A possible correlation between planetary radius and orbital period for small planets

Helled, Ravit; Lozovsky, Michael; Zucker, S.

doi:10.1093/mnrasl/slv158

Cited by 48 publications

(24 citation statements)

References 21 publications

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“…We expect that the Kepler completion levels would be significant for this regime and verify from these tests that the correlation of planetary radii with orbital periods does not change significantly in the 3 samples analyzed. Helled et al (2016) also suggested the existence of a correlation between planetary radius and orbital periods for exoplanets with radii smaller than 4R ⊕ using Kepler data. They did a statistical analysis that took into consideration completeness values for the detection of planets by Kepler (Silburt et al 2015) to conclude that this correlation was not the result of a selection bias.…”

Section: A Possible Correlation Between Planetary Radii and Orbital Pmentioning

confidence: 90%

A Spectroscopic Analysis of the California-Kepler Survey Sample. I. Stellar Parameters, Planetary Radii, and a Slope in the Radius Gap

Martínez

Cunha

Ghezzi

et al. 2019

ApJ

117

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We present results from a quantitative spectroscopic analysis conducted on archival Keck/HIRES high-resolution spectra from the California-Kepler Survey (CKS) sample of transiting planetary host stars identified from the Kepler mission. The spectroscopic analysis was based on a carefully selected set of Fe I and Fe II lines, resulting in precise values for the stellar parameters of effective temperature (T eff ) and surface gravity (log g). Combining the stellar parameters with Gaia DR2 parallaxes and precise distances, we derived both stellar and planetary radii for our sample, with a median internal uncertainty of 2.8% in the stellar radii and 3.7% in the planetary radii. An investigation into the distribution of planetary radii confirmed the bimodal nature of this distribution for the small radius planets found in previous studies, with peaks at: ∼1.47 ± 0.05 R ⊕ and ∼2.72 ± 0.10 R ⊕ , with a gap at ∼ 1.9R ⊕ . Previous studies that modeled planetary formation that is dominated by photo-evaporation predicted this bimodal radii distribution and the presence of a radius gap, or photoevaporation valley. Our results are in overall agreement with these models. The high internal precision achieved here in the derived planetary radii clearly reveal the presence of a slope in the photo-evaporation valley for the CKS sample, indicating that the position of the radius gap decreases with orbital period; this decrease was fit by a power law of the form R pl ∝ P −0.11 , which is consistent with photo-evaporation and Earth-like core composition models of planet formation.

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Section: A Possible Correlation Between Planetary Radii and Orbital Pmentioning

confidence: 90%

A Spectroscopic Analysis of the California-Kepler Survey Sample. I. Stellar Parameters, Planetary Radii, and a Slope in the Radius Gap

Martínez

Cunha

Ghezzi

et al. 2019

ApJ

117

View full text Add to dashboard Cite

show abstract

“…4. Below the ridge lies a parameter region that is poorly represented by the Kepler set because of the detection threshold (Helled et al 2016) that is determined by the S/N of a transit, which for a given stellar radius is proportional to R 2 p /a orb (see Sect. 2), or R 2 p /P 2/3 orb .…”

Section: Period-radius Diagram For Short-period Planetsmentioning

confidence: 99%

Dearth of short-period Neptunian exoplanets: A desert in period-mass and period-radius planes

Mazeh

Holczer

Faigler

2016

A&A

315

351

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A few studies have reported a significant dearth of exoplanets with Neptune mass and radius with orbital periods below 2-4 d. This cannot be explained by observational biases because many Neptunian planets with longer orbital periods have been detected. The existence of this desert is similar to the appearance of the so-called brown-dwarf desert that suggests different formation mechanisms of planets and stellar companions with short orbital periods. Similarly, the Neptunian desert might indicate different mechanisms of formation and evolution for hot Jupiters and short-period super-Earths. We here follow a previous study and examine the location and shape of the desert in both the period-mass and period-radius planes, using the currently available large samples of planets. The desert in the period-mass plane has a relatively sharp upper edge, with a planetary mass that is inversely proportional to the planetary orbital period, while the lower, somewhat blurred, boundary is located along masses that are apparently linearly proportional to the period. The desert in the period-radius plane of the transiting planets is less clear. It seems as if the radius along the upper boundary is inversely proportional to the period to the power of one-third, while the lower boundary shows a radius that is proportional to the period to the power of two-thirds. The combination of the two upper bounds of the desert, in the period-mass and period-radius planes, yields a planetary mass-radius relation of R p /R Jup (1.2 ± 0.3)(M p /M Jup ) 0.27 ± 0.11 for 0.1 M p /M Jup 1. The derived shape of the desert, which might extend up to periods of 5-10 d, could shed some light on the formation and evolution of close-in planets.

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“…On the other hand, the condensation processes that formed the protoplanetary ices remain uncertain, because the Galileo probe failed to measure the deep abundance of oxygen by diving into a dry area of Jupiter [46]. Achieving this measurement by means of remote radio observations is one of the key and most challenging goals of the Juno mission [47,48], currently in orbit around Jupiter. At Saturn, the data on composition are scarcer (see Fig.…”

Section: Giant Planets Compositionmentioning

confidence: 99%

In Situ exploration of the giant planets

et al. 2021

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Remote sensing observations suffer significant limitations when used to study the bulk atmospheric composition of the giant planets of our Solar System. This impacts our knowledge of the formation of these planets and the physics of their atmospheres. A remarkable example of the superiority of in situ probe measurements was illustrated by the exploration of Jupiter, where key measurements such as the determination of the noble gases’ abundances and the precise measurement of the helium mixing ratio were only made available through in situ measurements by the Galileo probe. Here we describe the main scientific goals to be addressed by the future in situ exploration of Saturn, Uranus, and Neptune, placing the Galileo probe exploration of Jupiter in a broader context. An atmospheric entry probe targeting the 10-bar level would yield insight into two broad themes: i) the formation history of the giant planets and that of the Solar System, and ii) the processes at play in planetary atmospheres. The probe would descend under parachute to measure composition, structure, and dynamics, with data returned to Earth using a Carrier Relay Spacecraft as a relay station. An atmospheric probe could represent a significant ESA contribution to a future NASA New Frontiers or flagship mission to be launched toward Saturn, Uranus, and/or Neptune.

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A possible correlation between planetary radius and orbital period for small planets

Cited by 48 publications

References 21 publications

A Spectroscopic Analysis of the California-Kepler Survey Sample. I. Stellar Parameters, Planetary Radii, and a Slope in the Radius Gap

A Spectroscopic Analysis of the California-Kepler Survey Sample. I. Stellar Parameters, Planetary Radii, and a Slope in the Radius Gap

Dearth of short-period Neptunian exoplanets: A desert in period-mass and period-radius planes

In Situ exploration of the giant planets

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