VbvAstE-001

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[19] Popper D.M. Rediscussion of eclipsing binaries.XVII.The detached early A type binaries PV Cassiopeae and WX Cephei Astron.J. 93 (1987) 672-677. [20] Lavrov M.I. and Lavrova N.V. Revisia fotometrichestih elementov u zatmennyh dvoinyh sistem s ekscentricheskimi orbitami.2.KT Cen Trudy Kaz.Gor.AO 49 (1985) 18-24 (in Russian). [21] Soderhjelm S. Observations of six southern eclipsing binaries for apsidal motion Astron.Astroph.Suppl.Ser 22 (1975) 263-283. [22] Gemenez A., Clausen J.V. and Anderson J. Four-color photometry of eclipsing binaries. XXIA. Photometric analysis and aspidal motion study of V346 Centauri, Astron.Astrophys. 160 (1986) 310-320. [23] Gemenez A., Chun-Hwey Kim and Il-Seong Nha Aspidal motion in the early-type eclipsing binaries CW Cephei, Y Cyg and AG Per Montly .Not.Roy.Astron.Soc. 224 (1987) 543-555. [24] Bocula R.A. Peresmotr elementov fotometricheskoi orbity zatmennyh sistem CW Cep, V 539 Ara, AG Per, AR Aur, RS Cha, ZZ Boo. Peremennye zvezdy21 (1983) 851-859 (in Russian). [25] Khaliulilin Kh.F. Relativistskoe vrashenie orbity zatmennoi dvoinoi sistemy EK Cep Astron.zh.60 (1983) 72-82 (in Russian). [26] Tomkin J. Secondaries of eclipsing binary. V. EK Cephei Astroph.J. 271 (1983) 717-724. [27] Claret A., Gemenez A. and Martin E.L. A test case of stellar evolution the eclipsing binary EK Cephei Astron.Astroph. 302 (1995) 741-744. [28] Volkov I.M. The discovery of apsidal motion in the eclipsing binary system α Cr B Inf.Bull.Var.Stars N3876,(1993) 1-2. [29] Quiroga R.J., van L.P.R. Angular momenta in binary systems Astroph.Space Sci. 146 (1988) 99-137. 115
[30] Hill G. and Holmgern D.E. Studies of early-type varieble stars Asrton.Astroph.297 (1995) 127-134. [31] Hill G. and Batten A.H. Studies of early-type varieble stars.III. The orbit and physical dimensions for V 380 Cygni Asrton.Astroph.141 (1984) 39-48. [32] Zakirov M.M. Ob apsidalnom dvizhenii v dvoinoi sisteme V 453 Cyg Astron.cirk.N1537,21 (in Russian). [33] Karetnikov V.G. Spectral investigation of eclipsing binary stars at the stage of mass exchange Publ.Astron.Inst.Czech.70 (1987) 273-276. [34] Mossakovskaya L.V. and Khaliulilin Kh.F. Prichina anomalnogo apsidalnogo dvizhenia v sisteme V 477 Cyg Astron.cirk.N1536, 23-24 (in Russian). [35] Gemenez A. and Quintana J.M. Apsidal motion and revised photometry elements of the eccentric eclipsing binary V 477 Cyg Astron.Astrophys. 260 (1992) 227-236. [36] Mossakovskaya L.V. and Khaliulilin Kh.F. Vrashenie linii apsid v sisteme V 478 Cyg Pisma v Astron.zh.22 (1996) 149-152. [37] Popper D.M. and Hill G. Rediscussion of eclipsing binaries.XVII.Spectroscopic orbit of OB system with a cross-correlation procedure Astron.J. 101 (1991) 600-615. [38] Khaliulilin Kh.F. The unique eclipsing binary system V 541 Cygni with relativistic apsidal motion Astrophys.J. 229 (1985) 668-673. [39] Lines R.D.,Lines H., Guinan E.F. and Carroll Time of minimum determination of eclipsing binary V 541 Cygni Inf.Bull.Var.Stars N3286,1-3. [40] Khaliulilin Kh.F. Vrashenie linii apsid v zatmennoi sisteme V 1143 Cyg Asrton. cirk.N1262,1-3 (in Russian). 116
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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
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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
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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
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: [9] Gemenez A. and Clausen J.V., Fo
Page 119 and 120: [52] Semeniuk I. Apsidal motion in
Page 121: [75] Andersen J. and Gimenes A. Abs
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