Pre-main Sequence Evolution
As can be seen from the calculations of cloud collapse described in Sect. 7.2, stars with mass M >3M ⊙ appear in the optical range immediately near to the main sequence. Objects of lower mass exist for part of the time as optical stars with radiation due to gravitational contraction energy. Consider evolution of a star from its appearance in the optical region until it reaches the main sequence, and its central temperature becomes sufficiently high to initiate a nuclear reaction converting hydrogen into helium (see review ).
KeywordsMain Sequence Stellar Mass Young Star Evolutionary Track Tauri Star
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