Global ISM model
Diving into the complexities of global and two-phase equilibrium ISM models based on theories by Wolfire, McKee, Hollenbach, and Tielens. Explore the ionization and heating processes involving FUV, X-ray, and cosmic rays, alongside cooling mechanisms like [CII] and Lya. Discover how varying factors like metallicity influence the stability and density of P2 phases. Delve into the interconnected nature of hot gas, supernovae tunnels, and the three-phase model in galactic disks, reshaping our understanding of stellar evolution and ISM dynamics.
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Presentation Transcript
Two phase model (Field, Goldsmith, Habing) Both Theories Are Based on HI in Two-Phase Equilibrium? (Wolfire, McKee, Hollenbach, & Tielens 2003) Ionization: FUV, X-ray, C.R. Heating: P.E., C.R., X-ray/EUV Cooling: [CII], [OI], Lya, e- recombination stable P2phase? P2phase /k 3000 G0 /fD K cm-3? where G0 = FUV radiation/local ISM value ? fD= (1+3.1 Z 0.365)/4.1 ? Z = metallicity relative to solar? n 2phase 20 G0 /fD cm-3 ?
SupernovaeTunnelsThree-phase model Radiative lifetime of hot gas (supernova interior) is long If the star-formation is high then multiple supernovae in given regions The supernovae connect Subsequent supernovae take place in a medium which is hot Radiative lifetime increases Soon the galactic disk is occupied by hot gas (displacing the WNM and WIM Three=phase model of the ISM
