Astrophysical and laboratory plasmas: HF properties under extreme conditions

TL;DR

This paper investigates the high-frequency electromagnetic properties of dense astrophysical plasmas under extreme conditions, providing numerical conductivity data relevant for understanding stellar magnetic fields and evolution.

Contribution

It introduces a numerical method to determine HF characteristics of dense plasmas in extreme environments, applicable to various stellar objects and conditions.

Findings

Calculated plasma conductivity values across IR, visible, and UV frequencies.

Method applicable to white dwarfs, red dwarfs, and the Sun.

Provides insights into magnetic field effects on stellar plasma behavior.

Abstract

The values of electrical conductivity of plasma of stars with a magnetic field or moving in the magnetic field of the other component in a binary system could be of significant interest, since they are useful for the study of thermal evolution of such objects, cooling, nuclear burning of accreted matter, and the investigation of their magnetic fields. So, on the basis of numerically calculated values for the dense plasma conductivity in an external HF electric field, we determine the HF characteristics of astrophysical plasmas under extreme conditions. The examined range of frequencies covers the IR, visible and near UV regions and consider electronic number density and temperature are in the ranges of $10^{21} \textrm{cm}^{-3} \le Ne$ and 20 000 $\le T$, respectively. The method developed here represents a powerful tool for research into white dwarfs with different atmospheric compositions (DA, DC etc.), and for investigation of some other stars (M-type red dwarfs, Sun etc.).