Mass-radius relation of low and very low-mass stars revisited with the VLTI

TL;DR

This study uses VLTI interferometry to measure the radii of low-mass stars, confirming stellar models and clarifying the impact of magnetic activity on star size discrepancies.

Contribution

It provides new interferometric radius measurements for low-mass stars, enhancing understanding of their luminosity and mass-radius relations and validating stellar evolution models.

Findings

Interferometric radii match stellar evolution model predictions.

Magnetically quiet stars' radii align with models, confirming magnetic activity's role.

Early K dwarfs' radii are consistent with a near-solar mixing length parameter.

Abstract

We measured the radii of 7 low and very low-mass stars using long baseline interferometry with the VLTI interferometer and its VINCI and AMBER near-infrared recombiners. We use these new data, together with literature measurements, to examine the luminosity- radius and mass-radius relations for K and M dwarfs. The precision of the new interferometric radii now competes with what can be obtained for double-lined eclipsing binaries. Interferometry provides access to much less active stars, as well as to stars with much better measured distances and luminosities, and therefore complements the information obtained from eclipsing systems. The radii of magnetically quiet late-K to M dwarfs match the predictions of stellar evolution models very well, providing direct confirmation that magnetic activity explains the discrepancy that was recently found for magnetically active eclipsing systems. The radii of the early K dwarfs are well reproduced for a mixing length parameter that approaches the solar value, as qualitatively expected.