Molecular dynamics and virial expansions for equilibrium thermodynamics in the solar interior

Details Molecular dynamics and virial expansions for equilibrium thermodynamics in the solar interior Molecular dynamics and virial expansions for equilibrium thermodynamics in the solar interior

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007phdt........19m&link_type=abstract

Proquest Dissertations And Theses 2007. Section 0208, Part 0606 133 pages; [Ph.D. dissertation].United States -- California: Un

Physics

1

Molecular Dynamics, Solar Model, Virial Expansions, Screening, Equation Of State, Hot, Dense Plasma, Equilibrium Thermodynamics, Solar Interior

Scientific paper

n the deep solar interior, matter is mostly fully ionized. Precise helioseismic and neutrino data provide an incredibly accurate description of the Sun. The established MHD and OPAL equations of state do not match the solar data to the available precision. A rigorous quantum-statistical formalism for Coulomb systems is used to develop new tools for equation of state modeling. Although the formalism is in principle a low-density development, the relevant parameters allow the formalism to be applied in the solar center. Solar models can also be improved through the study of nuclear reaction rates. The Coulomb potentials in the ionized plasma are screened, effectively truncating the interactions. This screening makes it easier for ions to tunnel through the potential barrier. In a seminal paper, Salpeter (1954) discussed this enhancement. He based his study on the approximation of a static screening potential. There is a legitimate concern that dynamic effects could alter the result. Since 1996, Shaviv and Shaviv have been examining this question by numerical molecular-dynamics simulations. The calculation is essentially classical, although electrons are treated with effective potentials to mimic some quantum corrections. Shaviv and Shaviv have reported dynamical effects for the fast protons which are the ions that are most likely to engage in nuclear reactions. Given the importance of these effects for solar and stellar modeling, molecular-dynamics simulations have been developed to verify the results of Shaviv and Shaviv in an independent calculation. These studies of hot, dense plasmas will help develop more accurate solar models.

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