“Diffuse ionized gas”的版本间差异

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[[electron temperature|电子温度]]
[[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==
==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(90 percent).
*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]] 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.
*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]

2024年7月22日 (一) 01:26的最新版本

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⊙)
  • 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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