Journal
ASTRONOMY & ASTROPHYSICS
Volume 577, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201526146
Keywords
Sun: evolution; stars: rotation; stars: activity; stars: solar-type; planets and satellites: atmospheres
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Funding
- Emerging Fields grant of the University of Vienna through the Faculty of Earth Sciences, Geography and Astronomy
- FWF NFN [S11601-N16, S11604-N16, S11607-N16]
- Austrian Science Fund (FWF)
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Aims. We aim to describe the pre-main-sequence and main-sequence evolution of X-ray and extreme-ultaviolet radiation of a solar-mass star based on its rotational evolution starting with a realistic range of initial rotation rates. Methods. We derive evolutionary tracks of X-ray radiation based on a rotational evolution model for solar-mass stars and the rotation-activity relation. We compare these tracks to X-ray luminosity distributions of stars in clusters with different ages. Results. We find agreement between the evolutionary tracks derived from rotation and the X-ray luminosity distributions from observations. Depending on the initial rotation rate, a star might remain at the X-ray saturation level for very different time periods, from approximate to 10 Myr to approximate to 300 Myr for slow and fast rotators, respectively. Conclusions. Rotational evolution with a spread of initial conditions leads to a particularly wide distribution of possible X-ray luminosities in the age range of 20-500 Myr, before rotational convergence and therefore X-ray luminosity convergence sets in. This age range is crucial for the evolution of young planetary atmospheres and may thus lead to very different planetary evolution histories.
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