Lithium in V505 Per

TL;DR

This study measures lithium abundances and stellar parameters of V505 Per's binary components, revealing differences in surface lithium and providing insights into stellar evolution at the Lithium Dip boundary.

Contribution

It provides new effective temperature measurements and lithium abundances for V505 Per, clarifying their position relative to the Lithium Dip and resolving previous discrepancies.

Findings

Surface lithium abundances differ between the stars.

Effective temperatures are higher than previously reported.

Surface rotation rate is slower than synchronous rotation.

Abstract

We determine the surface lithium abundance of the eclipsing binary components in V 505 Per (HIP 10961), A(Li)=2.65+/-0.07 and 2.35+/-0.1, which supports the rather unexpected conclusion that their surface Li abundances differ. We find effective temperatures 6600 K + 6550 K (~150 K higher than previously reported), which place the stars at the hot limit of the Lithium Dip, thus aleviating the previously suggested discrepancy with cluster stars of similar ages and temperatures. These temperatures are also more consistent with the system's Gaia spectral energy distribution. Our iron abundances, [Fe/H]=-0.15+\-0.07 and -0.25+\-0.1, agree with predictions of the higher temperatures deduced from our spectra and from evolutionary tracks. The surface rotation rate implied by our line profiles, 12.5+\-1 km/s, is smaller than the synchronous rotation rate, a curious result given the circular orbit and the age of the system.