• 主题
高级搜索  >
历史搜索 清空历史
首页> 外文期刊>The Astrophysical journal >ACCRETION ONTO THE COMPANION OF η CARINAE DURING THE SPECTROSCOPIC EVENT. Ⅱ. X-RAY EMISSION CYCLE
【24h】

ACCRETION ONTO THE COMPANION OF η CARINAE DURING THE SPECTROSCOPIC EVENT. Ⅱ. X-RAY EMISSION CYCLE

机译：光谱事件中ηCarinae同伴的吸收。 Ⅱ。 X射线发射周期

获取原文
获取原文并翻译 | 示例
           
页面导航
  • 摘要
  • 著录项
  • 相似文献
  • 相关主题

摘要

We calculate the X-ray luminosity and light curve for the stellar binary system η Car for the entire orbital period of 5.54 yr. By using a new approach we find, as suggested in previous works, that the collision of the winds blown by the two stars can explain the X-ray emission and temporal behavior. Most X-ray emission in the 2-10 keV band results from the shocked secondary stellar wind. The observed rise in X-ray luminosity just before minimum is due to the increase in density and subsequent decrease in radiative cooling time of the shocked fast secondary wind. Absorption, particularly of the soft X-rays from the primary wind, increases as the system approaches periastron and the shocks are produced deep inside the primary wind. However, absorption cannot account for the drastic X-ray minimum. The 70 day minimum is assumed to result from the collapse of the collision region of the two winds onto the secondary star. This process is assumed to shut down the secondary wind, and hence the main X-ray source. We show that this assumption provides a phenomenological description of the X-ray behavior around the minimum.
机译：我们在整个5.54年的轨道周期内计算了恒星二元系统ηCar的X射线光度和光曲线。通过使用一种新的方法，我们发现，如先前的研究所示，两颗恒星吹来的风的碰撞可以解释X射线的发射和时间行为。 2-10 keV波段中的大多数X射线发射是由受到冲击的次级恒星风引起的。观测到的X射线光度刚好在最小值之前的升高是由于密度的增加以及随后冲击的快速二次风的辐射冷却时间的减少所致。随着系统接近星云，并且冲击在初级风的内部深处产生，特别是来自初级风的软X射线的吸收增加。但是，吸收不能解释剧烈的X射线最小值。假定最少70天是由于两次风的碰撞区域塌陷到副星上。假定此过程将关闭次级风，从而关闭主X射线源。我们表明，该假设提供了最小值附近X射线行为的现象学描述。

著录项

相似文献

  • 外文文献
  • 中文文献
  • 专利
获取原文

客服邮箱：kefu@zhangqiaokeyan.com

京公网安备：11010802029741号 ICP备案号：京ICP备15016152号-6 六维联合信息科技 (北京) 有限公司©版权所有

  • 客服微信

  • 服务号