Radius valley scaling among low mass stars with TESS

TL;DR

This study detects and analyzes the radius valley in planets around low-mass M dwarf stars using TESS data, revealing a different scaling behavior compared to Sun-like stars and suggesting alternative planet formation mechanisms.

Contribution

It provides the first measurement of the radius valley around M dwarfs and compares its properties with models, highlighting differences from higher-mass stars.

Findings

Radius valley located at 1.64 R_⊕ for M dwarfs.

Radius valley scaling with stellar mass as R_p ∝ M_*^{0.15±0.04}.

Flatter scaling suggests alternative formation mechanisms.

Abstract

The Transiting Exoplanet Survey Satellite (TESS) has been highly successful in detecting planets in close orbits around low-mass stars, particularly M dwarfs. This presents a valuable opportunity to conduct detailed population studies to understand how these planets depend on the properties of their host stars. The previously observed radius valley in Sun-like stars has not been unambiguously detected among M dwarfs, and how its properties varies when compared with more massive stars remains uncertain. We use a volume-limited sample of low mass stars with precise photometric stellar parameters from the bioverse catalog of TESS Objects of Interest (TOIs) confirmed planets and candidates within 120 pc. We detect the radius valley around M dwarfs at a location of 1.64 $\pm$ 0.03 $R_{\oplus}$ and with a depth of approximately 45${\%}$. The radius valley among GKM stars scales with stellar mass as $R_p \propto M_*^{0.15\pm 0.04}$. The slope is consistent, within 0.3$\sigma$, with those around Sun-like stars. For M dwarfs, the discrepancy is 3.6$\sigma$ with the extrapolated slope from the Kepler FGK sample, marking the point where the deviation from previous results begins. Moreover, we do not see a clear shift in the radius valley between early and mid M dwarfs. The flatter scaling of the radius valley for lower-mass stars suggests that mechanisms other than atmospheric mass loss through photoevaporation may shape the radius distribution of planets around M dwarfs. Comparison of the slope with various planet formation and evolution models matches well with pebble accretion models including waterworlds, indicating a potentially different regime of planet formation that can be probed with exoplanets around the lowest mass stars.