Planet Formation—Observational Constraints, Physical Processes, and Compositional Patterns

Mordasini, Christoph; Burn, Remo

doi:10.2138/rmg.2024.90.03

Reviews in Mineralogy and Geochemistry

2024

DOI: 10.2138/rmg.2024.90.03

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Planet Formation—Observational Constraints, Physical Processes, and Compositional Patterns

Christoph Mordasini,

Remo Burn

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2024

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Cited by 4 publications

References 408 publications

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Host Stars and How Their Compositions Influence Exoplanets

Hinkel,

Youngblood,

Soares-Furtado

2024

Reviews in Mineralogy and Geochemistry

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Host Stars and How Their Compositions Influence Exoplanets

Hinkel,

Youngblood,

Soares-Furtado

2024

Reviews in Mineralogy and Geochemistry

View full text Add to dashboard Cite

The Evolution and Delivery of Rocky Extra-Solar Materials to White Dwarfs

Veras,

Mustill,

Bonsor

2024

Reviews in Mineralogy and Geochemistry

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Different Planetary Eccentricity-period (PEP) Distributions of Small and Giant Planets

Bashi,

Mazeh,

Faigler

2024

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We used the database of 1040 short-period (1 ≤ P < 200 days) exoplanets radial-velocity orbits to study the planetary eccentricity-period (PEP) distribution. We first divided the sample into low- and high-mass exoplanet subsamples based on the distribution of the (minimum) planetary masses, which displays a clear two-Gaussian distribution, separated at 0.165M J. We then selected 216 orbits, low- and high-mass alike, with eccentricities significantly distinct from circular orbits. The 131 giant-planet eccentric orbits display a clear upper envelope, which we model quantitatively, rises monotonically from zero eccentricity and reaches an eccentricity of 0.8 at P ∼ 100 days. Conversely, the 85 low-mass planetary orbits display a flat eccentricity distribution between 0.1 and 0.5, with almost no dependence on the orbital period. We show that the striking difference between the two PEP distributions is not a result of the detection technique used. The upper envelope of the high-mass planets, also seen in short-period binary stars, is a clear signature of tidal circularization, which probably took place inside the planets, while the small-planet PEP distribution suggests that the circularization was not effective, probably due to dynamical interactions with neighboring planets.

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Planet Formation—Observational Constraints, Physical Processes, and Compositional Patterns

Cited by 4 publications

References 408 publications

Host Stars and How Their Compositions Influence Exoplanets

Host Stars and How Their Compositions Influence Exoplanets

The Evolution and Delivery of Rocky Extra-Solar Materials to White Dwarfs

Different Planetary Eccentricity-period (PEP) Distributions of Small and Giant Planets

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