Transient Corotating Clumps Around Adolescent Low-Mass Stars From Four Years of TESS

TL;DR

This study used four years of TESS data to identify and analyze complex periodic variables (CPVs) around young, low-mass stars, revealing their properties, lifetimes, and possible origins related to magnetic fields and corotating dust or gas.

Contribution

First comprehensive TESS-based survey of CPVs around low-mass stars, identifying new objects and characterizing their variability and potential magnetic and circumstellar origins.

Findings

Most CPVs are young and low-mass stars.

Flux dips last around 100 cycles and are linked to corotating material.

Some dips match the timescale for transiting small bodies at the corotation radius.

Abstract

Complex periodic variables (CPVs) are stars that exhibit highly structured and periodic optical light curves. Previous studies have indicated that these stars are typically disk-free pre-main-sequence M dwarfs with rotation periods ranging from 0.2 to 2 days. To advance our understanding of these enigmatic objects, we conducted a blind search using TESS 2-minute data of 65,760 K and M dwarfs with $T$<16 mag and $d$<150 pc. We found 50 high-quality CPVs, and subsequently determined that most are members of stellar associations. Among the new discoveries are the brightest ($T$$\approx$9.5 mag), closest ($d$$\approx$20 pc), and oldest ($\approx$200 Myr) CPVs known. One exceptional object, LP 12-502, exhibited up to eight flux dips per cycle. Some of these dips coexisted with slightly different periods, and the shortest-duration dips precisely matched the expected timescale for transiting small bodies at the corotation radius. Broadly, our search confirms that CPVs are mostly young ($\lesssim$150 Myr) and low-mass ($\lesssim$0.4 $M_\odot$). The flux dips characteristic of the class have lifetimes of $\approx$100 cycles, although stellar flares seem to induce sudden dip collapse once every few months. The most plausible explanation for these phenomena remains corotating concentrations of gas or dust. The gas or dust is probably entrained by the star's magnetic field, and the sharp features could result from a multipolar field topology, a hypothesis supported by correspondences between the light curves of CPVs and of rapidly rotating B stars known to have multipolar magnetic fields.