X-rays from hot subdwarfs

详细信息    查看全文

• 作者：Sandro Mereghetti ; ^{sandro@iasf-milano.inaf.it" class="auth_mail" title="E-mail the corresponding author} ; Nicola La Palombara ^{nicola@iasf-milano.inaf.it" class="auth_mail" title="E-mail the corresponding author}
• 关键词：X-rays ; Hot subdwarfs ; Mass-loss ; Binaries ; White dwarfs ; Neutron stars
• 刊名：Advances in Space Research
• 出版年：2016
• 出版时间：1 September 2016
• 年：2016
• 卷：58
• 期：5
• 页码：809-820
• 全文大小：1019 K

文摘

Thanks to the high sensitivity of the instruments on board the XMM-Newton and Chandra satellites, it has become possible to explore the properties of the X-ray emission from hot subdwarfs. The small but growing sample of hot subdwarfs detected in X-rays includes binary systems, in which the X-rays result from wind accretion onto a compact companion (white dwarf or neutron star), as well as isolated sdO stars in which X-rays are probably due to shock instabilities in the wind. X-ray observations of these low mass stars provide information which can be useful also for our understanding of the winds of more luminous and massive early-type stars and can lead to the discovery of particularly interesting binary systems.