Numerical integral of resistance coefficients in diffusion

Abstract

The resistance coefficients in screen Coulomb potential of stellar plasma are evaluated in high accuracy. I have analyzed the possible singularities in the integral of scattering angle. There are possible singularities in the case of attractive potential. This may result in problem for numerical integral. In order to avoid the problem, I have used a proper scheme, e.g., splitting into many subintervals and the width of each subinterval is determined by the variation of the integrand, to calculate the scattering angle. The collision integrals are calculated by using Romberg's method therefore the accuracy is high (i.e., $\sim 10^{-12}$). The results of collision integrals and their derivatives in $-12\le \psi \le 5$ are listed. By using Hermite polynomial interpolation from those data, the collision integrals can be obtained with an accuracy of $10^{-10}$. For very weak coupled plasma ($\psi \ge 4.5$), analytical fittings for collision integrals are available with an accuracy of $10^{-11}$. I have compared the final results of resistance coefficients with other works and found that, for repulsive potential, the results are basically same to others, for attractive potential, the results in intermediate and strong coupled case show significant differences. The resulting resistance coefficients are tested in the solar model. Comparing with the widely used Cox et al.(1989) and Thoul et al. (1994) models, the resistance coefficients in screen Coulomb potential leads to a little weaker effect in solar model, which is contrary to the expectation of attempts to solve the solar abundance problem.

19 pages, 6 figures, 9 tables, accepted to ApJ

References in corpus (5)

• Fresh insights on the structure of the solar core
• Solving the discrepancy between the seismic and photospheric solar radius
• Extending plasma transport theory to strong coupling through the concept of an effective interaction potential
• The solar abundance problem: the effect of the turbulent kinetic flux on the solar envelope model
• The YNEV stellar evolution and oscillation code

Cited by in corpus (1)

• Core overshoot constrained by the absence of a solar convective core and some solar-like stars