Planet occurrence rate density models including stellar effective temperature

TL;DR

This paper develops new models for planet occurrence rates that incorporate stellar effective temperature, improving prediction accuracy across different star types, especially for M dwarfs, based on Kepler data.

Contribution

It introduces the first occurrence rate models explicitly including stellar effective temperature, with distinct fits for M stars and F-G-K stars, enhancing exoplanet occurrence predictions.

Findings

Models fit well with previous studies.

Inclusion of stellar temperature improves accuracy.

Distinct models for M and F-G-K stars.

Abstract

We present planet occurrence rate density models fit to Kepler data as a function of semi-major axis, planetary radius, and stellar effective temperature. We find that occurrence rates for M type stars with lower effective temperature do not follow the same trend as F, G, and K type stars when including a polynomial function of effective temperature in an occurrence rate density model and a better model fit includes a break in effective temperature. Our model fit for M type stars consists of power laws on semi-major axis and planetary radius. Our model fit for F, G, and K type stars consists of power laws on semi-major axis and planetary radius broken at 2.771$ R_\oplus $ and a quadratic function of stellar effective temperature. Our models show agreement with published occurrence rate studies and are the first to explicitly include stellar effective temperature as a variable. By introducing stellar effective temperature into our occurrence rate density models, we enable more accurate occurrence rate predictions for individual stars in mission simulation and science yield calculations for future and proposed exoplanet finding missions.