Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...361..546r&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 361, Oct. 1, 1990, p. 546-569. Research supported by NASA.
Astronomy and Astrophysics
Astrophysics
49
Neutral Currents, Pre-Main Sequence Stars, Protostars, Stellar Envelopes, Stellar Mass Ejection, Stellar Winds, Hydrogen, Photochemical Reactions, Photoionization
Scientific paper
The physical processes that control the thermal structure of lightly ionized winds from cool protostars are discussed. Attention is concentrated on the hydrogen gas, and the heating, cooling, and chemical processes that affect the neutral and ionic species of atomic and molecular hydrogen are examined. Warm silicate dust may condense out of the cooling wind and may heat the gas through collisions. Singly ionized sodium atoms, which do not recombine for the mass-loss rates considered, set a lower limit to the ionization fraction in the wind. Magnetic fields, which are presumed to accelerate the wind, couple directly to the ionic component of the gas and transfer momentum and energy to the neutral component through collisions. This process of ambipolar diffusion is found to be the dominant source of heat input to the gas.
Glassgold Alfred E.
Ruden Steven P.
Shu Frank H.
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