RXTE /ASM and Swift /BAT observations of spectral transitions in bright X-ray binaries in 2005–2010
RXTE /ASM and Swift /BAT observations of spectral transitions in bright X-ray binaries in 2005–2010
复制标题
DOI：
10.1088/1674-4527/11/4/006
复制
发表时间：
2010-12
影响因子：
1.8
通讯作者：
Jing Tang;Wenfei Yu;Zhen Yan
中科院分区：
文献类型：
--
作者：
Jing Tang;Wenfei Yu;Zhen Yan
我们已经研究了X射线光谱状态转换，可以看到在长期监测光变曲线的明亮的X射线双星从全天监视器（ASM）板载罗西X射线定时探测器（RXTE）和突发警报望远镜（BAT）板载斯威夫特在五年期间，从2005年至2010年。我们已经应用了一个程序来自动识别的硬软（H-S）的光谱状态转换的明亮的X射线双星监测的ASM和BAT。我们总共确定了128个硬到软的转变，其中59个发生在2008年之后。我们还测定了Yu & Yan之后约30个明亮的持久和瞬态黑洞和中子星星双星的跃迁通量和随后软态的峰值通量，更新了对应于H-S跃迁的光度和随后软态的峰值光度的测量结果，发现2008-2010年的光谱跃迁的光度相关性和光度范围与2008年以前的光谱跃迁的光度相关性和光度范围基本相同。这进一步加强了这样的想法，即在银河系X射线双星中发生H-S光谱跃迁的光度是由非稳态吸积参数决定的，例如质量吸积率的变化率，而不是质量吸积率本身。相关性也被发现在单个源4U 1608-52和4U 1636-53的数据中保持。
We have studied X-ray spectral state transitions that can be seen in the long-term monitoring light curves of bright X-ray binaries from the All-Sky Monitor (ASM) onboard the Rossi X-ray Timing Explorer (RXTE) and the Burst Alert Telescope (BAT) onboard Swift during a period of five years from 2005 to 2010. We have applied a program to automatically identify the hard-to-soft (H-S) spectral state transitions in the bright X-ray binaries monitored by the ASM and the BAT. In total, we identified 128 hard-to-soft transitions, of which 59 occurred after 2008. We also determined the transition fluxes and the peak fluxes of the following soft states, updated the measurements of the luminosity corresponding to the H-S transition and the peak luminosity of the following soft state in about 30 bright persistent and transient black hole and neutron star binaries following Yu & Yan, and found the luminosity correlation and the luminosity range of spectral transitions in data between 2008–2010 are about the same as those derived from data before 2008. This further strengthens the idea that the luminosity at which the H-S spectral transition occurs in the Galactic X-ray binaries is determined by non-stationary accretion parameters such as the rate-of-change of the mass accretion rate rather than the mass accretion rate itself. The correlation is also found to hold in data of individual sources 4U 1608-52 and 4U 1636-53.