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Title: THE DISK-WIND-JET CONNECTION IN THE BLACK HOLE H 1743-322

Abstract

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 ks 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 inmore » the context of disk winds and jets in other stellar-mass black holes, and possible launching mechanisms for black hole outflows.« less

Authors:
;  [1];  [2];  [3];  [4];  [5];  [6];  [7];  [8]
  1. Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109-1042 (United States)
  2. Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138 (United States)
  3. Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 OHA (United Kingdom)
  4. Department of Astronomy, University of Maryland, College Park, MD 20742 (United States)
  5. Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center, Code 662, Greenbelt, MD 20771 (United States)
  6. Department of Physics and Astronomy, Wayne State University, 666 West Hancock Street, Detroit, MI 48201 (United States)
  7. Astronomical Institute 'Anton Pannekoek', University of Amsterdam, Science Park 904, 1098-XH, Amsterdam (Netherlands)
  8. Department of Physics, University of Warwick, Coventry CV4 7AL (United Kingdom)
Publication Date:
OSTI Identifier:
22078466
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal Letters
Additional Journal Information:
Journal Volume: 759; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 2041-8205
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ABSORPTION; ACCRETION DISKS; BLACK HOLES; EMISSION; IONIZATION; MAGNETIC FIELDS; RELATIVISTIC RANGE; SPECTRA; X RADIATION

Citation Formats

Miller, J. M., King, A. L., Raymond, J., Fabian, A. C., Reynolds, C. S., Kallman, T. R., Cackett, E. M., Van der Klis, M., and Steeghs, D. T. H., E-mail: jonmm@umich.edu. THE DISK-WIND-JET CONNECTION IN THE BLACK HOLE H 1743-322. United States: N. p., 2012. Web. doi:10.1088/2041-8205/759/1/L6.
Miller, J. M., King, A. L., Raymond, J., Fabian, A. C., Reynolds, C. S., Kallman, T. R., Cackett, E. M., Van der Klis, M., & Steeghs, D. T. H., E-mail: jonmm@umich.edu. THE DISK-WIND-JET CONNECTION IN THE BLACK HOLE H 1743-322. United States. doi:10.1088/2041-8205/759/1/L6.
Miller, J. M., King, A. L., Raymond, J., Fabian, A. C., Reynolds, C. S., Kallman, T. R., Cackett, E. M., Van der Klis, M., and Steeghs, D. T. H., E-mail: jonmm@umich.edu. Thu . "THE DISK-WIND-JET CONNECTION IN THE BLACK HOLE H 1743-322". United States. doi:10.1088/2041-8205/759/1/L6.
@article{osti_22078466,
title = {THE DISK-WIND-JET CONNECTION IN THE BLACK HOLE H 1743-322},
author = {Miller, J. M. and King, A. L. and Raymond, J. and Fabian, A. C. and Reynolds, C. S. and Kallman, T. R. and Cackett, E. M. and Van der Klis, M. and Steeghs, D. T. H., E-mail: jonmm@umich.edu},
abstractNote = {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 ks 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.},
doi = {10.1088/2041-8205/759/1/L6},
journal = {Astrophysical Journal Letters},
issn = {2041-8205},
number = 1,
volume = 759,
place = {United States},
year = {2012},
month = {11}
}