Testing the asteroseismic estimates of stellar radii with surface brightness-colour relations and Gaia DR3 parallaxes. Red giants and red clump stars

TL;DR

This study compares stellar radii from asteroseismic scaling relations with those from surface brightness-colour relations and Gaia parallaxes, revealing good overall agreement but with systematic differences influenced by stellar properties and chemical composition.

Contribution

It provides a detailed comparison of radius estimates from multiple methods for a large sample of RGB and RC stars, highlighting dependencies on parallax, metallicity, and stellar mass, and reports new insights into the effects of [$ ext{Fe/H}$] and [$ ext{α}$/Fe] on these estimates.

Findings

SBCR radii agree well with asteroseismic estimates, with small systematic offsets.

Parallax quality significantly affects the agreement, with better agreement at higher parallaxes.

Chemical composition, especially [$ ext{Fe/H}$] and [$ ext{α}$/Fe], influences radius estimates.

Abstract

We compared stellar radii derived from asteroseismic scaling relations with those estimated using two independent surface brightness-colour relations (SBCRs) and Gaia DR3 parallaxes. We cross-matched asteroseismic and astrometric data for over 6,400 RGB and RC stars from the APO-K2 catalogue with the TESS Input Catalogue v8.2 to obtain precise V band magnitudes and E(B-V) colour excesses. We then adopted two different SBCRs from the literature to derive stellar radius estimates, denoted as $R^a$ and $R^b$, respectively. We analysed the ratio of these SBCR-derived radii to the asteroseismic radius estimates, $R$, provided in the APO-K2 catalogue. Both SBCRs exhibited good agreement with asteroseismic radius estimates. On average, $R^a$ was overestimated by 1.2% with respect to $R$, while $R^b$ was underestimated by 2.5%. For stars larger than 20 $R_{\odot}$, SBCR radii are systematically lower than asteroseismic ones. The agreement with asteroseismic radii shows a strong dependence on the parallax. The dispersion is halved for stars with a parallax greater than 2.5 mas. In this subsample, $R^b$ showed perfect agreement with $R$, while $R^a$ remained slightly overestimated by 3%. A trend with [Fe/H] of 4% to 6% per dex was found. For stars less massive than about 0.95 $M_{\odot}$, SBCR radii were significantly higher than asteroseismic ones, by about 6%. This overestimation correlated with the presence of extended helium cores in these stars' structures relative to their envelopes. Furthermore, radius ratios showed a dichotomous behaviour at higher masses, mainly due to the presence of several RC stars with SBCR radii significantly lower with respect to asteroseismology. This behaviour originates from a different response of asteroseismic scaling relations and SBCR to [$\alpha$/Fe] abundance ratios for massive stars, both in RGB and RC phases, which is reported here for the first time.