Radio-Continuum Emission from Shocked Stellar Winds in Low-Mass Stars

Details Radio-Continuum Emission from Shocked Stellar Winds in Low-Mass Stars Radio-Continuum Emission from Shocked Stellar Winds in Low-Mass Stars

Nov 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002apj...580..459g&link_type=abstract

The Astrophysical Journal, Volume 580, Issue 1, pp. 459-467.

Astronomy and Astrophysics

Astronomy

13

Hydrodynamics, Radio Continuum: Ism, Stars: Pre-Main-Sequence, Stars: Winds, Outflows

Scientific paper

Young stars of low and intermediate masses frequently show continuum emission in radio frequencies. The observed flux densities and spectral indices indicate that in most cases this emission is of thermal (free-free) origin and is produced in the powerful stellar winds emanating from the stars. However, this interpretation faces the problem of the ionization of the wind. Photoionization can be ruled out because of the insufficient number of UV photons emitted by this kind of star. In this paper, we present a model in which the ionization (and emission) is produced by internal shocks in the wind. These shocks are the result of periodic variations of the velocity of the wind at injection. It is shown that the free-free radio emission predicted by the model is in good agreement with those observed in young stars of low and intermediate masses.

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