“Diffuse ionized gas”的版本间差异

2016年6月15日 (三) 03:09的版本

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).

电子密度比 hot gas要高一点（ Typical values of the central electron density, central cooling time and total mass for the ETGs are ~ 0.1cm−3, ~ 5 x 10^6 yr and 5 x 1O^9 M⊙）

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.
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@@ 第3行： / 第3行： @@
 *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).
-:*[[electron density|电子密度比]]hot gas要高一点（ Typical values of the central electron density, central cooling time and total mass  for the ETGs are ~ 0.1cm−3, ~ 5 x 10^6 yr and 5 x 1O^9 M⊙）
+:*[[electron density|电子密度比]] hot gas要高一点（ Typical values of the central electron density, central cooling time and total mass  for the ETGs are ~ 0.1cm−3, ~ 5 x 10^6 yr and 5 x 1O^9 M⊙）
 *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]