Magnetic field evolution of white dwarfs in strongly interacting binary star systems

TL;DR

This paper investigates the generation and evolution of magnetic fields in white dwarfs within strongly interacting binary systems, focusing on dynamo mechanisms during the common envelope phase and their dependence on various physical parameters.

Contribution

It provides a detailed analysis of how dynamo action during the common envelope phase can produce residual magnetic fields in white dwarfs, highlighting conditions for sustained magnetic fields.

Findings

Residual magnetic fields are typically very weak (<10^-8 of external field) after common envelope dispersal.

A preferential dynamo orientation can produce more persistent magnetic fields lasting a few million years.

The residual field strength is proportional to the duration of dynamo activity during the common envelope phase.

Abstract

The surface magnetic field strength of white dwarfs is observed to vary from very little to around 10^9 G. Here we examine the proposal that the strongest fields are generated by dynamo action during the common envelope phase of strongly interacting stars that leads to binary systems containing at least one white dwarf. The resulting magnetic field depends strongly on the electrical conductivity of the white dwarf, the lifetime of the convective envelope and the variability of the magnetic dynamo. We assess the various energy sources available and estimate necessary lifetimes of the common envelope. In the case of a dynamo that leads a randomly oriented magnetic field we find that the induced field is confined to a thin boundary layer at the surface of the white dwarf. This then decays away rapidly upon dispersal of the common envelope. The residual field is typically less than 10^-8 times the strength of the external field. Only in the case where there is some preferential direction to the dynamo-generated field can an induced field, that avoids rapid decay, be produced. We show that a surface field of magnitude a few per cent of the external field may be produced after a few Myr. In this case the residual field strength is roughly proportional to the lifetime of the dynamo activity.