Energetics of star-planet magnetic interactions: Novel insights from 3D modelling

TL;DR

This paper uses 3D MHD simulations to derive a new scaling law for the power generated by star-planet magnetic interactions, providing more accurate estimates than previous analytical models.

Contribution

It presents a numerically supported scaling law for SPMI energetics based on extensive 3D simulations, improving upon existing analytical estimates.

Findings

Existing scaling laws underestimate SPMI power by at least an order of magnitude.

The derived scaling law accounts for extended magnetic structures and stellar wind interactions.

Power transfer depends on both planetary obstacles and the Alfven wings' magnetic interactions.

Abstract

Star-planet magnetic interactions (SPMI) occurring in the sub-Alfvenic regime can, in principle, induce stellar chromospheric hotspots. Currently, estimates of the power generated by SPMI primarily rely on analytical scaling laws that relate stellar and planetary parameters to the interaction energetics. The existing scaling laws published in the literature so far do not agree with each other by at least an order of magnitude. Our aim is to quantify an absolute upper limit on the power that a planet can channel back to its host star during such interactions, which in turn lead to the formation of stellar hotspots. By performing a series of 3D MHD simulations with varied parameters known to influence the energetics of SPMI, we derive a numerically supported scaling law that can be used to reliably estimate the energy channeled from the planet back to the star. Our results suggest that existing analytical scaling laws may not fully capture the power transferred from the planet to the star through SPMI. The scaling law derived from our numerical simulations appears to provide a more comprehensive estimate, reflecting dependencies on common stellar and planetary parameters also considered in earlier models. Moreover, our findings indicate that power generation involves not only the planetary obstacle itself but also the extended magnetic structure of the Alfven wings interacting with the streaming stellar wind. This study suggests that care should be taken when applying analogies directly from jovian sub-Alfvenic interactions to SPMI, as the underlying physical conditions (specifically the value of the Alfvenic Mach number) may not be directly comparable. Our numerically derived scaling law offers a potentially improved approach for estimating SPMI power, capturing some of the interaction's complexities exclusive to SPMI.