Recovery of the orbital parameters and pulse evolution of V0332+53 during a huge outburst

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The high mass X-ray binary (HMXB) V0332+53 became active at the end of 2004, with the outburst being monitored by RXTE and INTEGRAL at hard X-rays. Here, the orbital parameters are measured with the hard X-ray data through the fitting of the Doppler-shifted spin periods. The derived orbital period and the eccentricity are consistent with those reported by Stella et al. (1985) from earlier EXOSAT observations, whereas the projected semimajor axis and the periastron longitude are found to differ, from 48 {+-} 4 to 86{sub -10}{sup +6} lt-s and from 313{sup o} {+-} 10 to 282{sup o} {+-} 14, respectively. ... continued below

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Zhang, S; Qu, J L; Song, L M & Torres, D F May 5, 2005.

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The high mass X-ray binary (HMXB) V0332+53 became active at the end of 2004, with the outburst being monitored by RXTE and INTEGRAL at hard X-rays. Here, the orbital parameters are measured with the hard X-ray data through the fitting of the Doppler-shifted spin periods. The derived orbital period and the eccentricity are consistent with those reported by Stella et al. (1985) from earlier EXOSAT observations, whereas the projected semimajor axis and the periastron longitude are found to differ, from 48 {+-} 4 to 86{sub -10}{sup +6} lt-s and from 313{sup o} {+-} 10 to 282{sup o} {+-} 14, respectively. This would indicate an angular speed of {ge} 1.6 {sup o} {+-} 0.9 yr{sup -1} for the orbit over the past 20 years. The periastron passage time, TJD 13367 {+-} 1, is just around the time when the intensity reached the maximum and, an orbital period earlier is the time when the outburst occurred. This correlation resembles the behavior of a Type I outburst. During the outburst the source spun up with {dot P}{sub spin} = 8.01{sub -1.14}{sup 1.00} x 10{sup -6} s day{sup -1}. The evolution of the pulse profile is highly intensity dependent. The separation of the double pulses kept almost constant ({approx} 0.47) when the source was bright, and dropped to 0.37 within {le}3 days as the source became weaker. The pulse evolution of V0332+53 may correlate to the change in the dominance of emission between fan-beam and pencil-beam mechanisms.

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PDF-file: 13 pages; size: 0.2 Mbytes

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  • Journal Name: Astrophysical Journal Letters; Journal Volume: 630

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  • Report No.: UCRL-JRNL-212131
  • Grant Number: W-7405-ENG-48
  • Office of Scientific & Technical Information Report Number: 878187
  • Archival Resource Key: ark:/67531/metadc879206

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  • May 5, 2005

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  • Sept. 21, 2016, 2:29 a.m.

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  • Dec. 8, 2016, 9:10 p.m.

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Zhang, S; Qu, J L; Song, L M & Torres, D F. Recovery of the orbital parameters and pulse evolution of V0332+53 during a huge outburst, article, May 5, 2005; Livermore, California. (digital.library.unt.edu/ark:/67531/metadc879206/: accessed December 12, 2018), University of North Texas Libraries, Digital Library, digital.library.unt.edu; crediting UNT Libraries Government Documents Department.