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 3 publications

References 406 publications

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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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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 Regulated by Galactic-scale Interstellar Turbulence

Winter,

Benisty,

Andrews

2024

ApJL

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Planet formation occurs over a few Myr within protoplanetary disks of dust and gas, which are often assumed to evolve in isolation. However, extended gaseous structures have been uncovered around many protoplanetary disks, suggestive of late-stage infall from the interstellar medium (ISM). To quantify the prevalence of late-stage infall, we apply an excursion set formalism to track the local density and relative velocity of the ISM over the disk lifetime. We then combine the theoretical Bondi–Hoyle–Lyttleton (BHL) accretion rate with a simple disk evolution model, anchoring stellar accretion timescales to observational constraints. Disk lifetimes, masses, stellar accretion rates, and gaseous outer radii as a function of stellar mass and age are remarkably well reproduced by our simple model that includes only ISM accretion. We estimate that 20%−70% of disks may be mostly composed of material accreted in the most recent half of their lifetime, suggesting that disk properties are not a direct test of isolated evolution models. Our calculations indicate that BHL accretion can also supply sufficient energy to drive turbulence in the outer regions of protoplanetary disks with viscous α SS ∼ 10−5 to 10−1, although we emphasize that angular momentum transport and particularly accretion onto the star may still be driven by internal processes. Our simple approach can be easily applied to semianalytic models. Our results represent a compelling case for regulation of planet formation by large-scale turbulence, with broad consequences for planet formation theory. This possibility urgently motivates deep observational surveys to confirm or refute our findings.

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

Cited by 3 publications

References 406 publications

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

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

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

Planet Formation Regulated by Galactic-scale Interstellar Turbulence

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