Recent Hubble Space Telescope Results on X-Ray Novae

Hynes, R. I.; Haswell, C. A.; Chaty, S.; Shrader, C. R.; Cui, Wei; Mauche, Christopher W.

doi:10.1007/978-94-010-0700-9_15

Cited by 3 publications

(3 citation statements)

References 2 publications

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“…Follow up observations were carried out by Uemura et al 2000;Chaty et al 2000;Wren & McKay 2000;Mauche et al 2000;Pooley & Waldram 2000. Because of its unique position in the Galactic halo, this black hole (BH) binary suffered much less absorption and is widely studied in multi-wavelengths during both its active outbursting periods and in its quiescent state (Revnivtsev et al 2000;Cook et al 2000;Garcia et al 2000;Haswell et al 2000;Hynes et al 2000;McClintock et al 2000;Wagner et al 2000;Taranova & Shenavrin 2000;Esin et al 2001;Markoff et al 2001;Hynes et al 2003;Chaty et al 2003;Shahbaz et al 2005). The distance of this system is estimated to be around 1.8 kpc (McClintock et al 2001a).…”

Section: Introductionmentioning

confidence: 99%

Accretion flow properties of XTE J1118+480 during its 2005 outburst

Debnath

Chatterjee

Jana

et al. 2020

Res. Astron. Astrophys.

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We study spectral and temporal properties of Galactic short orbital period transient black hole XTE J1118+480 during its 2005 outburst using archival data of RXTE PCA and HEXTE instruments in the combined energy range of 3 – 100 keV. Spectral analysis with the physical two component advective flow (TCAF) model allows us to understand the accretion flow properties of the source. We found that this outburst of XTE J1118+480 is an unconventional outburst as the source was only in the hard state (HS). Our spectral analysis suggests that during the entire outburst, the source was highly dominated by the low angular momentum sub-Keplerian halo rate. Since the source was active in radio throughout the outburst, we make an effort to estimate X-ray contribution of jets to total observed X-ray emissions from the spectral analysis with the TCAF model. The total X-ray intensity shows a similar nature of evolution as that of radio and jet X-ray fluxes. This allowed us to define this ‘outburst’ also as a jet dominated ‘outburst’. Total X-ray flux is also found to subside when jet activity disappears. Our detailed spectral analysis also indicated that although the source was only in the HS during the outburst, in the late declining phase the spectrum became slightly softer due to the slow rise in the Keplerian disk rate.

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Section: Introductionmentioning

confidence: 99%

Accretion flow properties of XTE J1118+480 during its 2005 outburst

Debnath

Chatterjee

Jana

et al. 2020

Res. Astron. Astrophys.

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“…The black hole transient XTE J1859+226 in our sample is a typical black hole transient as well (Hynes et al 2002).…”

Section: Observationsmentioning

confidence: 74%

Power spectral properties of the soft spectral states in four black hole transients

Mao

2021

Res. Astron. Astrophys.

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The X-ray variability in the soft X-ray spectral state of black hole binaries is primarily characterized by a power-law noise (PLN), which is thought to originate from the propagation of the modulation in the mass accretion rate of a standard accretion disk flow. Such a PLN has also been revealed in the disk spectral component in the hard and the intermediate states in several black hole binaries. Here we present an investigation of the Rossi X-ray Timing Explorer (RXTE) observations of four black hole transients in which soft spectral states were observed twenty times or more. We show that in the soft spectral state, the PLN index varied in a large range between –1.64 and –0.62, and the fractional rms variability calculated in the 0.01 – 20 Hz frequency range reached as large as 7.67% and as low as 0.83%. Remarkably, we have found evidence of an inclination dependence of the maximal fractional rms variability, the averaged fractional rms variability and the fractional rms variability of the median in the sample based on current knowledge of inclination of black hole binaries. An inclination dependence has only been predicted in early magnetohydrodynamic simulations of isothermal disks limited to a high-frequency regime. In theory, the noise index is related to the physics of inward propagation of disk fluctuations, while the fractional rms amplitude reflects the intrinsic properties of the magnetohydrodynamic nature of the accretion flow. Our results therefore suggest that X-ray variability in the soft state can be used to put constraints on the properties of the accretion flow as well as the inclination of the accretion disk.

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“…Indeed, it was found that the whole broadband spectrum could, in some BHXBs; and a few neutron star XRBs (see Baglio et al 2022; Lewis et al 2010), at some stages in the hard state, potentially be jet dominated (e.g., Fender et al 2003; Markoff et al 2001; Russell et al 2010). Hynes et al (2003) found that the rapid variability of XTE J1118+480 has a power law spectrum with

\alpha =-0.6

from IR to X‐ray frequencies, also suggesting a common origin. Nowak et al (2005) asked the question “Is the IR coincidence just that?,” referring to the apparent agreement in GX 339–4 between the extrapolated radio and X‐ray power laws, and the IR spectral break.…”

Section: Introductionmentioning

confidence: 99%

On the infrared coincidence: What is the jet contribution to the X‐ray power law in GX 339–4?

Russell

2023

Astron Nachr

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The hard X-ray power law, prominent in the hard state in black hole X-ray binaries, is generally due to thermal Comptonization in the corona. Optically thin synchrotron emission from compact jets is commonly seen at infrared wavelengths in the hard state. The extent of this spectrum to higher energies remains uncertain. Here, a multi-wavelength study of GX 339-4 is presented.The infrared (IR) to X-ray spectral index is measured and compared to the X-ray spectral index fitted separately. On some dates in which the jet dominates the IR emission, the X-ray power law and the IR to X-ray power-law spectral indices are both in the range 𝛼 = −0.7 ± 0.2 (where F 𝜈 ∼ 𝜈 𝛼 ), that is, photon index, Γ = 1.7 ± 0.2. This suggests they could be the same power law with the same origin, or that this is a coincidence. On other dates in the hard state, 𝛼 IR−X < 𝛼 X , ruling out a common origin. It is likely that Comptonization dominates on most dates, as expected. However, the X-ray power law never appears to be fainter than the jet power law extrapolated from IR to X-ray, implying that the jet contribution imposes a lower limit to the X-ray flux. If confirmed, this would imply the cooling break in the synchrotron spectrum probably resides at X-ray or higher energies. It is suggested that X-ray spectral fitting should include an extra power law with a break (ideally fit to IR too).

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Recent Hubble Space Telescope Results on X-Ray Novae

Cited by 3 publications

References 2 publications

Accretion flow properties of XTE J1118+480 during its 2005 outburst

Accretion flow properties of XTE J1118+480 during its 2005 outburst

Power spectral properties of the soft spectral states in four black hole transients

On the infrared coincidence: What is the jet contribution to the X‐ray power law in GX 339–4?

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