Variation in the pre-transit Balmer line signal around the hot Jupiter HD 189733 b

TL;DR

This study investigates the variability of pre-transit Balmer line signals around HD 189733 b, revealing that stellar activity influences the signals and complicates interpretations of circumplanetary material presence.

Contribution

The paper provides new observations of pre-transit signals with variable strength, analyzes stellar activity proxies, and simulates stellar variability effects on the signals.

Findings

Pre-transit signals vary in strength and timing across transits.

Stellar activity levels influence the observed pre-transit signals.

Simulations show stellar variability can reproduce observed signal changes.

Abstract

As followup to our recent detection of a pre-transit signal around HD 189733 b, we obtained full pre-transit phase coverage of a single planetary transit. The pre-transit signal is again detected in the Balmer lines but with variable strength and timing, suggesting that the bow shock geometry reported in our previous work does not describe the signal from the latest transit. We also demonstrate the use of the Ca II H and K residual core flux as a proxy for the stellar activity level throughout the transit. A moderate trend is found between the pre-transit absorption signal in the 2013 data and the Ca II H flux. This suggests that some of the 2013 pre-transit hydrogen absorption can be attributed to varying stellar activity levels. A very weak correlation is found between the Ca II H core flux and the Balmer line absorption in the 2015 transit, hinting at a smaller contribution from stellar activity compared to the 2013 transit. We simulate how varying stellar activity levels can produce changes in the Balmer line transmission spectra. These simulations show that the strength of the 2013 and 2015 pre-transit signals can be reproduced by stellar variability. If the pre-transit signature is attributed to circumplanetary material, its evolution in time can be described by accretion clumps spiraling towards the star, although this interpretation has serious limitations. Further high-cadence monitoring at H-alpha is necessary to distinguish between true absorption by transiting material and short-term variations in the stellar activity level.