Transit Variability in Bow Shock-Hosting Planets

TL;DR

This paper explores how bow shock characteristics around exoplanets vary over time due to orbital motion and stellar environment changes, with implications for observational detection and understanding star-planet interactions.

Contribution

It provides a theoretical analysis of the causes and observational signatures of bow shock variability in exoplanets, especially in eccentric systems, expanding understanding of star-planet magnetic interactions.

Findings

Shock characteristics vary with orbital phase in eccentric systems.

Time offsets between UV and optical light curves are generally less than transit duration.

Non-thermal radio emissions are modulated by orbital phase.

Abstract

We investigate the formation of bow shocks around exoplanets as a result of the interaction of the planet with the coronal material of the host star, focusing on physical causes that can lead to temporal variations in the shock characteristics. We recently suggested that WASP-12b may host a bow shock around its magnetosphere, similarly to the one observed around the Earth. For WASP12b, the shock is detected in the near-UV transit light curve. Observational follow-up suggests that the near-UV light curve presents temporal variations, which may indicate that the stand-off distance between the shock and the planet is varying. This implies that the size of the planet's magnetosphere is adjusting itself in response to variations in the surrounding ambient medium. We investigate possible causes of shock variations for the known eccentric (e>0.3) transiting planets. We show that, because the distance from the star changes along the orbit of an eccentric planet, the shock characteristics are modulated by orbital phase. We predict time offsets between the beginnings of the near-UV and optical light curves that are, in general, less than the transit duration. Variations in shock characteristics caused in eccentric systems can only be probed if the shock is observed at different orbital phases, which is, in general, not the case for transit observations. However, non-thermal radio emission produced by the interaction of the star and planet should be modulated by orbital phase. We also quantify the response of the shock to variations in the coronal material itself due to, e.g., a non-axisymmetric stellar corona, planetary obliquity, intrinsic variations of the stellar magnetic field. Such variations do not depend on the system eccentricity. We conclude that, for systems where a shock is detectable through transit light curve observations, shock variations should be a common occurrence. (Abridged)