Early UV Ingress in WASP-12b: Measuring Planetary Magnetic Fields

TL;DR

This paper investigates the formation of bow shocks around exoplanets like WASP-12b to explain early UV ingress observations and proposes using these shocks to estimate planetary magnetic field strengths.

Contribution

It introduces a model for bow shock formation due to stellar magnetic fields or winds, providing a method to constrain planetary magnetic fields from UV transit data.

Findings

Shock formation occurs at plasma temperatures below (4-5) x 10^6 K.

A bow shock can form ahead of the planet, causing early UV ingress.

Estimated upper limit for WASP-12b's magnetic field is about 24 G.

Abstract

Recently, Fossati et al. observed that the UV transit of WASP-12b showed an early ingress compared to the optical transit. We suggest that the resulting early ingress is caused by a bow shock ahead of the planetary orbital motion. In this Letter we investigate the conditions that might lead to the formation of such a bow shock. We consider two scenarios: (1) the stellar magnetic field is strong enough to confine the hot coronal plasma out to the planetary orbit and (2) the stellar magnetic field is unable to confine the plasma, which escapes in a wind. In both cases, a shock capable of compressing plasma to the observed densities will form around the planet for plasma temperatures T < (4 - 5) x 10^6 K. In the confined case, the shock always forms directly ahead of the planet, but in the wind case the shock orientation depends on the wind speed and hence on the plasma temperature. For higher wind temperatures, the shock forms closer to the line of centers between the planet and the star. We conclude that shock formation leading to an observable early UV ingress is likely to be a common feature of transiting systems and may prove to be a useful tool in setting limits on planetary magnetic field strengths Bp. In the case of WASP-12b, we derive an upper limit of about Bp=24 G.