“Diffuse ionized gas”的版本间差异
跳到导航
跳到搜索
无编辑摘要 |
|||
| 第1行： | 第1行： | ||
==银河系中的DIG== |
==银河系中的DIG== |
||
*Referred to as the Reynolds layer, or warm ionized medium (WIM); |
*Referred to as the Reynolds layer, or warm ionized medium (WIM); |
||
*This warm (10^4 K), diffuse (n ~ 0.2 cm~3) gas fills 20% of the disk volume and accounts for most of the mass of ionized gas. |
*This warm (10^4 K), diffuse (n ~ 0.2 cm~3) gas fills 20% of the disk volume and accounts for most of the mass of ionized gas(90 percent). |
||
*In terms of energetics, the Galactic WIM requires at least 10^42 ergs s~1 to remain ionized. This power is more than can be comfortably supplied by supernova shocks, but significantly less than the Lyman continuum luminosity of massive stars. |
*In terms of energetics, the Galactic WIM requires at least 10^42 ergs s~1 to remain ionized. This power is more than can be comfortably supplied by supernova shocks, but significantly less than the Lyman continuum luminosity of massive stars. |
||
*[http://iopscience.iop.org/article/10.1086/306232/meta] |
*[http://iopscience.iop.org/article/10.1086/306232/meta] |
||
2016年3月8日 (二) 07:55的版本
银河系中的DIG
- Referred to as the Reynolds layer, or warm ionized medium (WIM);
- This warm (10^4 K), diffuse (n ~ 0.2 cm~3) gas fills 20% of the disk volume and accounts for most of the mass of ionized gas(90 percent).
- In terms of energetics, the Galactic WIM requires at least 10^42 ergs s~1 to remain ionized. This power is more than can be comfortably supplied by supernova shocks, but significantly less than the Lyman continuum luminosity of massive stars.
- [1]