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

Tutkimustuotos: Lehtiartikkelivertaisarvioitu

Tutkijat

  • G-B Zhang
  • F. Bernardini
  • D. M. Russell
  • J. D. Gelfand
  • J-P Lasota
  • A. Al Qasim
  • A. AlMannaei
  • Karri Koljonen

  • A. W. Shaw
  • F. Lewis
  • J. A. Tomsick
  • R. M. Plotkin
  • J. C. A. Miller-Jones
  • D. Maitra
  • J. Homan
  • P. A. Charles
  • P. Kobel
  • D. Perez
  • R. Doran

Organisaatiot

  • Chinese Academy of Sciences
  • New York Univ Abu Dhabi
  • INAF Osservatorio Astron Capodimonte, Istituto Nazionale Astrofisica - Italy
  • NYU, New York University, Ctr Cosmol & Particle Phys
  • Nicolaus Copernicus Astron Ctr, Polish Academy of Sciences
  • Univ Coll London, University College London, University of London, Mullard Space Sci Lab
  • University of Alberta
  • Liverpool John Moores Univ, Liverpool John Moores University, Astrophys Res Inst
  • University of California at Berkeley
  • Curtin Univ, Curtin University, Int Ctr Radio Astron Res
  • Wheaton Coll, Dept Phys & Astron
  • SRON, Netherlands Inst Space Res
  • University of Southampton
  • Gymnase Bugnon Sevelin
  • NUCLIO Nucleo Interact Astron
  • University of Turku

Kuvaus

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.

Yksityiskohdat

AlkuperäiskieliEnglanti
Artikkeli5
Sivumäärä10
JulkaisuAstrophysical Journal
Vuosikerta876
Numero1
TilaJulkaistu - 1 toukokuuta 2019
OKM-julkaisutyyppiA1 Julkaistu artikkeli, soviteltu

ID: 34112948