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Bibliography [1] Khaliulilin Kh.F. and Kozyreva V.S. Apsidal motion in the eclipsing binary system of BW Aqr Astrophys. and Space Sci., 120 (1986) 9-16. [2] Imbert M. Photoelectric radial velosities of eclipsing binaries. IV. Orbital elements of BW Aqr, Astron.Astrophys.Suppl., 69 (1987) 397-401. [3] Khaliulilin Kh.F. and Khaliulilina A.I. Fotometricheskoe issledovanie zatmenno-dvoinoi sistemy s relativistskim vrasheniem orbity V889 Aql, Astronom.zh.,66(1989)76-83 (in Russian). [4] Khaliulilin Kh.F. and Khaliulilina A.I. K probleme vrashenia linii apsid v zatmennoi sisteme V889 Aql, Astron.cirk., N1486 (1987) 5-7 (in Russian). [5] Clausen J.V. V 539 Arae: first accurate dimensions of eclipsing binaries, Astron.Astrophys., 308 (1996) 151-169. [6] Lavrov M.I. and Lavrova N.V. Revisia elementov fotometricheskoi orbity EK Cep, Astron.cirk. 971 (1977) 3-4 (in Russian). [7] Khaliulilin Kh.F. and Kozyreva V.S. Apsidal motion in the eclipsing binary AS Cam, Astrophys. and Space Sci., 120 (1994) 115-122. [8] Andersen J. and Clausen J.V., Absolute dimensions of eclipsing binaries.XV. EM Cainae, Astron.Astrophys. 213 (1989) 183-194. 113
[9] Gemenez A. and Clausen J.V., Four-color photometry of eclipsing binaries. XXIIA. Photometric elements and apsidal motion of GL Cainae, Astron.Astrophys. 161 (1986) 275-286. [10] Andersen J., Clausen J.V., Nordstrom B. and Reipurth B., Absolute dimensions of eclipsing binaries.I. The early-type detached system QX Cainae, Astron.Astrophys. 121 (1983) 271-280. [11] Gemenez A., Clausen J.V. and Jensen K.S. Four-color photometry of eclipsing binaries. XXIV. Aspidal motion of QX Cainae, ξ Phoenicis and NO Puppis, Astron.Astrophys. 159 (1986) 157-165. [12] De Greve J.P. Evolutionary models for detached close binaries: the system Arae and QX Cainae, Astron.Astrophys. 213 (1989) 195-203. [13] Malony F.P., Guinan E.F. and Mukherjec J. Eclipsing binary star as test of gravity theories Astron.J. 102 (1991) 256-261. [14] Mossakovskaya L.V. New photometric elements of AR Cas, an eclipsing binary system with apsidal motion Astron. and Astroph. Trans. 2 (1992) 163-167. [15] Haffer C.M. and Collins G.M. Computation of elements of eclipsing binary stars by high-speed computing machines Astroph.J.Suppl., 7 (1962) 351-410. [16] Crinklaw G. and Etzel P. A photometric analisis of the eclipsing binary OX Cassiopeiae Astron.J. 98 (1989) 1418-1426. [17] Claret A. and Gimenez A. The aspidal motion test of the internal stellar structure: comparision between theory and observations Astron.Astroph. 277 (1993) 487-502. [18] Wolf M. Aspidal motion in the eclipsing binary PV Cassiopeiae Monthly Not.Roy.Soc. 286 (1995) 875-878. 114
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Boris V.Vasiliev ASTROPHYSICS and a
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4
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5 The main parameters of star 29 5.
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8
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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
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2.10 log (TR/R o T o ) 1.55 1.00 me
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averaged temperature and averaged p
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log R/R o 1.5 1.3 1.1 0.9 measured
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The Table(6.2). The relations of ma
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The Table(6.2)(continuation). N Sta
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The Table(6.2)(continuation). N Sta
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log T/T o 1.0 0.9 0.8 0.7 0.6 measu
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Figure 6.4: The schematic of the st
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54
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Simultaneously, the torque of a bal
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At taking into account above obtain
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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
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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
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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: N Name of star U P M 1 /M ⊙ M 2 /
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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