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The Stellar Activity of TRAPPIST-1 and Consequences for the Planetary Atmospheres
Stockholm University, Faculty of Science, Department of Astronomy.
Number of Authors: 22017 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 851, no 2, article id 77Article in journal (Refereed) Published
Abstract [en]

The signatures of planets hosted by M dwarfs are more readily detected with transit photometry and radial velocity methods than those of planets around larger stars. Recently, transit photometry was used to discover seven planets orbiting the late-M dwarf TRAPPIST-1. Three of TRAPPIST-1's planets fall in the Habitable Zone, a region where liquid water could exist on the planetary surface given appropriate planetary conditions. We aim to investigate the habitability of the TRAPPIST-1 planets by studying the star's activity and its effect on the planets. We analyze previously published space-and ground-based light curves and show the photometrically determined rotation period of TRAPPIST-1 appears to vary over time due to complicated, evolving surface activity. The dramatic changes of the surface of TRAPPIST-1 suggest that rotation periods determined photometrically may not be reliable for this and similarly active stars. While the activity of the star is low, we use the premise of the cosmic shoreline to provide evidence that the TRAPPIST-1 environment has potentially led to the erosion of possible planetary atmospheres by extreme ultraviolet stellar emission.

Place, publisher, year, edition, pages
2017. Vol. 851, no 2, article id 77
Keywords [en]
stars: activity, stars: individual (TRAPPIST-1), stars: variables: general, starspots
National Category
Physical Sciences
Identifiers
URN: urn:nbn:se:su:diva-150950DOI: 10.3847/1538-4357/aa991eISI: 000418139100006OAI: oai:DiVA.org:su-150950DiVA, id: diva2:1174090
Available from: 2018-01-15 Created: 2018-01-15 Last updated: 2018-01-15Bibliographically approved

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