PLANETARY POPULATION SYNTHESIS COUPLED WITH ATMOSPHERIC ESCAPE: A STATISTICAL VIEW OF EVAPORATION
By Sheng Jin, C. Mordasini, V. Parmentier, R. van Boekel, Th. Henning, J. Ji. 2014
171 citations recorded by the source corpus.
We apply hydrodynamic evaporation models to different synthetic planet populations that were obtained from a planet formation code based on the core-accretion paradigm. We investigated the evolution of the planet populations using several evaporation models, which are distinguished by the driving force of the escape flow (X-ray or EUV), the heating efficiency in energy-limited evaporation regimes, or both. Although the mass distribution of the planet populations is barely affected by evaporation, the radius distribution clearly shows a break at approximately 2 R⊕. We find that evaporation can lead to a bimodal distribution of planetary sizes and to an “evaporation valley” running diagonally downward in the orbital distance—planetary radius plane, separating bare cores from low-mass planets that have kept some primordial H/He. Furthermore, this bimodal distribution is related to the initial characteristics of the planetary populations because low-mass planetary cores can only accrete small primordial H/He envelopes and their envelope masses are proportional to their core masses. We also find that the population-wide effect of evaporation is not sensitive to the heating efficiency of energy-limited description. However, in two extreme cases, namely without evaporation or with a 100% heating efficiency in an evaporation model, the final size distributions show significant differences; these two scenarios can be ruled out from the size distribution of Kepler candidates.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/ace7db5ba33805e837762843dd380b9ddf2dfad0
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In Astronomy and Astrophysics
Citations in the corpus
- THE IMPRINT OF EXOPLANET FORMATION HISTORY ON OBSERVABLE PRESENT-DAY SPECTRA OF HOT JUPITERS (2016, methodology): “In our evolutionary model (see Jin et al. 2014), the envelope evaporation rate due to XUV irradiation is modeled at high EUV fluxes with a radiationrecombination limited rate (Murray-Clay et al. 2009), and with an energy limited rate at lower fluxes.”
- An asteroseismic view of the radius valley: stripped cores, not born rocky (2017, background): “…models predict that atmospheric erosion of short-period planets results in the presence of a “photoevaporation valley”, i.e. a gap in the radius distribution of planets around 1.75−2 R⊕ (Owen & Wu 2013; Jin et al. 2014; Lopez & Fortney 2014; Chen & Rogers 2016; Lopez & Rice 2016; Owen & Wu 2017).”
- The California-Kepler Survey. III. A Gap in the Radius Distribution of Small Planets (2017, background): “Several authors have predicted the existence of a “photoevaporation valley” in the distribution of planet radii (e.g., Owen & Wu 2013; Lopez & Fortney 2014; Jin et al. 2014; Chen & Rogers 2016; Lopez & Rice 2016).”
- Atmospheric Escape and the Evolution of Close-In Exoplanets (2018, background): “Further studies by Jin et al. (2014), Howe & Burrows (2015) and Chen & Rogers (2016) found similar results.”
- Compositional Imprints in Density–Distance–Time: A Rocky Composition for Close-in Low-mass Exoplanets from the Location of the Valley of Evaporation (2017, methodology): “These prominent evaporation features are not very sensitive to the loss efficiency in an evaporation model (Jin et al. 2014).”
- They are small worlds after all: revised properties of Kepler M dwarf stars and their planets (2015, background): “15) as it relates to evaporation of H/He envelopes (e.g., Jin et al. 2014).”
- The Evaporation Valley in the Kepler Planets (2017, background): “For simplicity, we adopt a constant η = 0.1 (the so-called “energy-limited” approach, see e.g., Lopez & Fortney 2013).”
- The California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets (2017, background): “This gap was predicted by various groups who modeled the erosion erosion of envelopes (e.g. Lopez & Fortney 2013; Owen & Wu 2013; Jin et al. 2014; Chen & Rogers 2016).”
- The California-Kepler Survey. VII. Precise Planet Radii Leveraging Gaia DR2 Reveal the Stellar Mass Dependence of the Planet Radius Gap (2018, background): “A gap in the radius distribution was predicted by several groups who considered the effect of photoevaporation on planetary envelopes by X-ray and extreme ultraviolet (XUV) radiation (Lopez & Fortney 2013; Owen & Wu 2013; Jin et al. 2014; Chen & Rogers 2016).”
- Core-powered mass-loss and the radius distribution of small exoplanets (2017, background): “Owen & Wu (2013) have already noticed such a valley in the observations, and explained it by atmosphere evaporation due to high-energy stellar photons (see also Lopez & Fortney 2013; Jin et al. 2014; Chen & Rogers 2016; Lehmer & Catling 2017).”