VbvAstE-001

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N 10 9 8 7 6 5 4 3 2 1 0 6 7 8 9 10 11 12 13 14 log M/Mo Figure 11.3: The mass distribution of galaxies. [4]. On the abscissa, the logarithm of the galaxy mass over the Sun mass is shown. 89
This makes it possible to estimate the mass of a hot relativistic star M ≈ ( ) 6 ( ) 3/2 T⋆ c m T F Gm 2 p ≈ 10 9 M ⊙ (11.16) p According to the existing knowledge, among compact celestial objects only quasars have masses of this level. Apparently it is an agreed-upon opinion that quasars represent some relatively short stage of evolution of galaxies. If we adhere to this hypothesis, the lack of information about quasar mass distribution can be replaced by the distribution of masses of galaxies [4](Fig.11.3). It can be seen, that this distribution is in a qualitative agreement with supposition that quasars are composed from the relativistic hot plasma. Certainly the used estimation Eq.(11.14) is very arbitrary. It is possible to expect the existing of quasars which can have substantially lesser masses. As the steady-state particle density of relativistic matter n r is known (Eq.(11.10)), one can estimate the quasar radius: √ M R qu ≈ 3 qu ≈ 10 12 cm. (11.17) n rm p It is in agreement with the astronomer measuring data obtained from periods of the their luminosity changing. 11.2.5 About the cosmic object categorizations Thus, it seems possible under some assumptions to find characteristic parameters of different classes of stars, if to proceed from EOS of atomic, plasma and neutron substances. The EOS types can be compared with classes of celestial bodies. As any other EOS are unknown, it gives a reason to think that all classes of celestial bodies are discovered (Fig.11.4). 11.3 Several words about star evolution There are not formulas in this section, which could serve as a handhold for suggestions. The formulas of the previous sections can not help too in understanding that, as the evolution of the stars can proceed and as their transitions them from the one class to another are realized, since these formulas were received for the description of the star steady-state. There the comparison of the schemes to the substance categorization (Fig.(11.1)) and the categorization of star classes (Fig.(11.4)) can serve as the base of next suggestions. At analyzing of these schemes, one can suppose that the evolution of stellar objects is going at the reduction of their temperature. In light of it, it is possible to suppose the existing of one more body, from which the development began. Really, neutron matter at nuclear density (Eq.(11.13)) is not ultra-relativistic. At this density, corresponding 90
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Boris V.Vasiliev ASTROPHYSICS and a
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5 The main parameters of star 29 5.
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theories of stars that are not purs
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But plasma is an electrically polar
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can be described by definite ration
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But even at so high temperatures, a
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2.2 The energy-preferable state of
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20
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3.2 The equilibrium of a nucleus in
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24
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As a result, the electric force app
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and in accordance with Eq.(4.11), t
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The total kinetic energy of plasma
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we obtain η = 20 = 6.67, (5.24) 3
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40 N 35 30 10 9 8 7 6 5 4 3 2 1 A/Z
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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: N 10 9 8 7 6 5 4 3 2 1 0 1.0 1.1 1.
Page 93 and 94: to p F ≈ mc, its energy and press
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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
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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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