The K2 M67 Study: Precise Mass for a Turnoff Star in the Old Open Cluster M67

TL;DR

This study precisely measures the mass of a turnoff star in M67 using a binary system, revealing discrepancies with current models and suggesting the need for revised physics like diffusion and reduced overshooting.

Contribution

It provides the first precise mass measurement of a turnoff star in M67 and highlights the necessity to update stellar evolution models for better accuracy.

Findings

Mass of the turnoff star is 1.222±0.006 M_sun.

Models require higher metallicity to match observations.

Diffusion and reduced overshooting are likely needed in models.

Abstract

We present a study of the bright detached eclipsing main sequence binary WOCS 11028 (Sanders 617) in the open cluster M67. Although the binary has only one eclipse per orbital cycle, we show that the masses of the stars can be derived very precisely thanks to a strong constraint on the orbital inclination: $M_A = 1.222\pm0.006 M_\odot$ and $M_B = 0.909\pm0.004 M_\odot$. We use a spectral energy distribution fitting method to derive characteristics of the component stars in lieu of the precise radii that would normally be derived from a doubly-eclipsing binary. The deconvolution of the SEDs reveals that the brighter component of the binary is at the faint turnoff point for the cluster -- a distinct evolutionary point that occurs after the convective core has been established and while the star is in the middle of its movement toward lower surface temperature, before the so-called hook at the end of main sequence. The measurements are in distinct disagreement with evolution models at solar metallicity: higher metal abundances are needed to reproduce the characteristics of WOCS 11028 A. We discuss the changes to model physics that are likely to be needed to address the discrepancies. The clearest conclusions are that diffusion is probably necessary to reconcile spectroscopic abundances of M67 stars with the need for higher metallicity models, and that reduced strength convective overshooting is occurring for stars at the turnoff. At super-solar bulk metallicity, various indicators agree on a cluster age between about 3.5 and 4.0 Gyr.