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VbvAstE-001

Book Boris V. Vasiliev Astrophysics

the sum of separate

the sum of separate stars rotation. The possible combinations of a couple and their value of ∑ 2 1 ξi for stars consisting of light elements is shown in Table 8.4. star1 star2 ξ 1 + ξ 2 composed of composed of H H .25 H D 0.1875 H He 0.143 H hn 0.125 D D 0.125 D He 0.0815 D hn 0.0625 He He 0.037 He hn 0.0185 Table 8.4 The ”hn” notation in Table 8.4 indicates that the second component of the couple consists of heavy elements or it is a dwarf. The results of measuring of main parameters for close binary stars are gathered in [11]. For reader convenience, the data of these measurement is applied in the Table in Appendix. One can compare our calculations with data of these measurements. The distribution of close binary stars on value of (P/U)(P/T ) 2 is shown in Fig.8.1 on logarithmic scale. The lines mark the values of parameters ∑ 2 1 ξi for different light atoms in accordance with 8.27. It can be seen that calculated values the periastron rotation for stars composed by light elements which is summarized in Table8.4 are in good agreement with separate peaks of measured data. It confirms that our approach to interpretation of this effect is adequate to produce a satisfactory accuracy of estimations. 65

N -3.0 -2.5 -2.0 -1.5 -1.0 -0.5 0.0 0.5 12 12 He He+He D D+He H ; D+D H+He H+D H+H log(ξ 1 +ξ 2 ) 10 10 8 8 6 6 4 4 2 2 0 0 -3.0 -2.5 -2.0 -1.5 -1.0 -0.5 0.0 0.5 log[(P/U)(P/T) 2 ] Figure 8.1: The distribution of close binary stars [11] on value of (P/U)(P/T ) 2 . Lines show parameters ∑ 2 1 ξ i for different light atoms in according with 8.27. 66

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