Theoretical studies of mass loss and shock phenomena in cool star envelopes

Details Theoretical studies of mass loss and shock phenomena in cool star envelopes Theoretical studies of mass loss and shock phenomena in cool star envelopes

Feb 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988sao..reptq....h&link_type=abstract

Semiannual Progress Report No. 8, 1 Apr. - 30 Sep. 1987 Smithsonian Astrophysical Observatory, Cambridge, MA.

Astronomy and Astrophysics

Astrophysics

Emission Spectra, Plasma Heating, Shock Heating, Stellar Mass Ejection, Stellar Models, Stellar Spectra, Stellar Winds, T Tauri Stars, Far Infrared Radiation, H Alpha Line, Infrared Spectra, Oxygen, Sodium, Spectral Energy Distribution, Spectrum Analysis, Stellar Envelopes, Stellar Mass, Stellar Mass Accretion, Stellar Radiation, Sulfur

Scientific paper

To show the difficulty of producing the blue-shifted emission of (O I) and (S II) from T Tauri stars directly in the stellar wind, an element of gas in a radially expanding stellar wind was followed as it cooled and recombined. Results indicate that T Tauri winds must be heated at large distances from the star to produce the (S II) emission. A shock between the wind and the disk is an attractive mechanism to produce this heating. When the theory is applied to a simple disk model, a number of predictions and implications are evident, for example, that some T Tauri stars eject mass near the equatorial plane. In a second study, spectral energy distributions of T Tauri stars were analyzed to place limits on the amount of accretion which might occur during the early phase of stellar evolution. The best match to H-alpha line profiles is for models in which the turbulent velocity dominates close to the star, while expansion dominates farther out. Such a model predicts, for instance, that a mass loss rate of 1/10,000,000 solar masses per year is required to account for the blue-shifted Na I absorption of some objects.

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