A Plasma Torus around a Young Low-mass Star

Abstract A small fraction of red dwarfs younger than ∼100 million years show structured, periodic optical light curves suggestive of transiting opaque material that corotates with the star. However, the composition, origin, and even the existence of this material are uncertain. The main alternative hypothesis is that these complex periodic variables (CPVs) are explained by complex distributions of bright or dark regions on the stellar surfaces. Here we present time-series spectroscopy and photometry of a rapidly rotating ( P = 3.9 hr) CPV, TIC 141146667. The spectra show sinusoidal time-varying H α emission at twice to four times the star’s equatorial velocity, providing direct evidence for cool (≲10 4 K) plasma clumps trapped in corotation around a CPV. These data support the idea that young, rapidly rotating M dwarfs can sustain warped tori of cool plasma, similar to other rapidly rotating magnetic stars. Outstanding questions include whether dust clumps in these plasma tori explain CPV light curves and whether the tori originate from the star or are fed by external sources. Rough estimates suggest that ≳10% of M dwarfs host similar structures during their early lives.