The puzzling story of flare inactive ultra fast rotating M dwarfs. II. Searching for radial velocity variations. Issue 2 (29th January 2022)

• Record Type: Journal Article
• Authors: Ramsay, Gavin; Hakala, Pasi; Doyle, J Gerry; Doyle, Lauren; Bagnulo, Stefano
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 511:Issue 2(2022)
• Page Start: 2755
• Page End: 2764
• Publication Date: 2022-01-29
• Subjects: accretion, accretion discs -- stars: activity -- binaries close -- stars: flare -- stars: low-mass -- stars: magnetic field; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stac188
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Observations made using TESS revealed a sample of low-mass stars which show a periodic modulation on a period <0.2 d. Surprisingly, many of these ultra fast rotating (UFR) stars showed no evidence of flare activity which would be expected from such rapidly rotating stars. We present results from a spectroscopic survey of UFRs using the Nordic Optical Telescope to search for radial velocity variations which could reveal evidence for binarity. Our sample of 29 sources have a photometric period between 0.1–0.2 d, cover spectral classes of M0-4V, and show no evidence for flares. We detect only one source with clear radial velocity shifts, with another two having Gaia RUWE values which suggests they are binaries. Further observations reveal the former star possibly contains a brown dwarf companion with a mass of M 2 > 58 M Jup and probability P( M 2 < 90 M Jup ) = 50 per cent. There is no evidence for the companion in our spectra, strengthening the case for a brown dwarf companion. We also examine the folded TESS light curves of all our targets, finding at least two are eclipsing binaries and one which has been contaminated by a spatially nearby δ Sct star. We estimate that around 1/4 of our targets may have been contaminated by short period variable stars. However, the majority of our targets are consistent with being single, low mass stars whose variability is due to starspots. We outline the possible reasons why they are not flare active despite being such rapid rotators.