Volume 562, February 2014
|Number of page(s)||7|
|Section||Stellar structure and evolution|
|Published online||24 February 2014|
The relation between radio and X-ray luminosity of black hole binaries: affected by inner cool disks?
Max-Planck-Institut für Astrophysik,
Karl- Schwarzschildstr. 1,
Received: 1 August 2013
Accepted: 12 December 2013
Context. Observations of the black hole X-ray binaries GX 339-4 and V404 Cygni have brought evidence of a strong correlation between radio and X-ray emission during the hard spectral state; however, now more and more sources, the so-called “outliers”, are found with a radio emission noticeably below the established “standard” relation. Several explanations have already been considered, but the existence of dual tracks is not yet fully understood.
Aims. We suggest that in the hard spectral state re-condensation of gas from the corona into a cool, weak inner disk can provide additional soft photons for Comptonization, leading to a higher X-ray luminosity in combination with rather unchanged radio emission, which presumably traces the mass accretion rate.
Methods. As an example, we determined how much additional luminosity due to photons from an underlying disk would be needed to explain the data from the representative outlier source H1743-322.
Results. From the comparison with calculations of Compton spectra with and without the photons from an underlying disk, we find that the required additional X-ray luminosity lies well in the range obtained from theoretical models of the accretion flow.
Conclusions. The radio/X-ray luminosity relation resulting from Comptonization of additional photons from a weak, cool inner disk during the hard spectral state can explain the observations of the outlier sources, especially the data for H1743-322, the source with the most detailed observations. The existence or non-existence of weak inner disks on the two tracks might point to a difference in the magnetic fields of the companion stars. These could affect the effective viscosity and the thermal conductivity, hence also the re-condensation process.
Key words: accretion, accretion disks / black hole physics / X-rays: individuals: GX 339-4 / X-rays: individuals: V404 Cyg / X-rays: individuals: H1743-322 / X-rays: binaries
© ESO, 2014
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