Centrifugally driven winds from protostellar disks. I - Wind model and thermal structure

Details Centrifugally driven winds from protostellar disks. I - Wind model and thermal structure Centrifugally driven winds from protostellar disks. I - Wind model and thermal structure

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...408..115s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 408, no. 1, p. 115-159.

Astronomy and Astrophysics

Astrophysics

93

Accretion Disks, Protostars, Star Formation, Stellar Models, Stellar Winds, Temperature Distribution, Electron Density (Concentration), Gas Ionization, Hydrogen

Scientific paper

The thermal structure of a wind that is centrifugally driven from the surface of a protostellar disk is studied. A generalized version of the Blandford and Payne self-similar wind model is introduced, and the temperature and ionization distributions in the outflow are investigated. For the evolution of atomic winds, the heat equation and the rate equations that describe the ionization and excitation state of hydrogen are solved self-consistently. Ambipolar diffusion is found to be a robust mechanism for heating the gas. In the more powerful outflows, molecular hydrogen is collisionally dissociated close to the disk surface, and hydrogen is mainly atomic within a few astronomical units from the central source. It is also demonstrated that these outflows have enough momentum to lift dust grains from the disk surface.

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