“Diffuse ionized gas”的版本间差异

2024年7月22日 (一) 01:26的最新版本

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1行： / 第1行： @@
 [[electron temperature|电子温度]]
+==[[IFS观测]]==
+*DIG可以用Ha的等值宽度来做判据，EW(Ha)双峰分布
+*arXiv1907.08635：讨论了DIG对金属丰度测量的影响
 ==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).
-:*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⊙）
+:*[[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]