Abstract
A semi-empirical formulation is given of the rate of stellar mass loss by stellar winds. Evolutionary studies of stars in the pre-main sequence (T Tauri) stage are presented for a variety of rates of mass loss. It has been found that different mass loss rates produce only small changes in the positions of equal evolutionary time lines in HR diagrams. Thus it is concluded that the spread of points in HR diagrams of young clusters results from a spread in their times of formation. This is consistent with the initiation of star formation by violent hydrodynamic compression of a typical interstellar cloud.
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Ezer, D., Cameron, A.G.W. Pre-main sequence stellar evolution with mass loss. Astrophys Space Sci 10, 52–70 (1971). https://doi.org/10.1007/BF00654605
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DOI: https://doi.org/10.1007/BF00654605