The Radiative Energy Loss from the Shock Front

Details The Radiative Energy Loss from the Shock Front The Radiative Energy Loss from the Shock Front

Jun 1973

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1973pthph..49.1911n&link_type=abstract

Progress of Theoretical Physics, Vol. 49, No. 6, pp. 1911-1931

Physics

23

Scientific paper

The radiation loss from shock waves which are generated during the collapse of protostars has a great effect on the structure of protostars. In this paper, the effects of the continuum and line radiations on the shock structure are investigated and the radiation loss rates are calculated. Plane steady shocks are assumed and the ambient conditions are taken as v=60 ˜ 20 km/sec and ρ=10-8 ˜ 10-13 g/cm3. The atmospheres are assumed to consist of pure hydrogen atoms which have only three levels, i.e., the ground, excited and ionized levels. The computed results show that about 90 percent of the shock's initial kinetic energy escapes ashead of the shock front as the Balmer continuum radiation. However, in the case of low shock velocity (v ≲ 30 km/sec) or high ambient density (ρ ≳ 10-8 g/cm3), the fraction of the lost energy decreases below about 80 percent.

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