The Effects of Stellar Activity on Optical High-resolution Exoplanet Transmission Spectra

Chromospherically sensitive atomic lines display different spectra in stellar active regions, spots, and the photosphere, raising the possibility that exoplanet transmission spectra are contaminated by the contrast between various portions of the stellar disk. To explore this effect, we performed transit simulations of G-type and K-type stars for the spectral lines Ca ii K at 3933 ∗, Na i 5890 ∗, H i 6563 ∗ (Hα), and He i 10830 ∗. We find that strong facular emission and large coverage fractions can contribute a non-negligible amount to transmission spectra, especially for Hα, Ca ii K, and Na i D, while spots and filaments are comparatively unimportant. The amount of contamination depends strongly on the location of the active regions and the intrinsic emission strength. In particular, active regions must be concentrated along the transit chord in order to produce a consistent in-transit signal. Mean absorption signatures in Na i and Hα, for example, can reach ≈0.2% and 0.3%, respectively, for transits of active latitudes with line emission similar in strength to moderate solar flares. Transmission spectra of planets transiting active stars, such as HD 189733, are likely contaminated by the contrast effect, although the tight constraints on active region geometry and emission strength make it unlikely that consistent in-transit signatures are due entirely to the contrast effect. He i 10830 ∗ is not strongly affected and absorption signatures are likely diluted, rather than enhanced, by stellar activity. He i 10830 ∗ should thus be considered a priority for probing extended atmospheres, even in the case of active stars.