Considering Buoyancy in Calculations of the Hot SNR Gas in the Thick Disk of the Galaxy

Details Considering Buoyancy in Calculations of the Hot SNR Gas in the Thick Disk of the Galaxy Considering Buoyancy in Calculations of the Hot SNR Gas in the Thick Disk of the Galaxy

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...206.3809s&link_type=abstract

American Astronomical Society Meeting 206, #38.09; Bulletin of the American Astronomical Society, Vol. 37, p.491

Astronomy and Astrophysics

Astronomy

Scientific paper

A significant minority of galactic supernova explosions occur in the thick-disk, away from the galactic midplane. According to computer simulations, even if buoyancy is neglected the population of remnants born in the thick-disk contributes noticeably to the quantity of hot interstellar gas (traced by 1/4 keV X-rays, ultraviolet resonance line photons, and O VI column density) found in the high latitude sky. Furthermore, hot gas in the galactic thick-disk is thought to rise buoyantly, eventually cool, and later return to the disk. In this way, buoyancy is thought to drive a vertical circulation pattern which redistributes metals, thermal energy, and highly ionized gas into the upper reaches of the thick-disk and into the halo. In order to predict the longevity, appearance, and dynamics of this hot gas, we use a detailed computer simulation to model supernova remnants born at various heights above the galactic midplane and then we combine the simulation results with analytic calculations of buoyant motion. The resulting estimates of the hot bubbles' rise times, rise distances, high ion column densities, ultraviolet resonance line emission, and 1/4 keV X-ray emission are compared with observations of the high latitude sky.
This work was supported by NASA grant number NNG04GD78G.

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