Radius and Mass Distribution of Ultra-short-period Planets

被引：12

作者：

Uzsoy, Ana Sofia M. ^{[1
,2
]}

Rogers, Leslie A. ^{[2
]}

Price, Ellen M. ^{[3
]}

机构：

[1] North Carolina State Univ, Dept Phys, 421 Riddick Hall,Box 8202, Raleigh, NC 27695 USA

[2] Univ Chicago, Dept Astron & Astrophys, 5640 S Ellis Ave, Chicago, IL 60637 USA

[3] Harvard & Smithsonian, Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

来源：

ASTROPHYSICAL JOURNAL | 2021年 / 919卷 / 01期

关键词：

VERSATILE METHOD; SUPER-EARTH; CORE; SYSTEMS; IRON;

D O I：

10.3847/1538-4357/ac0bb8

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Ultra-short-period (USP) planets are an enigmatic subset of exoplanets defined by having orbital periods <1 day. It is still not understood how USP planets form, or to what degree they differ from planets with longer orbital periods. Most USP planets have radii R (circle plus), while planets that orbit further from their star extend to Jupiter size (>10 R (circle plus)). Several theories attempt to explain the formation and composition of USP planets: they could be remnant cores of larger gas giants that lost their atmospheres due to photoevaporation or Roche-lobe overflow, or they could have developed through mass accretion in the innermost part of the protoplanetary disk. The radius and mass distribution of USP planets could provide important clues to distinguish between potential formation mechanisms. In this study, we first verify and update the Kepler catalog of USP planet host star properties, incorporating new data collected by the Gaia mission where applicable. We then use the transit depths measured by Kepler to derive a radius distribution and present occurrence rates for USP planets. Using spherical and tidally distorted planet models, we then derive a mass distribution for USP planets. Comparisons between the updated USP planet mass distribution and simulated planetary systems offer further insights into the formation and evolutionary processes shaping USP planet populations.

引用

页数：11

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