# Magnetospheric Truncation, Tidal Inspiral, and the Creation of Short and   Ultra-Short Period Planets

**Authors:** Eve J. Lee, Eugene Chiang

arXiv: 1702.08461 · 2017-06-28

## TL;DR

This paper explores how magnetospheric truncation and tidal forces influence the distribution and formation of short and ultra-short period planets, providing a unified explanation for observed occurrence rate patterns.

## Contribution

It introduces a model linking stellar magnetospheres and tidal interactions to planet period distributions, explaining the observed cutoffs and spacing of ultra-short period planets.

## Key findings

- Planet occurrence rates match models with in situ formation and disk truncation.
- Tidal migration explains the wider spacing of ultra-short period planets.
- Predictions for occurrence rate breaks around A stars at ~1 day.

## Abstract

Sub-Neptunes around FGKM dwarfs are evenly distributed in log orbital period down to $\sim$10 days, but dwindle in number at shorter periods. Both the break at $\sim$10 days and the slope of the occurrence rate down to $\sim$1 day can be attributed to the truncation of protoplanetary disks by their host star magnetospheres at co-rotation. We demonstrate this by deriving planet occurrence rate profiles from empirical distributions of pre-main-sequence stellar rotation periods. Observed profiles are better reproduced when planets are distributed randomly in disks---as might be expected if planets formed in situ---rather than piled up near disk edges, as would be the case if they migrated in by disk torques. Planets can be brought from disk edges to ultra-short ($< 1$ day) periods by asynchronous equilibrium tides raised on their stars. Tidal migration can account for how ultra-short period planets (USPs) are more widely spaced than their longer period counterparts. Our picture provides a starting point for understanding why metal-rich stars tend to harbor more USPs, and why the sub-Neptune population drops at $\sim$10 days regardless of whether the host star is of type FGK or early M. We predict planet occurrence rates around A stars to also break at short periods, but at $\sim$1 day instead of $\sim$10 days because A stars rotate faster than lower mass stars (this prediction presumes that the planetesimal building blocks of planets can drift inside the dust sublimation radius).

## Full text

_Full body text omitted from this summary view._ Fetch the complete paper as Markdown: https://tomesphere.com/paper/1702.08461/full.md

## Figures

11 figures with captions in the complete paper: https://tomesphere.com/paper/1702.08461/full.md

## References

74 references — full list in the complete paper: https://tomesphere.com/paper/1702.08461/full.md

---
Source: https://tomesphere.com/paper/1702.08461