Completing the puzzle of the 2004–2005 outburst in V0332+53: the brightening phase included
Completing the puzzle of the 2004–2005 outburst in V0332+53: the brightening phase included
复制标题
DOI：
10.1111/j.1365-2966.2009.15791.x
复制
发表时间：
2009-09
影响因子：
4.8
通讯作者：
S. Tsygankov;A. Lutovinov;A. L. M. F. Astrophysics;Garching;H Germany;S. R. Institute;Moscow;Russia.;I. Physics;N. Novgorod
中科院分区：
文献类型：
--
作者：
S. Tsygankov;A. Lutovinov;A. L. M. F. Astrophysics;Garching;H Germany;S. R. Institute;Moscow;Russia.;I. Physics;N. Novgorod
本文介绍了2004-2005年X射线脉冲星V0332+53强烈爆发期间RXTE天文台获得的数据分析。首次详细分析了爆发增亮阶段的观测资料。在增亮和衰减阶段的源参数和它们的演变的比较显示，没有任何滞后行为的证据。发现在增亮和衰减阶段，回旋吸收线的能量对光度的依赖关系几乎相同。完整的数据序列，包括爆发增亮和衰落阶段，使它有可能施加更严格的约束磁场的源。脉冲轮廓和脉冲分数的光度和光子能量的函数进行了研究。
Analysis of the data obtained with the RXTE observatory during a powerful outburst of the X-ray pulsar V0332+53 in 2004–2005 is presented. Observational data covering the outburst brightening phase are analysed in detail for the first time. A comparison of source parameters and their evolution during the brightening and fading phases shows no evidence for any hysteretic behaviour. It is found that the dependences of the energy of the cyclotron absorption line on the luminosity during the brightening and fading phases are almost identical. The complete data sequence including the outburst brightening and fading phases makes it possible to impose the more stringent constraints on the magnetic field in the source. The pulse profile and pulsed fraction are studied as functions of the luminosity and photon energy.