<i>Father Charles E. Coughlin: Surrogate Spokesman for the Disaffected</i>. Ronald H. Carpenter

Thompson, P.M.

doi:10.1086/490471

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“…Where comp i is the survey completeness evaluated at the radius and orbital period of each planet in the bin, n is the number of stars surveyed, n p is the number of planets in each bin. The planet list is taken from Thompson et al (2017), using a disposition score cut of 0.9. The stellar properties are taken from Mathur et al (2017), removing giant stars with logg < 4.2 and culling the G dwarfs by selecting stars with 5300 K < T ef f < 6000 K. The completeness of each star is calculated with KeplerPORT (Burke & Catanzarite 2017), and the survey completeness is calculated by averaging over all stars that were successfully searched for planets according to the timeoutsumry flag.…”

Section: Application Of the Classification Scheme To Obtain Planet Ocmentioning

confidence: 99%

Exoplanet Classification and Yield Estimates for Direct Imaging Missions

Kopparapu

Hébrard

Belikov

et al. 2018

ApJ

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Future NASA concept missions that are currently under study, like Habitable Exoplanet Imaging Mission (HabEx) & Large Ultra-Violet Optical Infra Red (LUVOIR) Surveyor, would discover a large diversity of exoplanets. We propose here a classification scheme that distinguishes exoplanets into different categories based on their size and incident stellar flux, for the purpose of providing the expected number of exoplanets observed (yield) with direct imaging missions. The boundaries of this classification can be computed using the known chemical behavior of gases and condensates at different pressures and temperatures in a planetary atmosphere. In this study, we initially focus on condensation curves for sphalerite ZnS, H 2 O, CO 2 and CH 4 . The order in which these species condense in a planetary atmosphere define the boundaries between different classes of planets. Broadly, the planets are divided into rocky (0.5 − 1.0R ⊕ ), super-Earths (1.0 − 1.75R ⊕ ), sub-Neptunes (1.75 − 3.5R ⊕ ), sub-Jovians (3.5 − 6.0R ⊕ ) and Jovians (6 − 14.3R ⊕ ) based on their planet sizes, and 'hot', 'warm' and 'cold' based on the incident stellar flux. We then calculate planet occurrence rates within these boundaries for different kinds of exoplanets, η planet , using the community

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Section: Application Of the Classification Scheme To Obtain Planet Ocmentioning

confidence: 99%