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High Energy Exoplanet Transits

Published online by Cambridge University Press:  12 September 2017

Joe Llama Open the ORCID record for Joe Llama [Opens in a new window]  and
Evgenya L. Shkolnik
Joe Llama
Affiliation:
Lowell Observatory, 1400 W. Mars Hill Road, Flagstaff, AZ. 86001. USA email: joe.llama@lowell.edu
Evgenya L. Shkolnik
Affiliation:
ASU School of Earth and Space Exploration, Tempe, AZ 85287. USA email: shkolnik@asu.edu
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Abstract

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X-ray and ultraviolet transits of exoplanets allow us to probe the atmospheres of these worlds. High energy transits have been shown to be deeper but also more variable than in the optical. By simulating exoplanet transits using high-energy observations of the Sun, we can test the limits of our ability to accurately measure the properties of these planets in the presence of stellar activity. We use both disk-resolved images of the Solar disk spanning soft X-rays, the ultraviolet, and the optical and also disk-integrated Sun-as-a-star observations of the Lyα irradiance to simulate transits over a wide wavelength range. We find that for stars with activity levels similar to the Sun, the planet-to-star radius ratio can be overestimated by up to 50% if the planet occults an active region at high energies. We also compare our simulations to high energy transits of WASP-12b, HD 189733, 55 Cnc b, and GJ 436b.

Keywords

Sun: activitystars: activitystars: spots(stars:) planetary systems
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S328: Living Around Active Stars , October 2016 , pp. 356 - 362
Copyright
Copyright © International Astronomical Union 2017 

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