VbvAstE-001

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40 N 35 30 10 9 8 7 6 5 4 3 2 1 A/Z 1.5 25 20 15 10 5 0 -2.0 -1.5 -1.0 -0.5 0.0 0.5 1.0 1.5 2.0 log M/Mo. Figure 5.1: The mass distribution of binary stars [10]. On abscissa, the logarithm of the star mass over the Sun mass is shown. Solid lines mark masses, which agree with selected values of A/Z from Eq.(5.26). 33
40 N 35 30 10 9 8 7 6 5 4 3 2 1 A/Z 1.5 25 20 15 10 5 0 -2.0 -1.5 -1.0 -0.5 0.0 0.5 1.0 1.5 2.0 binary stars close binary stars log M/Mo. Figure 5.2: The mass distribution of close binary stars [11]. On abscissa, the logarithm of the star mass over the Sun mass is shown. Solid lines mark masses, which agree with selected values of A/Z from Eq.(5.26). The binary star spectrum is shown for comparison. 34
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: we obtain η = 20 = 6.67, (5.24) 3
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 and 52: log T/T o 1.0 0.9 0.8 0.7 0.6 measu
Page 53 and 54: Figure 6.4: The schematic of the st
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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