Neutrino Emissivities as a Probe of the Internal Magnetic Fields of White Dwarfs

TL;DR

This paper investigates how internal magnetic fields in white dwarfs influence neutrino emission processes, affecting their cooling rates and offering a potential method to probe their hidden magnetic interior.

Contribution

It demonstrates that neutrino pair synchrotron radiation significantly impacts white dwarf cooling and that internal magnetic fields can be constrained through neutrino emissivity analysis.

Findings

Magnetic fields in WDs can modify cooling rates via neutrino emission.

Neutrino pair synchrotron radiation is a dominant cooling contribution in magnetic WDs.

Internal magnetic fields are constrained to be less than approximately 6×10^{11} G.

Abstract

The evolution of white dwarfs (WDs) depends crucially on thermal processes. The plasma in their core can produce neutrinos which escape from the star, thus contributing to the energy loss. While in absence of a magnetic field the main cooling mechanism is plasmon decay at high temperature and photon surface emission at low temperature, a large magnetic field in the core hiding beneath the surface even of ordinary WDs, and undetectable to spectropolarimetric measurements, can potentially leave an imprint in the cooling. In this paper, we revisit the contribution to WD cooling stemming from neutrino pair synchrotron radiation and the effects of the magnetic field on plasmon decay. Our key finding is that even if observations limit the magnetic field strength at the stellar surface, magnetic fields in the interior of WDs -- with or without a surface magnetic field -- can be strong enough to modify the cooling rate, with neutrino pair synchrotron emission being the most important contribution. This effect may not only be relevant for the quantification and interpretation of cooling anomalies, but also suggests that the internal magnetic fields of WDs should be smaller than $\sim 6\times 10^{11}\,\rm G$, slightly improving bounds coming from a stability requirement. While our simplified treatment of the WD structure implies that further studies are needed to reduce the systematic uncertainties, the estimates based on comparing the emissivities illustrate the potential of neutrino emission as a diagnostic tool to study the interior of WDs.