Coulomb corrections to the equation of state of nuclear statistical equilibrium matter: implications for SNIa nucleosynthesis and the accretion-induced collapse of white dwarfs

Details Coulomb corrections to the equation of state of nuclear statistical equilibrium matter: implications for SNIa nucleosynthesis and the accretion-induced collapse of white dwarfs Coulomb corrections to the equation of state of nuclear statistical equilibrium matter: implications for SNIa nucleosynthesis and the accretion-induced collapse of white dwarfs

Aug 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999mnras.307..984b&link_type=abstract

Monthly Notices, Volume 307, Issue 4, pp. 984-992.

Physics

37

Scientific paper

Coulomb corrections to the equation of state of degenerate matter are usually neglected in high-temperature regimes, owing to the inverse dependence of the plasma coupling constant, Gamma, on temperature. However, nuclear statistical equilibrium matter is characterized by a large abundance by mass of large-Z (iron group) nuclei. It is found that Coulomb corrections to the ion ideal gas equation of state of matter in nuclear statistical equilibrium are important at temperatures T<~5-10x10^9K and densities rho>~10^8gcm^-3. At a temperature T=8.5x10^9K and a density rho=8x10^9gcm^-3, the neutronization rate is larger by >~28per cent when Coulomb corrections are included. However, the conductive velocity of a thermonuclear deflagration wave in C-O drops by ~16per cent when Coulomb corrections to the heat capacity are taken into account. The implications for SNIa models and nucleosynthesis, and also for the accretion-induced collapse of white dwarfs, are discussed. Particularly relevant is the result that the minimum density for collapse of a white dwarf to a neutron star is shifted down to 5.5-6x10^9gcm^-3, a value substantially lower than previously thought.

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