Wind from T Tauri Stars

Details Wind from T Tauri Stars Wind from T Tauri Stars

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998pasj...50..587k&link_type=abstract

Publications of the Astronomical Society of Japan, v.50, p.587-595.

Astronomy and Astrophysics

Astronomy

1

Stars: Angular-Momentum Loss, Stars: Mass Loss, Stars: T Tauri Stars, Stars: Winds

Scientific paper

Previously, it was shown by DeCampli that an isothermal wind of T Tauri stars cannot explain both the mass-loss rates and X-ray observations. Since the assumption of an isothermal wind does not hold in general, we recalculated the structure of a steady and spherically symmetric stellar wind, taking the heating luminosity and its range as input parameters. Our result shows that when the heating luminosity becomes greater than 10(-4) LO , a sonic point lies inside the heating region, contrary to the case of the solar wind. In this case, there exist two solutions for the same heating luminosity and the same mass-loss rate. In one solution, heat is transported by conduction, and in the other solution it is transported by convection. When the heating luminosity is as high as 1 LO , the mass-loss rate is about 10(-9) ~ 10(-8}MO yr({-1)) . In the former solution, the corona shines with a temperature of about 7times 10(7 K) and with an X-ray luminosity of about 10(-3) LO , in agreement with X-ray observations. However, the time scale of the angular-momentum loss is greater than 10(8 yr) and this solution, itself, may be insufficient for the angular-momentum loss. This result stems from the smallness of the viscosity coefficient. If global magnetic fields exist, this problem may be solved. In the latter solution, the temperature is at most 4times 10(6}{ K) , but the time scale of the angular-momentum loss becomes about 10(7 yr) even if magnetic fields do not exist.

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