiengo;D. Torres;G. Török;R. Turolla;P. Uttley;S. Vaughan;S. Vercellone;R. Waters;A. Watts;R. Wawrzaszek;N. Webb;J. Wilms;L. Zampieri;A. Zezas;J. Ziolkowski

通讯作者：

STUDIES OF THE ORIGIN OF HIGH-FREQUENCY QUASI-PERIODIC OSCILLATIONS OF MASS-ACCRETING BLACK HOLES IN X-RAY BINARIES WITH NEXT-GENERATION X-RAY TELESCOPES

用下一代X射线望远镜研究X射线双星中吸质黑洞高频准周期振荡的起源

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