On a transition from solar-like coronae to rotation-dominated jovian-like magnetospheres in ultracool main-sequence stars

TL;DR

This paper explores the transition in magnetic and atmospheric properties of ultracool main-sequence stars, suggesting a shift from solar-like coronae to Jupiter-like magnetospheres as stars cool beyond spectral type M5.

Contribution

It proposes a transition in stellar atmospheres from solar-like to jovian-like magnetospheres in ultracool stars, supported by a scaling relationship and observational evidence.

Findings

Stars cooler than M5 have more dipolar magnetic fields.

Chromospheric and coronal emissions weaken significantly in ultracool stars.

Radio emissions persist, likely dominated by electron-cyclotron maser processes.

Abstract

For main-sequence stars beyond spectral type M5 the characteristics of magnetic activity common to warmer solar-like stars change into the brown-dwarf domain: the surface magnetic field becomes more dipolar and the evolution of the field patterns slows, the photospheric plasma is increasingly neutral and decoupled from the magnetic field, chromospheric and coronal emissions weaken markedly, and the efficiency of rotational braking rapidly decreases. Yet, radio emission persists, and has been argued to be dominated by electron-cyclotron maser emission instead of the gyrosynchrotron emission from warmer stars. These properties may signal a transition in the stellar extended atmosphere. Stars warmer than about M5 have a solar-like corona and wind-sustained heliosphere in which the atmospheric activity is powered by convective motions that move the magnetic field. Stars cooler than early-L, in contrast, may have a jovian-like rotation-dominated magnetosphere powered by the star's rotation in a scaled-up analog of the magnetospheres of Jupiter and Saturn. A dimensional scaling relationship for rotation-dominated magnetospheres by Fan et al. (1982) is consistent with this hypothesis.