Stellar rotation and its connection to the evolution of hydrogen-dominated atmospheres of exoplanets
arXiv:2111.09653 · doi:10.1002/asna.20210077
Abstract
The population of known low- to intermediate-mass exoplanets shows a large spread in densities, which is believed to be due to the diversity of planetary atmospheres and thus controlled by planetary atmospheric mass loss. One of the main drivers of long-term atmospheric escape is the absorption of high-energy XUV radiation from the host star. For main sequence solar-like stars, rotation and XUV radiation are closely connected, with faster rotating stars being XUV brighter and with both rotation and XUV decreasing with time. This evolution, however, does not follow a unique path, as stars born with the same mass and metallicity can have widely different initial rotation rates. This non-uniqueness holds up to about 1 Gyr, while atmospheric escape from exoplanets is strongest. The atmospheric mass loss through this period is often deciding the future of the planet and its position in the observed population. Therefore, the diversity of possible stellar histories can be an uncertain factor affecting the predictions of population studies. Here, I explore its relevance for different planets and different host stars.
9 pages, 5 figures, proceedings of the XMM-Newton Workshop 2021 "A High-Energy View of Exoplanets and their Environments". Original article can be found at https://onlinelibrary.wiley.com/doi/10.1002/asna.20210077
References in corpus (20)
- Modules for Experiments in Stellar Astrophysics (MESA)
- Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics
- Planetary population synthesis coupled with atmospheric escape: a statistical view of evaporation
- The Mass-Dependence of Angular Momentum Evolution in Sun-Like Stars
- Planetary Candidates Observed by Kepler VI: Planet Sample from Q1-Q16 (47 Months)
- The Extreme Ultraviolet and X-Ray Sun in Time: High-Energy Evolutionary Tracks of a Solar-Like Star
- Stellar Winds on the Main-Sequence II: the Evolution of Rotation and Winds
- XUV-driven mass loss from extrasolar giant planets orbiting active stars
- A giant impact as the likely origin of different twins in the Kepler-107 exoplanet system
- Photoevaporation vs. core-powered mass-loss: model comparison with the 3D radius gap
- Aeronomical constraints to the minimum mass and maximum radius of hot low-mass planets
- Relation of X-ray activity and rotation in M dwarfs and predicted time-evolution of the X-ray luminosity
- Planet formation by pebble accretion in ringed disks
- Kepler-411: a four-planet system with an active host star
- Hydrodynamic simulations of captured protoatmospheres around Earth-like planets
- Susceptibility of planetary atmospheres to mass loss and growth by planetesimal impacts: the impact shoreline
- Close-in sub-Neptunes reveal the past rotation history of their host stars: atmospheric evolution of planets in the HD3167 and K2-32 planetary systems
- A critical assessment of the applicability of the energy-limited approximation for estimating exoplanetary mass-loss rates
- How does the mass and activity history of the host star affect the population of low-mass planets?
- Aerosol Constraints on the Atmosphere of the Hot Saturn-mass planet WASP-49b