Constraints on accretion column parameters for the intermediate polar LS Pegasi from the power spectrum of its optical light curve

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• 作者：A. N. Semena (19331)
  M. G. Revnivtsev (19331)
  I. M. Khamitov (29331)
  R. A. Burenin (19331)
  T. Ak (39331)
  Z. Eker (29331) (49331)
  M. N. Pavlinsky (19331)
  
• 关键词：low ; mass X ; ray binaries ; accretion ; thermal instability in accretion column
• 刊名：Astronomy Letters
• 出版年：2013
• 出版时间：April 2013
• 年：2013
• 卷：39
• 期：4
• 页码：227-236
• 全文大小：633KB
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• 作者单位：A. N. Semena (19331)
  M. G. Revnivtsev (19331)
  I. M. Khamitov (29331)
  R. A. Burenin (19331)
  T. Ak (39331)
  Z. Eker (29331) (49331)
  M. N. Pavlinsky (19331)
  
  19331. Space Research Institute, Russian Academy of Sciences, Profsoyuznaya ul. 84/32, Moscow, 117997, Russia
  29331. TUBITAK National Observatory, Antalya, 07058, Turkey
  39331. Scientific Faculty, Department of Astronomy and Space Science, Istanbul University, Istanbul, Turkey
  49331. Faculty of Sciences, Department of Space Science and Technology, Akdeniz University, Antalya, Turkey
  
• ISSN：1562-6873

文摘

The properties of the hot zone in the accretion flow near the surface of a magnetized white dwarf have been studied. For this purpose, the aperiodic optical variability of LS Peg, one of the brightest intermediate polars in the northern sky, has been investigated. The main radiation of the hot zone, which is then reemitted in the optical band, results from the radiation of an optically thin plasma heated during the passage of the accretion flow of a standing shock. Recently, Semena and Revnivtsev (2012) have shown that the aperiodic variability (flickering) of accreting magnetized white dwarfs should have a characteristic feature in the range of Fourier frequencies corresponding to the plasma cooling time in this hot region. The photometric brightness measurements for LS Peg made with the RTT-150 telescope using a high-speed ANDOR iXon CCD array have allowed the break frequency in the power spectrum of the source’s variability to be constrained. Constraints on the geometry of the accretion column for the white dwarf in LS Peg and on the plasma parameters in it have been obtained.