The EXOSAT medium energy (ME) sample of dwarf novae
The EXOSAT medium energy (ME) sample of dwarf novae
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EXOSAT 矮新星中能 (ME) 样本
DOI：
10.1086/173444
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发表时间：
1993
期刊：
影响因子：
--
通讯作者：
K. Shiokawa
中科院分区：
文献类型：
--
作者：
K. Mukai;K. Shiokawa
我们提出了我们的分析EXOSAT中能（ME）档案数据矮新星。用EXOSAT观测了许多矮新星;不幸的是，很大一部分用ME仪器没有探测到或探测到的程度很低。我们对最亮的矮新星天鹅座SS的分析表明，计数率和硬度比之间的相关性很小，与早期的报告相反。这很可能是执行背景减除时出现轻微误差的结果。这种明显的相关性的缺乏有利于在吸积盘和白色矮星之间形成一个致密的边界层作为硬X射线发射区，而不是一个扩展的日冕
We present our analysis of the EXOSAT medium energy (ME) archival data on dwarf novae. Many dwarf novae were observed with EXOSAT; unfortunately, a significant fraction resulted in nondetection or marginal detection with the ME instrument. Our analysis of the brightest dwarf nova, SS Cyg, shows little correlation between the count rate and the hardness ratio, contrary to an earlier report. This is likely to be the result of a slight error in background subtraction performed. The apparent lack of correlation favors a compact boundary layer between the accretion disk and the white dwarf as the hard X-ray emitting region, rather than an extended corona