IN SITU FORMATION AND DYNAMICAL EVOLUTION OF HOT JUPITER SYSTEMS

By K. Batygin, P. Bodenheimer, Gregory Laughlin. 2015

142 citations recorded by the source corpus.

Hot Jupiters, giant extrasolar planets with orbital periods shorter than ∼10 days, have long been thought to form at large radial distances, only to subsequently experience long-range inward migration. Here, we offer the contrasting view that a substantial fraction of the hot Jupiter population formed in situ via the core-accretion process. We show that under conditions appropriate to the inner regions of protoplanetary disks, rapid gas accretion can be initiated by super-Earth-type planets, comprising 10–20 Earth masses of refractory material. An in situ formation scenario leads to testable consequences, including the expectation that hot Jupiters should frequently be accompanied by additional low-mass planets with periods shorter than ∼100 days. Our calculations further demonstrate that dynamical interactions during the early stages of planetary systems’ lifetimes should increase the inclinations of such companions, rendering transits rare. High-precision radial velocity monitoring provides the best prospect for their detection.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/65e46c4ba6e232bfa97c221704e7e528b533b016

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In Astronomy and Astrophysics

1. J. Owen
2. Timothy Morton
3. E. Petigura
4. B. Fulton
5. Andrew W. Howard
6. G. Marcy
7. J. Johnson
8. J. Winn

In Instrumentation

1. Timothy Morton
2. J. Owen
3. E. Petigura
4. Andrew W. Howard
5. G. Marcy
6. B. Fulton
7. J. Winn
8. J. Johnson

Citations in the corpus

• The California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets (2017, background): “A non-exhaustive list of theories includes star-planet Kozai (e.g. Wu & Murray 2003), planetplanet Kozai (e.g. Naoz et al. 2011), smooth disk-driven Type-I migration (e.g. Ida & Lin 2008), high eccentricity migration, and in situ formation (e.g. Batygin et al. 2016).”
• Dearth of short-period Neptunian exoplanets - a desert in period-mass and period-radius planes (2016, background): “Another suggestion that considered a common formation mechanism for super-Earths and hot Jupiters has been made by Batygin et al. (2015), who argued for in situ formation of hot Jupiters.”
• Photoevaporation and high-eccentricity migration created the sub-Jovian desert (2018, background): “…Chatterjee & Tan 2014; Lee et al. 2014; Lee & Chiang 2016; Mohanty et al. 2017) suggested that low-mass super-Earths/mini-Neptunes formed in situ, close to their current orbital locations, while Boley et al. (2016); Batygin et al. (2016) suggested that hot-Jupiters could also have formed in-situ.”
• The GAPS Programme with HARPS-N at TNG - XIV. Investigating giant planet migration history via improved eccentricity and mass determination for 231 transiting planets (2017, unknown): “Alternative theories to both high-eccentricity and disc migration to explain the presence of hot and warm giant planets in compact systems foresee in situ formation (Batygin et al. 2016; Huang et al. 2016), although these theories need observational corroboration (Batygin et al. 2016).”