Inclination and relativistic effects in the outburst evolution of black hole transients

Muñoz-Darias, T.; Coriat, M.; Plant, Daniel; Ponti, G.; Fender, R. P.; Dunn, Robert

doi:10.1093/mnras/stt546

Cited by 79 publications

(80 citation statements)

References 51 publications

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“…Other low inclination systems such as GX 339−4 and XTE J1817−330 show ultra soft disk dominated spectra in their lowest luminosity soft states, where the disk dominated spectra have the lowest temperature. In Cyg X-1 the ratio of unabsorbed 6-10 keV/2-6 keV flux in our softest spectrum is 0.05 not < 0.03 as observed in GX 339−4 (Muñoz-Darias et al 2013). Either Cyg X-1 does not quite reach the soft state proper, or the spin in Cyg X-1 is much higher than that of GX 339−4.…”

Section: Discussioncontrasting

confidence: 41%

Black hole spin of Cygnus X-1 determined from the softest state ever observed

Kawano

Done

Yamada

et al. 2017

Publications of the Astronomical Society of Japan

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We show the softest ever spectrum from Cyg X-1, detected in 2013 with Suzaku. This has the weakest high energy Compton tail ever seen from this object, so should give the cleanest view of the underlying disk spectrum, and hence the best determination of black hole spin from disk continuum fitting. Using the standard model of a disk with simple non-thermal Comptonisation to produce the weak high energy tail gives a high spin black hole. However, we get a significantly better fit by including an additional, low temperature thermal Comptonisation component, which allows a much lower black hole spin. Corroboration of the existence of an additional Compton component comes from the frequency dependent hard lags seen in the rapid variability in archival high/soft state data. These can not be explained if the continuum is a single non-thermal Comptonisation component, but are instead consistent with a radially stratified, multi zone Comptonisation spectrum, where the spectrum is softer further from the black hole. A complex multi-zone Comptonisation continuum is required to explain both spectra and timing together, and this has an impact on the derived black hole spin.

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Section: Discussioncontrasting

confidence: 41%

Black hole spin of Cygnus X-1 determined from the softest state ever observed

Kawano

Done

Yamada

et al. 2017

Publications of the Astronomical Society of Japan

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“…This is also confirmed by the detection of equatorial disk winds during the soft state of the source (Ponti et al 2012; as well as the shape of its hardness-intensity diagram (HID; Muñoz-Darias et al 2013). Currently, there are no dynamical constraints on the BH mass.…”

Section: Introductionmentioning

confidence: 68%

The Reverberation Lag in the Low-Mass X-Ray Binary H1743-322

Marco

Ponti

2016

ApJ

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The evolution of the inner accretion flow of a black hole X-ray binary (BHXRB) during the outburst is still a matter of active research. X-ray reverberation lags are powerful tools to constrain the disk-corona geometry. We present a study of X-ray lags in the black hole transient H1743-322. We compared results obtained from the analysis of all the publicly available XMM-Newton observations. These observations were carried out during two different outbursts, happened in 2008 and 2014. During all the observations the source is caught in the hard state and at similar luminosities (L 3−10 keV /L Edd ∼ 0.004). We detected a soft X-ray lag of ∼60 ms, most likely due to thermal reverberation. We did not detect any significant change of the lag amplitude among the different observations, indicating a similar disk-corona geometry at the same luminosity in the hard state. On the other hand, we observe significant differences between the reverberation lag detected in H1743-322 and in GX 339-4 (at similar luminosities in the hard state), which might indicate variations of the geometry from source to source.

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“…Based on the X-ray dipping behaviour observed in one observation it is believed that the inclination angle of its accretion disc is relatively high (>70 • ) to our line of sight . A systematic study of the effect of orbital inclination on the shape of the HID and the accretion disc temperature supports a high inclination angle for H 1743-322 (Muñoz-Darias et al 2013).…”

Section: Introductionmentioning

confidence: 75%

UsingXMM–Newtonto study the energy-dependent variability of H 1743-322 during its 2014 outburst

Stiele

2016

Mon. Not. R. Astron. Soc.

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Black hole transients during bright outbursts show distinct changes of their spectral and variability properties as they evolve during an outburst, that are interpreted as evidence for changes in the accretion flow and X-ray emitting regions. We obtained an anticipated XMMNewton ToO observation of H 1743-322 during its outburst in September 2014. Based on data of eight outbursts observed in the last 10 years we expected to catch the start of the hardto-soft state transition. The fact that neither the general shape of the observed power density spectrum nor the characteristic frequency show an energy dependence implies that the source still stays in the low-hard state at the time of our observation near outburst peak. The spectral properties agree with the source being in the low-hard state and a Swift/XRT monitoring of the outburst reveals that H 1743-322 stays in the low-hard state during the entire outburst (a. k. a. 'failed outburst'). We derive the averaged QPO waveform and obtain phase-resolved spectra. Comparing the phase-resolved spectra to the phase averaged energy spectrum reveals spectral pivoting. We compare variability on long and short time scales using covariance spectra and find that the covariance ratio does not show an increase towards lower energies as has been found in other black hole X-ray binaries. There are two possible explanations: either the absence of additional disc variability on longer time scales is related to the rather high inclination of H 1743-322 compared to other black hole X-ray binaries or it is the reason why we observe H 1743-322 during a failed outburst. More data on failed outbursts and on high-inclination sources will be needed to investigate these two possibilities further.

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Inclination and relativistic effects in the outburst evolution of black hole transients

Cited by 79 publications

References 51 publications

Black hole spin of Cygnus X-1 determined from the softest state ever observed

Black hole spin of Cygnus X-1 determined from the softest state ever observed

The Reverberation Lag in the Low-Mass X-Ray Binary H1743-322

UsingXMM–Newtonto study the energy-dependent variability of H 1743-322 during its 2014 outburst

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