Radiative transfer dynamo effect

TL;DR

This paper explores how radiative interactions in rotating, radiating plasma can generate magnetic fields, revealing that including kinetic effects significantly enhances predictions of magnetic field strength.

Contribution

It introduces the importance of kinetic effects in modeling the radiative transfer dynamo effect, which were previously neglected in theoretical predictions.

Findings

Kinetic effects substantially increase predicted magnetic field strengths.

Radiative interactions can produce magnetic fields in astrophysical plasma.

The dynamo effect efficiency varies with plasma conditions.

Abstract

Magnetic fields in rotating and radiating astrophysical plasma can be produced due to a radiative interaction between plasma layers moving relative to each other. The efficiency of current drive, and with it the associated dynamo effect, is considered in a number of limits. It is shown here, however, that predictions for these generated magnetic fields can be significantly higher when kinetic effects, previously neglected, are taken into account.