Stellar wind-magnetosphere interaction at exoplanets: computations of auroral radio powers

TL;DR

This paper models auroral radio emissions from exoplanets with Earth-like magnetospheres, considering magnetic interactions, saturation effects, and different stellar ages, to predict radio power outputs relevant for detection.

Contribution

It provides detailed calculations of exoplanetary auroral radio powers incorporating magnetospheric saturation and compares these with existing empirical laws, offering improved predictions for various planetary and stellar conditions.

Findings

Radio power increases with magnetic field strength for saturated magnetospheres.

Radio power decreases with increasing orbital distance.

Hot Jupiters' radio emissions are overestimated by the Radiometric Bode's Law.

Abstract

We present calculations of the auroral radio powers expected from exoplanets with magnetospheres driven by an Earth-like magnetospheric interaction with the solar wind. Specifically, we compute the twin cell-vortical ionospheric flows, currents, and resulting radio powers resulting from a Dungey cycle process driven by dayside and nightside magnetic reconnection, as a function of planetary orbital distance and magnetic field strength. We include saturation of the magnetospheric convection, as observed at the terrestrial magnetosphere, and we present power law approximations for the convection potentials, radio powers and spectral flux densities. We specifically consider a solar-age system and a young (1 Gyr) system. We show that the radio power increases with magnetic field strength for magnetospheres with saturated convection potential, and broadly decreases with increasing orbital distance. We show that the magnetospheric convection at hot Jupiters will be saturated, and thus unable to dissipate the full available incident Poynting flux, such that the magnetic Radiometric Bode's Law (RBL) presents a substantial overestimation of the radio powers for hot Jupiters. Our radio powers for hot Jupiters are $\sim$5-1300 TW for hot Jupiters with field strengths of 0.1-10 $B_J$ orbiting a Sun-like star, while we find that competing effects yield essentially identical powers for hot Jupiters orbiting a young Sun-like star. However, in particular for planets with weaker magnetic fields our powers are higher at larger orbital distances than given by the RBL, and there are many configurations of planet that are expected to be detectable using SKA.