The dynamics of a Galactic fountain

Details The dynamics of a Galactic fountain The dynamics of a Galactic fountain

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999arep...43..142s&link_type=abstract

Astronomy Reports, Volume 43, Issue 3, March 1999, pp.142-148

Astronomy and Astrophysics

Astronomy

Scientific paper

In the "galactic fountain" model, hot, buoyant gaseous cavities provide an important mechanism for the transfer of mass and energy in the Galactic halo. The influence of thermal conductivity and radiative losses on the evolution of such cavities is examined. The joint action of heat conduction and radiative cooling leads to the development of a cooling wave propagating in the direction of the hot (thermally unstable) gas. At temperatures typical for hot interstellar gas, the cavities are subject to erosion by the intrusion of such cooling waves. This effect substantially decreases the efficiency of the galactic fountain: the rate of ejection of hot gas from the disk (M_* <<< 0.3 M_solar/yr) is not sufficient to support the halo in a steady state.

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