The role of inner disk edges in shaping ultra-short-period planet systems around late M dwarfs

TL;DR

This study uses N-body simulations to explore how the inner edge of protoplanetary disks influences the formation of ultra-short-period planets around late M dwarfs, highlighting the importance of disk edge location.

Contribution

It demonstrates that the formation of USP planets is strongly dependent on the inner disk edge, with only certain edge configurations leading to their creation.

Findings

USP planets form when the disk's inner edge is fixed close-in or inward-evolving.

Planets tend to follow the movement of the disk's inner edge during formation.

Formation is favored when the inner edge is near the star's corotation radius.

Abstract

Close-in rocky planets are the most common type of exoplanets around late M dwarfs, ranging from more temperate worlds to highly irradiated lava planets with molten surfaces, and many theoretical studies have attempted to explain their formation. However, the origin of rocky planets with orbital periods shorter than one day, known as ultra-short-period (USP) planets, remains uncertain. We aim to investigate whether the formation and survival of USP planets is connected to the location of the inner edge of the protoplanetary disk, considering different disk edge prescriptions. We use N-body simulations that include planet-disk interactions, star-planet tidal interactions, and relativistic corrections, applied to a sample of lunar-mass planetary seeds growing via pebble accretion in a low-viscosity disk ($\alpha_t = 10^{-4}$). The inner edge of the disk is modeled in three ways: as a fixed close-in edge, as an outward-evolving edge set by the magnetospheric truncation radius, and as an inward-evolving edge defined by the corotation radius. USP planet formation appears to be tightly controlled by the location of the disk's inner edge. Our simulations show that only the close-in-fixed-edge Scenario and the inward-evolving-edge Scenario are capable of producing USP planets, as planets tend to follow the movement of the disk's inner edge. This suggests that USP planet formation is favored when the inner edge remains close to the corotation radius of a rapidly rotating star.