Computer Science – Sound
Scientific paper
Dec 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...18311404b&link_type=abstract
American Astronomical Society, 183rd AAS Meeting, #114.04; Bulletin of the American Astronomical Society, Vol. 25, p.1462
Computer Science
Sound
Scientific paper
We have calculated the time-dependent, nonequilibrium thermal and ionization history of gas cooling radiatively from 10(6) K in a one-dimensional, planar,steady-state flow model of the galactic fountain, including the effects of radiative transfer. We find that inclusion of the effects of self-ionization of the flow, combined with the requirement that the gas undergo a constant density (isochoric) phase in its evolution allows such a flow to match the observed galactic halo column densities of C IV, Si IV, and N V and UV emission from C IV and O III for a range of initial temperatures (5.5 < log T0 <6.5) and cooling regions sizes homogenous on scales of D0>15 pc.For an initial flow velocity v0 ~ 100km/s, comparable to the sound speed of a 10(6) K gas, the initial density is found to be n_{H,0} ~ 2times 10(-2) cm(-3) , in reasonable agreement with other observational estimates of ionized halo gas, and D0 ~ 40pc. We compare predicted H alpha fluxes, total ionizing flux, free-free radio emission, and broadband X-ray fluxes with observed values. Finally, we present results of 1-D hydrodynamical calculations of radiative shocks lead to the physical conditions necessary to produce such a cooling flow.
Benjamin Robert A.
Shapiro Paul R.
No associations
LandOfFree
Cooling Galactic Fountain Gas does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Cooling Galactic Fountain Gas, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Cooling Galactic Fountain Gas will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-781825