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    Bright Mini-outburst Ends the 12 yr Long Activity of the Black Hole Candidate Swift J1753.5-0127

    80253.pdf (3.498Mb)
    Access Status
    Open access
    Authors
    Zhang, G.B.
    Bernardini, F.
    Russell, D.M.
    Gelfand, J.D.
    Lasota, J.P.
    Qasim, A.A.
    Almannaei, A.
    Koljonen, K.I.I.
    Shaw, A.W.
    Lewis, F.
    Tomsick, J.A.
    Plotkin, Richard
    Miller-Jones, James
    Maitra, D.
    Homan, J.
    Charles, P.A.
    Kobel, P.
    Perez, D.
    Doran, R.
    Date
    2019
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Zhang, G.B. and Bernardini, F. and Russell, D.M. and Gelfand, J.D. and Lasota, J.P. and Qasim, A.A. and Almannaei, A. et al. 2019. Bright Mini-outburst Ends the 12 yr Long Activity of the Black Hole Candidate Swift J1753.5-0127. Astrophysical Journal. 876 (1): ARTN 5.
    Source Title
    Astrophysical Journal
    DOI
    10.3847/1538-4357/ab12dd
    ISSN
    0004-637X
    Faculty
    Faculty of Science and Engineering
    School
    School of Elec Eng, Comp and Math Sci (EECMS)
    Funding and Sponsorship
    http://purl.org/au-research/grants/arc/FT140101082
    Remarks

    Copyright © 2019 The American Astronomical Society. All rights reserved.

    URI
    http://hdl.handle.net/20.500.11937/80171
    Collection
    • Curtin Research Publications
    Abstract

    © 2019. The American Astronomical Society. All rights reserved. We present optical, UV, and X-ray monitoring of the short orbital period black hole X-ray binary candidate Swift J1753.5-0127, focusing on the final stages of its 12 yr long outburst that started in 2005. From 2016 September onward, the source started to fade, and within 3 months, the optical flux almost reached the quiescent level. Soon after that, using a new proposed rebrightening classification method, we recorded a mini-outburst and a reflare in the optical light curves, peaking in 2017 February (V ∼ 17.0) and May (V ∼ 17.9), respectively. Remarkably, the mini-outburst has a peak flux consistent with the extrapolation of the slow decay before the fading phase preceding it. The following reflare was fainter and shorter. We found from optical colors that the temperature of the outer disk was ∼11,000 K when the source started to fade rapidly. According to the disk instability model, this is close to the critical temperature when a cooling wave is expected to form in the disk, shutting down the outburst. The optical color could be a useful tool to predict decay rates in some X-ray transients. We notice that all X-ray binaries that show mini-outbursts following a main outburst are short orbital period systems (<7 hr). In analogy with another class of short-period binaries showing similar mini-outbursts, the cataclysmic variables of the RZ LMi type, we suggest that mini-outbursts could occur if there is a hot inner disk at the end of the outburst decay.

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