A study of X-ray emission from Ap and Am stars
A study of X-ray emission from Ap and Am stars
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Ap 和 Am 星 X 射线发射的研究
DOI：
10.1086/183924
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发表时间：
1982
期刊：
影响因子：
--
通讯作者：
T. Snow
中科院分区：
文献类型：
--
作者：
W. Cash;T. Snow
爱因斯坦天文台的成像比例计数器对20颗被归类为Ap或Am的恒星进行了成像，以寻找日冕发射的证据。据发现，一个上午星星将不会是一个源（在10至28尔格/秒的水平），除非它是在一个光谱联星的周期低于约10天。密近双星中的X射线可以用晚型二次星的RS CVn效应来解释，证据是反对来自Am星的强辐射。在观测到的九颗Ap恒星中，有四颗被发现。虽然X射线可能是由未被探测到的晚型矮星伴星产生的，但大部分的探测结果使Ap星本身成为可能的发射源。
Twenty stars classified as either Ap or Am have been imaged by the Imaging Proportional Counter on the Einstein Observatory in a search for evidence of coronal emission. It is found that an Am star will not be a source (at the 10 to the 28th ergs/sec level) unless it is in a spectroscopic binary with a period below about 10 days. The X-rays in the close binaries can be explained by the RS CVn effect in the late-type secondary, and the evidence is against strong emission from Am stars. Among the nine Ap stars observed, four were detected. While it is possible that the X-rays are being generated by undetected late-type dwarf companions, the large fraction of detections makes the Ap stars themselves the likely source of emission.