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016 Fig. 10 Comparison of the activity expansion method (curve labeled OPAL) with the shock wave experiments of Erskin, Rosznyai, and Ross (1994). To demonstrate the importance of Coulomb interations, the simple Saha equation is also shown. 7 Equation of State Comparisons The EOS properties frequently needed in stellar modeling are the first order thermodynamic quantities and the following second order quantities (Cox and Guili 1968) XT = {dinp)T (37) 36 Rogers: Stellar plasmas (38) (39) Comparisons of the several EOS methods described above have been carried out by Da'ppen (1992).

Ap. , and Van Horn, H. , Ap. , J. Stat. , Ap. , Quantum Statistics of Charged Particle Systems (Plenum Press: New York), (1986) Van Horn: Stellar structure and evolution 15 Kurilenkov, Yu. , and Van Horn, H. , these proceedings Lee, U. , Strohmayer, T. , and Van Horn, H. , Ap. , P. A. S. , and Salpeter, E. , Ap. J. , Rev. Mexicana Astron. , Dahn, C. C , and Monet, D. , Ap. , 332, 891, (1988) Magalhaes, J. , Weir, A. , Conrath, B. , Gierasch, P. , and Leroy, S. , Nature, 337, 444, (1989) Magalhaes, J.

In a recent paper Dziembowski, Pamyatnykh, and Sienkiewicz (1992) used helioseismological data to test the MHD equation of state. 95. We have used the activity expansion method (Section 7) to study two points in this region (Rogers and Iglesias 1993). 0259 g/cm3. We were able to draw several conclusions (see Figure 1 of Rogers and Iglesias 1993). 4 Fig. 11 Comparison of %p on an isochore with p=10*5-5. Part a compares the EFF and MHD equations of state; solid line EFF and the dashed line MHD. The mixture is 90% H and 10% He by number abundance.

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Ahmad Khan Kharal: A Punjabi Hero of 1857 by Saeed Bhutta


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