MHD simulations of the space weather in Proxima b: Habitability conditions and radio emission

TL;DR

This study uses 3D MHD simulations to analyze the space weather environment, magnetic shielding, and radio emissions of Proxima b under various stellar wind conditions, informing its habitability and detectability.

Contribution

It provides the first detailed 3D magneto-hydrodynamic modeling of Proxima b's space weather and radio emission, considering both calm and extreme stellar wind scenarios.

Findings

Proxima b's magnetic field can shield the surface from stellar wind under most conditions.

Radio emission can reach up to 7×10^{19} erg/s during calm space weather.

Extreme space weather increases radio emission by over two orders of magnitude.

Abstract

The habitability of exoplanets hosted by M-dwarf stars dramatically depends on their space weather. We present 3D magneto-hydrodynamic simulations to characterise the magneto-plasma environment and thus the habitability of the Earth-like planet Proxima b when it is subject to both calm and extreme (CME-like) space weather conditions. We study the role of the stellar wind and planetary magnetic field, and determine the radio emission arising from the interaction between the stellar wind of Proxima and the magnetosphere of its planet Proxima b. We find that if Prox b has a magnetic field similar to that of the Earth ($B_{\rm p} = B_\oplus \approx 0.32$ G) or larger, the magnetopause standoff distance is large enough to shield the surface from the stellar wind for essentially any planetary tilt but the most extreme values (close to $90^{\circ} $), under a calm space weather. Even if Proxima b is subject to more extreme space weather conditions, the planet is well shielded by an Earth-like magnetosphere ($B_{\rm p} \approx B_\oplus$; $ \approx 23.5^{\circ}$), or if it has tilt smaller than that of the Earth. For calm space weather conditions, the radio emission caused by the day-side reconnection regions can be as high as 7$\times10^{19}$ erg s$^{-1}$ in the super-Alfv\'enic regime, and is on average almost an order of magnitude larger than the radio emission in the sub-Alfv\'enic cases, due to the much larger contribution of the bow shock. We also find that the energy dissipation at the bow shock is independent of the angle between the planet's magnetic dipole and the incident stellar wind flow. If Prox b is subject to extreme space weather conditions, the radio emission is more than two orders of magnitude larger than under calm space weather conditions. This result yields expectations for a direct detection--from Earth--in radio of giant planets in close-in orbits.