Multi-wavelength coverage of state transitions in the new black hole X-ray binary swift J1910.2-0546

Degenaar, N.; Maitra, D.; Reynolds, M. T.; Miller, J. M.; Reis, R. C.; King, A. L.; Gültekin, K.; Cackett, E. M.; Bailyn, C. D.; Buxton, M. M.; MacDonald, R. K. D.; Fabian, A. C.; Fox, D. B.

doi:10.1088/0004-637X/784/2/122

Title: Multi-wavelength coverage of state transitions in the new black hole X-ray binary swift J1910.2-0546

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Abstract

Understanding how black holes accrete and supply feedback to their environment is one of the outstanding challenges of modern astrophysics. Swift J1910.2-0546 is a candidate black hole low-mass X-ray binary that was discovered in 2012 when it entered an accretion outburst. To investigate the binary configuration and the accretion morphology, we monitored the evolution of the outburst for ≅3 months at X-ray, UV, optical (B, V, R, I), and near-infrared (J, H, K) wavelengths using Swift and SMARTS. The source evolved from a hard to a soft X-ray spectral state with a relatively cold accretion disk that peaked at ≅0.5 keV. A Chandra/HETG spectrum obtained during this soft state did not reveal signatures of an ionized disk wind. Both the low disk temperature and the absence of a detectable wind could indicate that the system is viewed at relatively low inclination. The multi-wavelength light curves revealed two notable features that appear to be related to X-ray state changes. First, a prominent flux decrease was observed in all wavebands ≅ 1-2 weeks before the source entered the soft state. This dip occurred in (0.6-10 keV) X-rays ≅ 6 days later than at longer wavelengths, which could possibly reflect the viscous timescalemore »« less

Authors:

Degenaar, N.; Maitra, D.; Reynolds, M. T.; Miller, J. M.; Reis, R. C.; King, A. L.; Gültekin, K. ^[1]; Cackett, E. M. ^[2]; Bailyn, C. D.; Buxton, M. M.; MacDonald, R. K. D. ^[3]; Fabian, A. C. ^[4]; Fox, D. B. ^[5]

Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109 (United States)
Department of Physics and Astronomy, Wayne State University, 666 West Hancock Street, Detroit, MI 48201 (United States)
Astronomy Department, Yale University, P.O. Box 208101, New Haven, CT 06520-8101 (United States)
Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 OHA (United Kingdom)
Department of Astronomy and Astrophysics, Pennsylvania State University, 525 Davey Laboratory, University Park, PA 16802 (United States)

Publication Date:: Tue Apr 01 00:00:00 EDT 2014

OSTI Identifier:: 22357243

Resource Type:: Journal Article

Journal Name:: Astrophysical Journal

Additional Journal Information:: Journal Volume: 784; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X

Country of Publication:: United States

Language:: English

Subject:: 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCRETION DISKS; ASTROPHYSICS; BINARY STARS; BLACK HOLES; CONFIGURATION; DECAY; EMISSION; EVOLUTION; INCLINATION; MASS; QUENCHING; SOFT X RADIATION; SPECTRA; STARS; VISIBLE RADIATION; WAVELENGTHS

Citation Formats


                    Degenaar, N., Maitra, D., Reynolds, M. T., Miller, J. M., Reis, R. C., King, A. L., Gültekin, K., Cackett, E. M., Bailyn, C. D., Buxton, M. M., MacDonald, R. K. D., Fabian, A. C., Fox, D. B., and Rykoff, E. S., E-mail: degenaar@umich.edu. Multi-wavelength coverage of state transitions in the new black hole X-ray binary swift J1910.2-0546.  United States: N. p., 2014. 
        Web.  doi:10.1088/0004-637X/784/2/122.

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                    Degenaar, N., Maitra, D., Reynolds, M. T., Miller, J. M., Reis, R. C., King, A. L., Gültekin, K., Cackett, E. M., Bailyn, C. D., Buxton, M. M., MacDonald, R. K. D., Fabian, A. C., Fox, D. B., & Rykoff, E. S., E-mail: degenaar@umich.edu. Multi-wavelength coverage of state transitions in the new black hole X-ray binary swift J1910.2-0546.  United States.  https://doi.org/10.1088/0004-637X/784/2/122

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                    Degenaar, N., Maitra, D., Reynolds, M. T., Miller, J. M., Reis, R. C., King, A. L., Gültekin, K., Cackett, E. M., Bailyn, C. D., Buxton, M. M., MacDonald, R. K. D., Fabian, A. C., Fox, D. B., and Rykoff, E. S., E-mail: degenaar@umich.edu. 2014.  
        "Multi-wavelength coverage of state transitions in the new black hole X-ray binary swift J1910.2-0546".  United States.  https://doi.org/10.1088/0004-637X/784/2/122.

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@article{osti_22357243,

  title        = {Multi-wavelength coverage of state transitions in the new black hole X-ray binary swift J1910.2-0546},

  author       = {Degenaar, N. and Maitra, D. and Reynolds, M. T. and Miller, J. M. and Reis, R. C. and King, A. L. and Gültekin, K. and Cackett, E. M. and Bailyn, C. D. and Buxton, M. M. and MacDonald, R. K. D. and Fabian, A. C. and Fox, D. B. and Rykoff, E. S., E-mail: degenaar@umich.edu},

  abstractNote = {Understanding how black holes accrete and supply feedback to their environment is one of the outstanding challenges of modern astrophysics. Swift J1910.2-0546 is a candidate black hole low-mass X-ray binary that was discovered in 2012 when it entered an accretion outburst. To investigate the binary configuration and the accretion morphology, we monitored the evolution of the outburst for ≅3 months at X-ray, UV, optical (B, V, R, I), and near-infrared (J, H, K) wavelengths using Swift and SMARTS. The source evolved from a hard to a soft X-ray spectral state with a relatively cold accretion disk that peaked at ≅0.5 keV. A Chandra/HETG spectrum obtained during this soft state did not reveal signatures of an ionized disk wind. Both the low disk temperature and the absence of a detectable wind could indicate that the system is viewed at relatively low inclination. The multi-wavelength light curves revealed two notable features that appear to be related to X-ray state changes. First, a prominent flux decrease was observed in all wavebands ≅ 1-2 weeks before the source entered the soft state. This dip occurred in (0.6-10 keV) X-rays ≅ 6 days later than at longer wavelengths, which could possibly reflect the viscous timescale of the disk. Second, about two weeks after the source transitioned back into the hard state, the UV emission significantly increased while the X-rays steadily decayed. We discuss how these observations may reflect changes in the accretion morphology, perhaps related to the quenching/launch of a jet or the collapse/recovery of a hot flow.},

  doi          = {10.1088/0004-637X/784/2/122},

  url          = {https://www.osti.gov/biblio/22357243},
  journal      = {Astrophysical Journal},

  issn         = {0004-637X},

  number       = 2,

  volume       = 784,

  place        = {United States},

  year         = {Tue Apr 01 00:00:00 EDT 2014},

  month        = {Tue Apr 01 00:00:00 EDT 2014}

}

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