- Text
- Plasma,
- Density,
- Electron,
- Equilibrium,
- Binary,
- Radius,
- Stellar,
- Eclipsing,
- Parameters,
- Equation,
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Book Boris V. Vasiliev Astrophysics

Chapter 6 The thermodynamic relations of intra-stellar plasma 6.1 The thermodynamic relation of star atmosphere parameters Hot stars steadily generate energy and radiate it from their surfaces. This is nonequilibrium radiation in relation to a star. But it may be a stationary radiation for a star in steady state. Under this condition, the star substance can be considered as an equilibrium. This condition can be considered as quasi-adiabatic, because the interchange of energy between both subsystems - radiation and substance - is stationary and it does not result in a change of entropy of substance. Therefore at consideration of state of a star atmosphere, one can base it on equilibrium conditions of hot plasma and the ideal gas law for adiabatic condition can be used for it in the first approximation. It is known, that thermodynamics can help to establish correlation between steadystate parameters of a system. Usually, the thermodynamics considers systems at an equilibrium state with constant temperature, constant particle density and constant pressure over all system. The characteristic feature of the considered system is the existence of equilibrium at the absence of a constant temperature and particle density over atmosphere of a star. To solve this problem, one can introduce averaged pressure ̂P ≈ GM2 , (6.1) R 4 0 39

averaged temperature and averaged particle density ∫ V ̂T = T dV V ∼ T 0 ( R0 R ⋆ ) (6.2) ̂n ≈ NA (6.3) R 3 0 After it by means of thermodynamical methods, one can find relation between parameters of a star. 6.1.1 The c P /c V ratio At a movement of particles according to the theorem of the equidistribution, the energy kT/2 falls at each degree of freedom. It gives the heat capacity c v = 3/2k. According to the virial theorem [12, 22], the full energy of a star should be equal to its kinetic energy (with opposite sign)(Eq.(5.3)), so as full energy related to one particle E = − 3 kT (6.4) 2 In this case the heat capacity at constant volume (per particle over Boltzman’s constant k) by definition is ( ) dE c V = = − 3 (6.5) dT V 2 The negative heat capacity of stellar substance is not surprising. It is a known fact and it is discussed in Landau-Lifshitz course [12]. The own heat capacity of each particle of star substance is positive. One obtains the negative heat capacity at taking into account the gravitational interaction between particles. By definition the heat capacity of an ideal gas particle at permanent pressure [12] is where W is enthalpy of a gas. As for the ideal gas [12] c P = ( dW dT ) , (6.6) P W − E = NkT, (6.7) and the difference between c P and c V c P − c V = 1. (6.8) Thus in the case considered, we have c P = − 1 2 . (6.9) Supposing that conditions are close to adiabatic ones, we can use the equation of the Poisson’s adiabat. 40

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This makes it possible to estimate

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to p F ≈ mc, its energy and press

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approach to the separation of the E

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is evident as soon as in this proce

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Figure 12.1: The dependence of the

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Figure 12.2: a) The external radius

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It gives a possibility to conclude

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This allows us to explain the obser

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[14] Landau L.D. and Lifshits E.M.:

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N Name of star U P M 1 /M ⊙ M 2 /

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[9] Gemenez A. and Clausen J.V., Fo

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[30] Hill G. and Holmgern D.E. Stud

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[52] Semeniuk I. Apsidal motion in

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[75] Andersen J. and Gimenes A. Abs