Exploring the M-dwarf Luminosity--Temperature--Radius Relationships using Gaia DR2

Abstract

There is growing evidence that M-dwarf stars suffer radius inflation when compared to theoretical models, suggesting that models are missing some key physics required to completely describe stars at effective temperatures $(T_{\mathrm{SED}})$ less than about 4000K. The advent of Gaia DR2 distances finally makes available large datasets to determine the nature and extent of this effect. We employ an all-sky sample, comprising of $>$15\,000 stars, to determine empirical relationships between luminosity, temperature and radius. This is accomplished using only geometric distances and multiwave-band photometry, by utilising a modified spectral energy distribution fitting method. The radii we measure show an inflation of $3-7\%$ compared to models, but no more than a $1-2\%$ intrinsic spread in the inflated sequence. We show that we are currently able to determine M-dwarf radii to an accuracy of $2.4\%$ using our method. However, we determine that this is limited by the precision of metallicity measurements, which contribute $1.7\%$ to the measured radius scatter. We also present evidence that stellar magnetism is currently unable to explain radius inflation in M-dwarfs.

Accepted for publication in MNRAS 3 August 2019. 19 pages, 19 figures. Online supplementary material currently available at https://github.com/sammorrell/mn19-supplementary-material and https://doi.org/10.24378/exe.1683

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