REVIEW 6 cited by
The mass-radius relation of exoplanets, revisited
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
The mass-radius relation of exoplanets, revisited
read the original abstract
Determining the mass-radius ($M$-$R$) relation of exoplanets is important for exoplanet characterization. Here we present a re-analysis of the $M$-$R$ relations and their transitions using exoplanetary data from the PlanetS catalog which only includes planets with reliable mass and radius determinations. We find that "small planets" correspond to planets with masses of up to $\sim4.4 M_\oplus$ (within 17%) where $R \propto M^{0.27}$. Planets with masses between $\sim4.4$ and $127 M_\oplus$ (within 5%) can be viewed as "intermediate-mass" planets, where $R \propto M^{0.67}$. Massive planets, or gas giant planets, are found to have masses beyond $127 M_\oplus$ with an $M$-$R$ relation of $R \propto M^{-0.06}$. By analyzing the radius-density relation we also find that the transition between "small" to "intermediate-size" planets occurs at a planetary radius of $\sim1.6 R_\oplus$ (within 3%). Our results are consistent with previous studies and provide an ideal fit for the currently-measured planetary population.
Forward citations
Cited by 6 Pith papers
-
The influence of composition gradients on giant planet radii
Composition gradients change giant-planet radii only by altering total entropy over time; after a ~Gyr decoupling age the radius depends only on mass and bulk metallicity.
-
Volcanic Satellites and Ion Escape in the Magnetospheres of Ultra-Cool and Brown Dwarf Stars
A tidally heated, Io-like planet orbiting LSR J1835+3259 within about 10-14 stellar radii could supply the ~100,000 kg/s plasma flow implied by its auroral radio emission.
-
Dynamically Selected Mass-Radius Relationship for Low Mass Exoplanets
Planets inferred to have suffered giant collisions are more massive than pristine ones but retain comparable hydrogen envelope fractions, implying collisions occurred before disk gas dispersal.
-
Revisiting TOI-4438 and TOI-442 planetary systems with new observations from SPIRou and TESS
Refined masses and radii for TOI-4438 b and TOI-442 b, stellar rotation periods from magnetic variability, and a single-transit planet candidate around TOI-4438.
-
HD 148797: A bright F-type star with two moderate-period low-density sub-Jovian planets. Compact multi-planet architectures are common in the Neptunian savanna
HD 148797 hosts two ~40 ME, ~8.3 RE, low-density savanna planets near a 1.619 period ratio whose anti-correlated TTVs yield masses and support compact multi-planet architectures as typical in the savanna.
-
Radio emission from star-planet interactions
SKA can transform exoplanet science via radio M-SPI detections if given substantial dedicated time comparable to successful optical campaigns, based on ECMI scaling and ensemble predictions.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.