An infall model for the T Tauri phenomenon

Details An infall model for the T Tauri phenomenon An infall model for the T Tauri phenomenon

Dec 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976apj...210..377u&link_type=abstract

Astrophysical Journal, vol. 210, Dec. 1, 1976, pt. 1, p. 377-391.

Astronomy and Astrophysics

Astrophysics

201

Emission Spectra, Gravitational Collapse, Stellar Evolution, Stellar Spectra, T Tauri Stars, Variable Stars, H Alpha Line, H Beta Line, Kinetic Energy, Line Spectra, Radiative Transfer, Shock Layers, Stellar Models

Scientific paper

An infall model which produces P Cygni type II emission lines is presented. The blueshifted apparent absorption feature in these emission lines is interpreted in this model as the overlap region between a strong emission line centered near the rest velocity of the star and a weaker emission line at a velocity near -150 km/s. According to this model the energy source for the continuum and line-emission features observed in T Tauri stars is the kinetic energy of the infalling matter. A weak flux of soft X-rays is produced in the high-temperature postshock gas. These X-rays may be responsible for producing the nebulae observed near some T Tauri stars.

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