4 months ago


Book Boris V. Vasiliev Astrophysics

It can be found for the

It can be found for the known density distribution inside a planet γ(r). Furthermore, accounting to the thermodynamic equation for chemical potential dχ = m′ dp (12.17) γ (where m ′ is the ion mass) from the equation of state Eq.(12.4), the chemical potential is ( ) χ = αm ′ (k + 1)γ 1/k − γ1/k − k 2 γ (12.18) 1 − k and the density of the internal energy of the core is ε in = χγ ( 3 m − p = ′ αn 2 γ5/3 n + 3γn 2/3 − 9 ) 2 γn . (12.19) Doing analogous calculations for the mantle, we obtain ε im = α m ( γ 2 m (r) γ 2 0 + γm(r) γ 0 − γm(r) ln γm(r) ) − 2 γ 0 γ 0 The electric energy exists only inside the core and its density is . (12.20) E 2 (r) 8π = 2π 9 Gγ2 nr 2 . (12.21) Since the thermal energy is neglected, to calculate the full energy of the planet, it is necessary to integrate Eqs.(12.19), (12.20), and (12.22) over the volume of the planet and sum them and Eq.(12.16). To do this, we need to determine the values of constants composing these equations. 12.5 The density distribution inside the Earth The mass M and radius R of the Earth are known. Therefore, we know the average density of the Earth < γ > ∼ = 5.5g/cm 3 . On the basis of the geophysical data, we accept that the density of matter and bulk module on the surface of the mantle is γ 0 ∼ = 3.2g/cm 3 and B = 1.3 · 10 12 dyn/cm 2 . These values are characteristic for basalts [24]. Based on the above said we determine R 0 and the parameter α m. We can found the value of the parameter α m as we know the values of γ 0 and < γ > and therefore we can find the ratio ( ) 1/3 R γ0 = = 0.835. (12.22) R 0 < γ > Next from all possible solutions we choose the one that actually meets the condition (12.22). In fact this procedure is reduced to choosing the parameter m ′ , i.e. the ion mass related to each free electron in electron-ion plasma of the core. The total energy (related to GM/R 0) is plotted as a function of the parameter m ′ in fig.(12.1). 99

Figure 12.1: The dependence of the total energy of the planet (over GM 2 R 0 ) on the size of the polarized core composed of some metal with different averaged ion mass m ′ per one conductivity electron. 100

• Spectral line broadening i t h i l l i t h i l l in astrophysical plasmas
Nuclear Astrophysics
Astrophysical consequences of color superconductivity - Infn
Parametric Instabilities in Plasmas. - Applications of Electronics in ...
Probabilistic combination of stellar astrophysical parameter ...
Astronomy Astrophysics - Uppsala Astronomical Observatory
V. Parkhomchuk, BINP Novosibirsk - BETACOOL home page
Computational Astrophysics: N-Body Exercise
Non-neutral plasma equilibria with weak axisymmetric magnetic ...
nonlinear processes in field theory and astrophysics -
the eclipsing binary v1061 cygni: confronting stellar evolution ...
Binary systems and fundamental stellar parameters
Instabilities and pattern formation in low-temperature plasmas
ASTROPHYSICS 3; SEMESTER 1 TUTORIAL 3: Nuclear Fusion and ...
2. astrophysical constants and parameters - Particle Data Group
Quantum Phenomena in the Realm of Cosmology and Astrophysics
Astrophysics Dynamics of electron beams in the solar corona ...
2. astrophysical constants and parameters - Particle Data Group