By Barus C.

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**Example text**

24 Assume the nucleus consist5 of two ideal, nonrelativistic Fermi gases, one of Z protons and the other of N = A Z neutrons. Show that the energy of the nuclcus (excluding rest energy) IS ~ Here E;. (thc Fermi energy excluding rest energy) is defined by putting A nucleons in a volume V with four nucleons per momentum state. Determine E;. from the measured density of nuclei. 72 x 10’Hparticles/cm’. By considering deviations from the case N = Z (minimum of E ) , derive the symmetry term and show that about 4 the value of h4 comes from this simple Pauli Principle picture.

21 Verify Eqs. 19). -equilibrium, and extreme relativistic degeneracy. 2). Show that p $ is greater than this value for all densities above that determined by Eq. 12), thus verifying that the equilibrium is stable. The results of this section are not, strictly speaking, applicable to the case of gravitational collapse with escaping neutrinos, even when the collapse occurs quasistatically and at zero temperature. Thermodynamic equilibrium is not achieved in an open system, and the n-p-e composition must be determined by solving appropriate rate equations for the various reactions.

34) solves Eq. 27) but not Eq. 28). 3. The consequences of this result for low-mass white dwarf structure will be discussed in Chapter 3. 15) as one might expect (cf. 18). A more complete treatment of corrections to the equation of state in the regime explored in this section is given by Salpeter (1961) and Salpeter and Zapolsky (1967). For most applications, the results of Feynmann, Metropolis, and Teller for the Thomas-Fermi-Dirac model are adequate for the low-density ~ . 1 1). 37) 9Zel’dovich and Novikov (1971) give a simple but heuristic derivation of the exponent 10/3 appearing in Eq.

### An Adjustment in Relation to the Fresnel Coefficient(en)(6s) by Barus C.

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