X-ray emission from star forming regions

被引：0
|
作者：
Flaccomio, E. [1 ]
机构：
[1] INAF Osservatorio Astron Palermo, I-90134 Palermo, Italy
来源：
X-RAY ASTRONOMY-2009: PRESENT STATUS, MULTI-WAVELENGTH APPROACH AND FUTURE PERSPECTIVES, PROCEEDINGS | 2010年 / 1248卷
关键词：
Stars: pre-main sequence; Stars: formation; planetary systems: protoplanetary disks; T-TAURI-STARS; ORION ULTRADEEP PROJECT; LOW-MASS STARS; YOUNG STARS; EXTREME-ULTRAVIOLET; LINE EMISSION; PROTOPLANETARY DISKS; CIRCUMSTELLAR DISKS; ACCRETION; NEBULA;
D O I：
10.1063/1.3475268
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Contrary to the classical "cold" view of star formation, star forming clouds and YSOs abound with high energy phenomena. YSOs of almost all masses are intense sources of X-rays, with luminosities well above those of main sequence stars. Most of this emission originates in coronae, qualitatively similar to those of the Sun and of other main sequence stars. X-rays are also emitted in shocks at the base of mass accretion funnels and in jets. Diffuse X-ray emission from high mass star forming cloud has also been detected. I discuss the current status of observations with regard to these X-ray emission mechanisms, and the influence of X-rays from YSOs on circumstellar disks.
引用
收藏
页码：3 / 8
页数：6
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