VbvAstE-001

More documents

Recommendations

Info

45 µ/L=G 1/2 /c Log µ 35 25 Mercury Titan Io Venus Pluto Neptun Mars Earth Uranus 78 Vir Jupiter Saturn Sun Psr 0531+21 Psr Her X-1 Psr 4U0115+13 15 30 40 50 60 Log L Figure 7.1: The observed values of magnetic moments of celestial bodies vs. their angular momenta [18]. In ordinate, the logarithm of the magnetic moment (in Gs · cm 3 ) is plotted; in abscissa the logarithm of the angular momentum (in erg · s) is shown. The solid line illustrates Eq.(13.2). The dash-dotted line fits of observed values. 57
At taking into account above obtained relations, one can see that this field is weakly depending on Z and A/Z, i.e. on the star temperature, on the star radius and mass. It depends linearly on the velocity of star rotation only: ( ) 3/2 me α 3/4 c H ≈ −50 √ Ω ≈ −2 · 10 9 Ω Oe. (7.11) m p G The magnetic fields are measured for stars of Ap-class [16]. These stars are characterized by changing their brightness in time. The periods of these changes are measured too. At present there is no full understanding of causes of these visible changes of the luminosity. If these luminosity changes caused by some internal reasons will occur not uniformly on a star surface, one can conclude that the measured period of the luminosity change can depend on star rotation. It is possible to think that at relatively rapid rotation of a star, the period of a visible change of the luminosity can be determined by this rotation in general. To check this suggestion, we can compare the calculated dependence (Eq.7.11) with measuring data [16] (see Fig. 7.2). Evidently one must not expect very good coincidence of calculations and measuring data, because calculations were made for the case of a spherically symmetric model and measuring data are obtained for stars where this symmetry is obviously violated. So getting consent on order of the value can be considered as wholly satisfied. It should be said that Eq.(7.11) does not working well in case with the Sun. The Sun surface rotates with period T ≈ 25 ÷ 30 days. At this velocity of rotation, the magnetic field on the Sun pole calculated accordingly to Eq.(7.11) must be about 1 kOe. The dipole field of Sun according to experts estimation is approximately 20 times lower. There can be several reasons for that. 58
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 and 34: we obtain η = 20 = 6.67, (5.24) 3
Page 35 and 36: 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: Simultaneously, the torque of a bal
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
show all

VbvAstE-001

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?