VbvAstE-001

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log L/L o 6 5 4 measured L~M 3.74 3 2 1 theory L~M 11/3 0 -1 -0.1 0.1 0.3 0.5 0.7 0.9 1.1 1.3 1.5 log M/M o Figure 6.3: The dependence of star luminosity on the star mass of close binary stars [11]. The luminosities are normalized to the luminosity of the Sun, the stars masses are normalized to the mass of the Sum. The data are shown on double logarithmic scale. The solid line shows the result of fitting of measurement data L ∼ M 3.74 . The theoretical dependence L ∼ M 11/3 (Eq.6.24) is shown by dotted line. 51
Figure 6.4: The schematic of the star interior 6.3.1 The compilation of the results of calculations Let us put together the results of calculations. It is energetically favorable for the star to be divided into two volumes: the core is located in the central area of the star and the atmosphere is surrounding it from the outside. (Fig.6.4). The core has the radius: ( a B c R ⋆ = 2.08 Z(A/Z) Gm 2 p It is roughly equal to 1/10 of the stellar radius. At that the mass of the core is equal to ) 1/2 ≈ 1.41 · 1011 cm. (6.25) Z(A/Z) M ⋆ = 6.84 M Ch ( A Z ) 2 . (6.26) It is almost exactly equal to one half of the full mass of the star. 52
Page 3 and 4: Boris V.Vasiliev ASTROPHYSICS and a
Page 5 and 6: 4
Page 7 and 8: 5 The main parameters of star 29 5.
Page 9 and 10: 8
Page 11 and 12: theories of stars that are not purs
Page 13 and 14: But plasma is an electrically polar
Page 15 and 16: can be described by definite ration
Page 17 and 18: But even at so high temperatures, a
Page 19 and 20: 2.2 The energy-preferable state of
Page 21 and 22: 20
Page 23 and 24: 3.2 The equilibrium of a nucleus in
Page 25 and 26: 24
Page 27 and 28: As a result, the electric force app
Page 29 and 30: and in accordance with Eq.(4.11), t
Page 31 and 32: The total kinetic energy of plasma
Page 33 and 34: we obtain η = 20 = 6.67, (5.24) 3
Page 35 and 36: 40 N 35 30 10 9 8 7 6 5 4 3 2 1 A/Z
Page 37 and 38: One can show it easily, that in thi
Page 39 and 40: 2.10 log (TR/R o T o ) 1.55 1.00 me
Page 41 and 42: averaged temperature and averaged p
Page 43 and 44: log R/R o 1.5 1.3 1.1 0.9 measured
Page 45 and 46: The Table(6.2). The relations of ma
Page 47 and 48: The Table(6.2)(continuation). N Sta
Page 49 and 50: The Table(6.2)(continuation). N Sta
Page 51: log T/T o 1.0 0.9 0.8 0.7 0.6 measu
Page 55 and 56: 54
Page 57 and 58: Simultaneously, the torque of a bal
Page 59 and 60: At taking into account above obtain
Page 61 and 62: 60
Page 63 and 64: of periastron rotation of close bin
Page 65 and 66: 8.3 The angular velocity of the aps
Page 67 and 68: N -3.0 -2.5 -2.0 -1.5 -1.0 -0.5 0.0
Page 69 and 70: Figure 9.1: (a) The power spectrum
Page 71 and 72: Figure 9.2: (a) The measured power
Page 73 and 74: 9.3 The basic elastic oscillation o
Page 75 and 76: 9.5 The spectrum of solar core osci
Page 77 and 78: star mass spectrum. At first, we ca
Page 79 and 80: where ˜ λ C = m ec is the Compto
Page 81 and 82: This energy is many orders of magni
Page 83 and 84: 82
Page 85 and 86: Figure 11.1: The steady states of s
Page 87 and 88: It opens a way to estimate the mass
Page 89 and 90: N 10 9 8 7 6 5 4 3 2 1 0 1.0 1.1 1.
Page 91 and 92: This makes it possible to estimate
Page 93 and 94: to p F ≈ mc, its energy and press
Page 95 and 96: 94
Page 97 and 98: approach to the separation of the E
Page 99 and 100: is evident as soon as in this proce
Page 101 and 102: Figure 12.1: The dependence of the
Page 103 and 104:
Figure 12.2: a) The external radius
Page 105 and 106:
104
Page 107 and 108:
It gives a possibility to conclude
Page 109 and 110:
This allows us to explain the obser
Page 111 and 112:
[14] Landau L.D. and Lifshits E.M.:
Page 113 and 114:
N Name of star U P M 1 /M ⊙ M 2 /
Page 115 and 116:
[9] Gemenez A. and Clausen J.V., Fo
Page 117 and 118:
[30] Hill G. and Holmgern D.E. Stud
Page 119 and 120:
[52] Semeniuk I. Apsidal motion in
Page 121:
[75] Andersen J. and Gimenes A. Abs
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