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VI/156 M-dwarf Lum-Temp-Radius relationships (Morrell+, 2019)
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drwxr-xr-x 2 cats archive 89 Oct 16 2020 v02 Beginning of ReadMe :VI/156 M-dwarf Lum-Temp-Radius relationships (Morrell+, 2019)
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Exploring the M-dwarf Luminosity - Temperature - Radius Relationships
using Gaia DR2.
Morrell S.A.F, Naylor T.
<Mon. Not. R. Astron. Soc. 489, 2615-2633 (2019)>
=2019MNRAS.489.2615M
=2019yCat.6156....0M
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ADC_Keywords: Stars, late-type ; Stars, M-type ; Stars, diameters ;
Effective temperatures ; Magnitudes
Keywords: techniques: photometric - stars: fundamental parameters -
stars: late-type - stars: low-mass - stars: magnetic fields
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 (TSED) 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 >15000 stars, to determine empirical relation-ships
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 nomore 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.
Description:
We have measured the temperature, radius, and luminosity of a sample
of 15274 late K and early M-dwarf stars using a modified SED
fitting method. This method requires only accurate photometry and
precision astrometry and thus adds a fourth method to those used to
evaluate the veracity of stellar models. Importantly, this method
works natively in the Teff-R space which is crucial for the
characterization of exoplanets. We have derived empirical TSED-R and
LSED-R relations, which can be used to characterize exoplanet host
stars and validate stellar evolution models.