Predicted extreme-ultraviolet line emission for nearby main-sequence B stars
Predicted extreme-ultraviolet line emission for nearby main-sequence B stars
复制标题
预测附近主序 B 星的极紫外线发射
DOI：
10.1086/170614
复制
发表时间：
1991
期刊：
影响因子：
--
通讯作者：
W. Waldron
中科院分区：
文献类型：
--
作者：
J. Macfarlane;J. Cassinelli;B. Welsh;P. Vedder;J. Vallerga;W. Waldron
O星和B星的X射线发射源目前仍是争论的主题。冲击波通过O星和B星的风传播，以前曾被提出来解释它们观测到的X射线光度。速度跳跃数百公里/秒的强烈冲击可以将部分风加热到10 6 - 10 7 K，产生X射线和极紫外线（EUV）发射线的主要来源。或者，风底部的日冕也可能是X射线发射的原因。本文研究了早期B星高温X射线发射区产生的EUV谱线的特征
The source of the X-ray emission from O and B stars is currently the subject of debate. Shocks propagating through the winds of O and B stars have previously been proposed to explain their observed X-ray luminosities. Strong shocks with velocity jumps of several hundred km/s can heat portions of the wind to 10 6 -10 7 K, producing major sources of X-ray and extreme-ultraviolet (EUV) emission lines. Alternatively, a corona at the base of the wind might also be responsible for the X-ray emission. Here, the characteristics of EUV lines produced in high-temperature X-ray emitting regions of early B stars are investigated