VbvAstE-001

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while the radius of the star will R ≈ 10 −2 R odot . (11.11) Easy to see that the density of matter and the radius are characteristic of cosmic bodies, called dwarfs. The neutron matter. Pulsars. Dwarfs may be considered as stars where a process of neutronization is just beginning. At a nuclear density, plasma turns into neutron matter. 1 At taking into account the above assumptions, the stars composed of neutron matter, must also have the same equilibrium condition Eq.((11.9)). As the density of neutron matter: ( n n = p3 F 3π 2 = ξ3 mnc ) 3 (11.12) 3 3π 2 (where m n - the neutron mass), then the condition ((11.9)) allows to determine the equilibrium density of matter within a neutron star n n = n n ≈ 4 · 10 39 (11.13) particles in cm 3 . The substitution of the values of the neutron density in the equilibrium condition Eq.(5.2) shows that, in accordance with our assessment of all the neutron stars in the steady state should have a mass of order of magnitude equal to the mass of the Sun. The measured mass distribution of pulsar composing binary stars [21] is shown on Fig.11.2. It can be considered as a confirmation of the last conclusion. 11.2.4 The hot relativistic plasma.Quasars Plasma is hot if its temperature is higher than degeneration temperature of its electron gas. The ratio of plasma temperature in the core of a star to the temperature of degradation of its electron gas for case of non-relativistic hot star plasma is (Eq.(2.23)) T ⋆ ≈ 40 (11.14) T F (n ⋆) it can be supposed that the same ratio must be characteristic for the case of a relativistic hot star. At this temperature, the radiation pressure plays a main role and accordingly the equation of the pressure balance takes the form: GM 2 6RV ( ) ≈ π2 (kT ⋆) 4 3 T⋆ ≈ kT n (11.15) 45 (c) 3 T F 1 At nuclear density neutrons and protons are indistinguishable inside pulsars as inside a huge nucleus. It permits to suppose a possibility of gravity induced electric polarization in this matter. 87
N 10 9 8 7 6 5 4 3 2 1 0 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 M pulsar /M o Figure 11.2: The mass distribution of pulsars from binary systems [21].On abscissa the logarithm of pulsar mass in solar mass is shown. 88
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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
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: It opens a way to estimate the mass
Page 91 and 92: This makes it possible to estimate
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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