Relativistic X-Ray Lines from the Inner Accretion Disks Around Black Holes

By J. Miller. 2007

353 citations recorded by the source corpus.

AbstractRelativistic X-ray emission lines from the inner accretion disks around black holes are reviewed. Recent observations with the Chandra X-ray Observatory, X-ray Multi-Mirror Mission-Newton, ...

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1d2f8e12ccd6d7ee4c9825548577c5570437fcc2

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Citations in the corpus

Measuring the spins of accreting black holes (2011, methodology): “For a review, see Miller (2007).”
STELLAR-MASS BLACK HOLE SPIN CONSTRAINTS FROM DISK REFLECTION AND CONTINUUM MODELING (2009, background): “Iron emission lines formed in the inner accretion disk will bear the imprints of the strong Doppler shifts and gravitational red-shifts endemic to that region, and so can serve as incisive probes of the innermost relativistic regime (for a review, see Miller 2007).”
The Accretion Disk Wind in the Black Hole GRO J1655–40 (2008, background): “Fortunately, we can improve our understanding of black holes and their accretion disks by focusing on timing studies, emission lines broadened by orbital motions, ad disk winds (e.g. Strohmayer 2000, Miller 2007, Proga 2003, Miller et al. 2006) .”
The Masses and Spins of Neutron Stars and Stellar-Mass Black Holes (2014, background): “Parameters central to the blurring include the emissivity of the disk reflection spectrum (typically a power-law in radius, with zero–two breaks; see [253, 254, 255] ), and the inclination of the inner disk.”
Irradiation of an accretion disc by a jet: general properties and implications for spin measurements of black holes (2013, background): “These relativistic lines are presentin a significant fraction of AGN spectra (Guainazzi, Bianchi & Dovčiak2006; Nandra et al. 2007; Longinotti et al. 2008; Patrick et al. 2011) and Galactic black hole binaries (Miller 2007; Duro et al. 2011; Fabian et al. 2012a).”
Observational evidence for a correlation between jet power and black hole spin (2011, methodology): “In addition to the CF method, a second method based on fitting the profile of the relativistically broadened Fe Kα line has been used to estimate BH spins (Reynolds & Nowak 2003; Miller 2007).”
Cosmological Black Hole Spin Evolution by Mergers and Accretion (2008, methodology): “…relation between the BH mass and the mass of the galactic bulge hosting the BH. Spin measurements are generally more uncertain (Narayan 2005; Miller 2007), and the cosmological coevolution of BH masses and spins is a significant open problem in our understanding of quasars and AGNs (Gammie…”
Black hole accretion discs in the canonical low‐hard state (2009, background): “As mentioned above, a further feature in the X-ray spectra of BHBs are the various reflection signatures associated with the reprocessing of hard radiation by the cool accretion disc.”
Relativistic iron K X-ray reverberation in NGC 4151 (2011, methodology): “Broadening of Xray spectral features caused by relativistic effects has been the main tool in studying these systems (Miller 2007 for a review).”
THE SPIN OF THE SUPERMASSIVE BLACK HOLE IN NGC 3783 (2011, background): “…physics around SMBHs, including the effects of black hole spin, comes from examining relativistically broadened spectral features that are emitted from the surface layers of the inner accretion disk in response to irradiation by the hard X-ray source (Reynolds & Nowak 2003; Miller 2007).”
TESTING THE NO-HAIR THEOREM WITH OBSERVATIONS IN THE ELECTROMAGNETIC SPECTRUM. IV. RELATIVISTICALLY BROADENED IRON LINES (2012, background): “Such iron lines have been observed in both galactic black holes and AGN (see Reynolds & Nowak 2003; Miller 2007 for reviews).”
The role of the reflection fraction in constraining black hole spin (2014, background): “Reflection of X-rays off the innermost parts of the accretiondisc is highly affected by general relativistic effects, leading to strong broadening of the reflection features (see, e.g., Fabian et al. 1989; Laor 1991; Reynolds & Nowak 2003; Miller 2007; Dauser et al. 2010).”
Precise mass and spin measurements for a stellar-mass black hole through X-ray timing: the case of GRO J1655-40 (2013, methodology): “The Fe Kα line method is based on the modelling of the relativistically broadened profile of the iron line (see Miller 2007 and Reynolds 2013 for recent reviews and e.g. Miniutti, Fabian & Miller 2004; Brenneman & Reynolds 2006; Yamada et al. 2009; Reis et al. 2011; Steiner et al. 2012; Miller et…”
Broad iron L line and X-ray reverberation in 1H0707-495 (2009, background): “…broad iron K line seen in many AGN, is a further confirmation that the observed X-ray spectra from suppermassive black holes in radiatively efficient AGN are emitted from within few gravitational radii of the black hole (Tanaka et al. 1995; Nandra et al. 2007, see Miller 2007 for a review).”
THE CORES OF THE Fe Kα LINES IN ACTIVE GALACTIC NUCLEI: AN EXTENDED CHANDRA HIGH ENERGY GRATING SAMPLE (2010, background): “…Kα emission may be comparable to any additional, relativistically broadened Fe Kα line emission that may be present, and indeed, in many cases may be the only component of the Fe Kα line (e.g., see Guainazzi et al. 2006; Nandra et al. 2007; Miller 2007; Turner & Miller 2009; Bianchi et al. 2009).”