Dynamics of Cool Fronts in Optically Thin Hot Plasmas

Details Dynamics of Cool Fronts in Optically Thin Hot Plasmas Dynamics of Cool Fronts in Optically Thin Hot Plasmas

Mar 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...531..838i&link_type=abstract

The Astrophysical Journal, Volume 531, Issue 2, pp. 838-845.

Astronomy and Astrophysics

Astronomy

4

Hydrodynamics, Ism: General, Plasmas, Shock Waves

Scientific paper

Steady cool fronts supported by nonsaturated thermal conduction in optically thin plasmas are analyzed. Explicit relations for the pressure (p2), number density (n2), temperature (T2), and flow velocity (v2) behind the front are found as functions of the temperature T1 and the intake Mach number M1 ahead of the cool front. Weak cool fronts may exist only for intake velocities less than the isothermal sound speed. Behind these kinds of fronts, the flow retards, cools down, and is compressed. Strong cool fronts exist for intake Mach numbers greater than a threshold value depending on T1. In these fronts, two compression branches appear, a high-compression branch well below the isotherm for which n1/n2<(γ-1)/(γ+1) and a weak-compression branch, close to (but below) the isotherm. In particular, in the high-compression branch for low values of M1 quasi-isobaric cool fronts occur when the ratio n1/n2 is close to the maximum value, where this branch just emerges, beyond which the pressure of the flow behind the front increases when n1/n2 decreases. The implications of these results on the formation of cool condensations in the hot interstellar medium gas and in the solar atmosphere are outlined.

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