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    Outburst and Post-Outburst Active Phase of the Black Hole X-Ray Binary V4641 Sagittarii in 2002

    134627_17589_0308154v1.pdf (1.445Mb)
    Access Status
    Open access
    Authors
    Uemura, Makoto
    Kato, Taichi
    Ishioka, Ryoko
    Tanabe, Kenji
    Torii, Ken
    Santallo, Roland
    Monard, Berto
    Markwardt, Craig
    Swank, Jean
    Sault, Robert
    Macquart, Jean-Pierre
    Linnolt, Michael
    Kiyoto, Seiichiro
    Stubbings, Rod
    Nelson, Peter
    Richards, Tom
    Bailyn, Charles
    West, Doug
    Masi, Gianluca
    Miyashita, Atsushi
    Sano, Yasuo
    Scarmato, Toni
    Date
    2003
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Uemura, Makoto and Kato, Taichi and Ishioka, Ryoko and Tanabe, Kenji and Torii, Ken and Santallo, Roland and Monard, Berto and Markwardt, Craig and Swank, Jean and Sault, Robert and Macquart, Jean-pierre and Linnolt, Michael and Kiyoto, Seiichiro and Stubbings, Rod and Nelson, Peter and Richards, Tom and Bailyn, Charles and West, Doug and Masi, Gianluca and Miyashita, Atsushi and Sano, Yasuo and Scarmato, Toni. 2003. Outburst and Post-Outburst Active Phase of the Black Hole X-Ray Binary V4641 Sagittarii in 2002. Publications of Astronomical Society of Japan. 56 (SP1): pp. S61-S75.
    Source Title
    Publications of Astronomical Society of Japan
    Additional URLs
    http://pasj.asj.or.jp/v56/sp1/56s103/56s103-frame.html
    ISSN
    0004-6264
    Faculty
    Faculty of Science and Engineering
    Curtin Institute of Radio Astronomy
    URI
    http://hdl.handle.net/20.500.11937/7826
    Collection
    • Curtin Research Publications
    Abstract

    The black hole X-ray binary V4641 Sgr experienced an outburst in 2002 May, which was detected at X-ray, optical, and radio wavelengths. The outburst lasted for only 6 days, but the object remained active for the next several months. Here, we report on the detailed properties of light curves during the outburst and the post-outburst active phase. We reveal that rapid optical variations of -100s became more prominent when a thermal flare weakened and the optical spectrum flattened in the Ic, Rc, and V-band regions. In conjunction with the flat spectrum in the radio range, this strongly indicates that the origin of rapid variations is not thermal emission, but synchrotron emission. Just after the outburst, we detected repeated flares at optical and X-ray wavelengths. The optical and X-ray light curves exhibited a strong correlation with the X-rays lagging by about 7min. The X-ray lag can be understood in terms of a hot region propagating into the inner region of the accretion flow. The short X-ray lag, however, requires modifications of this simple scenario to account for the short propagation time. We also detected high-amplitude rapid variations 50 days after the outburst, which we call optical flashes. During the most prominent optical flash, the object brightened by 1.2mag only within 30s. The released energy indicates that the emission source should be at the innermost region of the accretion flow. (author abst.)

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