view Abstract Citations (49) References (44) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Galactic Fountains and Extended H i Disks Corbelli, E. ; Salpeter, E. E. Abstract Some of the hot material, ejected into the galactic halo by the more violent supernova events, can rise many kiloparsecs and then start cooling radiatively and falling back toward the outer part of the galactic plane (distances from the center >~20 kpc). Depending upon the temperature and mass-flow rate initiated by such an "outer galactic fountain," the dynamic hot downward flow can form an extended H I disk or shape and evaporate a preexisting one. These downward flows have been studied, using a one-dimensional steady state model which includes an extragalactic flux of soft X-rays but omits electron heat conduction. The pressure profile and column densities of H II and warm H I are given as functions of the injection temperature T_i_ and of the mass-flow rate. A small fraction of the total supernova energy release, if channeled into an outer galactic fountain with T_i_ ~ 2 or 3 x 10^6^ K, can form cool extended disks. A corona with T_i_ ~ 5-7 x 10^6^ K is more likely to evaporate and shrink a preexisting H I disk. If disk galaxies were formed with appreciably larger disks than now, as suggested by one type of quasar absorption lines, the subsequent shrinkage may have been caused by stronger hot fountains in young galaxies. Weak present-day fountains can also be effective in compressing an outer H I disk and, possibly, in giving it a sharp edge. Publication: The Astrophysical Journal Pub Date: March 1988 DOI: 10.1086/166116 Bibcode: 1988ApJ...326..551C Keywords: Cosmic Gases; Disk Galaxies; Ejecta; H I Regions; Spiral Galaxies; Absorption Spectra; Astronomical Models; Conductive Heat Transfer; High Temperature Gases; Quasars; Steady Flow; Thermal Stability; Astrophysics; GALAXIES: INTERNAL MOTIONS; GALAXIES: STRUCTURE; HYDRODYNAMICS; RADIO SOURCES: 21 CM RADIATION full text sources ADS |
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