Modelling the X-ray, EUV and infrared coronal-line emission from PNe

被引：0
|
作者：
Zhekov, SA
Perinotto, M
机构：
[1] UNIV FLORENCE, DIPARTIMENTO ASTRON & SCI SPAZIO, I-50125 FLORENCE, ITALY
[2] BULGARIAN ACAD SCI, SPACE RES INST, BU-1000 SOFIA, BULGARIA
[3] OSSERV ASTROFIS ARCETRI, I-50125 FLORENCE, ITALY
来源：
ASTRONOMY & ASTROPHYSICS | 1996年 / 309卷 / 02期
关键词：
planetary nebulae; general; X-ray; interstellar infrared; interstellar; lines;
D O I：
暂无
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present spherically symmetric interacting-winds model of planetary nebulae aimed at the study of the hot bubble in their structure. A similarity solution for the hot-bubble structure is derived in the case of a time-dependent wind of the central star and taking into account the effects of thermal conductivity. This solution is used to model the X-ray, EUV and infrared-coronal line emission (lambda > 1 mu) from planetary nebulae. These results can be used to check the consistency of the interacting-winds model by a comparison with space and ground-based observations with high spatial resolution.
引用
收藏
页码：648 / 654
页数：7
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