Ionization in Atmospheres of Brown Dwarfs and Extrasolar Planets V: Alfv\'{e}n Ionization

TL;DR

This paper proposes Alfvén ionization as an efficient mechanism to produce localized plasmas in the atmospheres of low-mass objects like brown dwarfs and exoplanets, explaining observed radio and X-ray emissions.

Contribution

It demonstrates the applicability of Alfvén ionization in low-mass object atmospheres and predicts resulting observable plasma signatures, expanding understanding of atmospheric ionization processes.

Findings

Alfvén ionization can achieve ionization levels of 10^{-6} to 1 in atmospheres.

Most efficient at mid to low pressures where seed plasma is magnetized.

Observable signatures include Bremsstrahlung and spectral lines from plasma ions.

Abstract

Observations of continuous radio and sporadic X-ray emission from low-mass objects suggest they harbour localized plasmas in their atmospheric environments. For low-mass objects, the degree of thermal ionization is insufficient to qualify the ionized component as a plasma, posing the question: what ionization processes can efficiently produce the required plasma that is the source of the radiation? We propose Alfv\'{e}n ionization as a mechanism for producing localized pockets of ionized gas in the atmosphere, having sufficient degrees of ionization ($\geq10^{-7}$) that they constitute plasmas. We outline the criteria required for Alfv\'{e}n ionization and demonstrate it's applicability in the atmospheres of low-mass objects such as giant gas planets, brown dwarfs and M-dwarfs for both solar and sub-solar metallicities. We find that Alfv\'{e}n ionization is most efficient at mid to low atmospheric pressures where a seed plasma is easier to magnetize and the pressure gradients needed to drive the required neutral flows are the smallest. For the model atmospheres considered, our results show that degrees of ionization of $10^{-6}-1$ can be obtained as a result of Alfv\'{e}n ionization. Observable consequences include continuum Bremsstrahlung emission, superimposed with spectral lines from the plasma ion species (e.g. He, Mg, H$_{2}$ or CO lines). Forbidden lines are also expected from the metastable population. The presence of an atmospheric plasma opens the door to a multitude of plasma and chemical processes not yet considered in current atmospheric models. The occurrence of Alfv\'{e}n ionization may also be applicable to other astrophysical environments such as protoplanetary disks.