The Disk-Wind-Jet Connection in the Black Hole H 1743-322. (arXiv:1208.4514v1 [astro-ph.HE])

The Disk-Wind-Jet Connection in the Black Hole H 1743-322. (arXiv:1208.4514v1 [astro-ph.HE]):
X-ray disk winds are detected in spectrally soft, disk-dominated phases of
stellar-mass black hole outbursts. In contrast, compact, steady, relativistic
jets are detected in spectrally hard states that are dominated by non-thermal
X-ray emission. Although these distinctive outflows appear to be almost
mutually exclusive, it is possible that a disk wind persists in hard states but
cannot be detected via X-ray absorption lines owing to very high ionization.
Here, we present an analysis of a deep, 60 ksec Chandra/HETGS observation of
the black hole candidate H 1743-322 in the low/hard state. The spectrum shows
no evidence of a disk wind, with tight limits, and within the range of ionizing
flux levels that were measured in prior Chandra observations wherein a wind was
clearly detected. In H 1743-322, at least, disk winds are actually diminished
in the low/hard state, and disk winds and jets are likely state-dependent and
anti-correlated. These results suggest that although the launching radii of
winds and jets may differ by orders of magnitude, they may both be tied to a
fundamental property of the inner accretion flow, such as the mass accretion
rate and/or the magnetic field topology of the disk. We discuss these results
in the context of disk winds and jets in other stellar-mass black holes, and
possible launching mechanisms for black hole outflows.