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Ebisawa, Ken; Kubota, Aya; Mizuno, T.; Życki, P. T.

doi:10.1023/a:1011697718976

Cited by 8 publications

(10 citation statements)

References 10 publications

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“…• (see Ebisawa et al 2001;Gierliński et al 2001), and the Doppler-boosted disk emission fits well the observed high energy cutoff of the soft component. In the best fit for K-44-00 the inner disk radius R in = 3.80 +2.20 −2.56 R g , for i = 70…”

Section: State B Spectrasupporting

confidence: 67%

“…Our analysis of RXTE data of the micro-quasar GRS 1915+105 reveals all the spectral features typically found in high/soft states of accreting black holes (see Gierliński et al 1999;Życki et al 2001;Zdziarski et al 2001). The hard component is well fit by a non-thermal Comptonization, the soft component is usually complex, and the reprocessed component is present, highly ionized and further broadened and smeared.…”

Section: Discussionmentioning

confidence: 66%

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Spectral modeling of the three spectral states of the Galactic microquasar GRS 1915+105

Sobolewska¹,

Życki²

2003

A&A

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Abstract.We have analyzed Rossi X-ray Timing Explorer spectral data of the Galactic micro-quasar GRS 1915+105 in its various spectral states, as defined by Belloni et al. (2000). In states A and B the spectra are dominated by a strong soft thermal component, accompanied by a weak harder tail. The soft component is rather complex and cannot be described as a simple accretion disk emission. Relativistic effects in Kerr metric contribute to the complexity of the soft component but are not sufficient to fully account for it. As found previously, state C spectra are dominated by a Comptonized component, with small contribution from disk photons. The X-ray reprocessed component is highly significant in those spectra and, in contrast to the usual hard state spectra from accreting black holes, it is highly ionized.

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Section: State B Spectrasupporting

confidence: 67%

Section: Discussionmentioning

confidence: 66%

Spectral modeling of the three spectral states of the Galactic microquasar GRS 1915+105

Sobolewska¹,

Życki²

2003

A&A

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“…Gierliński et al 2001;Ebisawa et al 2001;Bhattacharyya et al 2001). There are three reasons why our results are different.…”

Section: Dependence Of the Luminosity On The Inclination Anglementioning

confidence: 99%

The structure and radiation spectra of illuminated accretion disks in AGN

Czerny

Różáńska

Dovčiak

et al. 2004

A&A

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Abstract. We discuss a model of the X-ray variability of active galactic nuclei (AGN). We consider multiple spots that originate on the surface of an accretion disk following intense irradiation by coronal flares. The spots move with the disk around the central black hole and eventually decay while new spots continuously emerge. We construct time sequences of the spectra of the spotted disk and compute the corresponding energy-dependent fractional variability amplitude. We explore the dependence on the disk inclination and other model parameters. AGN seen at higher inclination with respect to the observer, such as Seyfert 2 galaxies, are expected to have a fractional variability amplitude of the direct emission that is by a factor of a few higher than objects seen face on, such as Seyfert 1s.

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“…Okada et al 1998; Mizuno et al 1999). Contrary, stellar mass Kerr black holes accreting above their Eddington limit can account for these sources (Watarai, Mizuno & Mineshige 2001; Ebisawa et al 2003). Alternatively, mild beaming could be important (King et al 2001), although the shape of the surrounding nebula indicates that it is illuminated by a nearly isotropic emission source (Wang 2002).…”

Section: Introductionmentioning

confidence: 99%

Spectral energy distribution of super-Eddington flows

Heinzeller

Mineshige

Ohsuga

2006

Monthly Notices of the Royal Astronomical Society

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Spectral properties of super-Eddington accretion flows are investigated by means of a parallel line-of-sight calculation. The subjacent model, taken from two-dimensional radiation hydrodynamic simulations by Ohsuga et al. (2005), consists of a disc accretion region and an extended atmosphere with high velocity outflows. The non-gray radiative transfer equation is solved, including relativistic effects, by applying the FLD approximation. The calculated spectrum is composed of a thermal, blackbody-like emission from the disc which depends sensitively on the inclination angle, and of high energy X-ray and gamma-ray emission from the atmosphere. We find mild beaming effects in the thermal radiation for small inclination angles. If we compare the face-on case with the edge-on case, the average photon energy is larger by a factor of ~1.7 due mainly to Doppler boosting, while the photon number density is larger by a factor of ~3.7 due mainly to anisotropic matter distribution around the central black hole. This gives an explanation for the observed X-ray temperatures of ULXs which are too high to be explained in the framework of intermediate-mass black holes. While the main features of the thermal spectral component are consistent with more detailed calculations of slim accretion discs, the atmosphere induces major changes in the high-energy part, which cannot be reproduced by existing models. In order to interpret observational data properly, simple approaches like the Eddington-Barbier approximation cannot be applied.Comment: 10 pages, 8 figures, accepted for publication in MNRA

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Untitled

Cited by 8 publications

References 10 publications

Spectral modeling of the three spectral states of the Galactic microquasar GRS 1915+105

Spectral modeling of the three spectral states of the Galactic microquasar GRS 1915+105

The structure and radiation spectra of illuminated accretion disks in AGN

Spectral energy distribution of super-Eddington flows

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