Computer Science
Scientific paper
Mar 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982msngr..27....4l&link_type=abstract
The Messenger, No.27, P. 4, 1982
Computer Science
1
Scientific paper
Stars which are so young that they are still contracting and have not yet reached the main sequence are called pre-mainsequence stars or pms stars. Observationally it is possible to distinguish between several categories of pms stars representing different kinds of stars and phases of evolution. An important and very weil observed (though not weil understood) group of such stars are the T-Tauri stars. They are generally found close to the interstellar clouds in which they were born, and compared to normal older stars they exhibit several peculiarities such as: irregular light variations, strong emission lines, high lithium abundance and excess emission both at ultraviolet and infrared wavelengths. If one determines the luminosities and surface temperatures for T-Tauri stars and plots them in an HR-diagram (such as Fig. 1) one finds that they occupy a region weil above the main sequence. This location coincides with theoretical evolutionary tracks for contracting stars with masses of about 1 solar mass, calculated by Iben. Iben's models which are the ones which best agree with the latest observations of pms stars also show that the T-Tauri are younger than a few million years. Because their masses appear to be about that of the sun we identify the T-Tauri stars as the progenitors of solar-type stars.
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