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The models of non-rotating and rotating 2.31M
\ stars of Population I composition have been calculated, starting at the threshold of stability. A 2.31M
\ star was chosen to compare the results with the observational parameters of the primary component of the well-known detached binary YZ Cassiopeiae. The effects of rotation on the internal structure during the evolution of the star were studied by constructing sequences of axisymmetric rotating models under the assumption that angular momentum was conserved according to a predetermined angular velocity distribution depending on the structure of the star.The first section of this paper deals with effects of rotation on the evolutionary behaviours of the 2.31M
\ star through the pre-Main-Sequence evolution as well as the zero-age Main Sequence.In the second section of this paper, the evolutionary studies have been extended up to near-hydrogen exhaustion phase in order to obtain a theoretical model corresponding to the given mass and radius of the primary component of YZ Cassiopeiae. The theoretical models were found to be in a good agreement with observational parameters. The computed rotating models of the primary of YZ Cassiopeiae indicates that its evolutionary age is 6.01×108 years; and the central hydrogen content 0.183 — which means that about 75% of its original value was depleted. 相似文献
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Evolution of the gravitational contraction phase of stars having masses 0.3 < M/M⊙ < 1.5 were studied along with deuterium
burning. The equation of state developed by Mihalas et al. (1988) and OPAL opacity tables were used in our investigation.
The theoretical time lines were compared with observations.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
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