Probabilistic Mass-Radius Relationship for Sub-Neptune-Sized Planets

TL;DR

This paper introduces the first probabilistic mass-radius relationship for sub-Neptune-sized exoplanets, accounting for intrinsic scatter and uncertainties, using a Bayesian framework to improve mass estimates from radii.

Contribution

It presents a novel Bayesian probabilistic model for the mass-radius relation of sub-Neptune planets, incorporating intrinsic dispersion and measurement uncertainties.

Findings

Best-fit power law: M/M_⊕=2.7(R/R_⊕)^1.3

Mass scatter of approximately 1.9 M_⊕

Provides a framework for analyzing dependencies on period and stellar properties

Abstract

The Kepler Mission has discovered thousands of planets with radii $<4\ R_\oplus$, paving the way for the first statistical studies of the dynamics, formation, and evolution of these sub-Neptunes and super-Earths. Planetary masses are an important physical property for these studies, and yet the vast majority of Kepler planet candidates do not have theirs measured. A key concern is therefore how to map the measured radii to mass estimates in this Earth-to-Neptune size range where there are no Solar System analogs. Previous works have derived deterministic, one-to-one relationships between radius and mass. However, if these planets span a range of compositions as expected, then an intrinsic scatter about this relationship must exist in the population. Here we present the first probabilistic mass-radius relationship (M-R relation) evaluated within a Bayesian framework, which both quantifies this intrinsic dispersion and the uncertainties on the M-R relation parameters. We analyze how the results depend on the radius range of the sample, and on how the masses were measured. Assuming that the M-R relation can be described as a power law with a dispersion that is constant and normally distributed, we find that $M/M_\oplus=2.7(R/R_\oplus)^{1.3}$, a scatter in mass of $1.9\ M_\oplus$, and a mass constraint to physically plausible densities, is the "best-fit" probabilistic M-R relation for the sample of RV-measured transiting sub-Neptunes ($R_{pl}<4\ R_\oplus$). More broadly, this work provides a framework for further analyses of the M-R relation and its probable dependencies on period and stellar properties.