Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 815, Issue 1, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/815/1/L12
Keywords
planets and satellites: atmospheres; planets and satellites: terrestrial planets; planet-star interactions; stars: activity; stars: low-mass; stars: rotation
Categories
Funding
- FWF NFN project [S11601-N16, S11602-N16, S11604-N16, S11607-N16]
- University of Vienna through the Faculty of Earth Sciences, Geography and Astronomy
- FWF project [P27256-N27]
Ask authors/readers for more resources
Terrestrial planets formed within gaseous protoplanetary disks can accumulate significant hydrogen envelopes. The evolution of such an atmosphere due to XUV driven evaporation depends on the activity evolution of the host star, which itself depends sensitively on its rotational evolution, and therefore on its initial rotation rate. In this Letter, we derive an easily applicable method for calculating planetary atmosphere evaporation that combines models for a hydrostatic lower atmosphere and a hydrodynamic upper atmosphere. We show that the initial rotation rate of the central star is of critical importance for the evolution of planetary atmospheres and can determine if a planet keeps or loses its primordial hydrogen envelope. Our results highlight the need for a detailed treatment of stellar activity evolution when studying the evolution of planetary atmospheres.
Authors
I am an author on this paper
Click your name to claim this paper and add it to your profile.
Reviews
Recommended
No Data Available