English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We determine absolute dimensions and abundances for the three F-typemain-sequence detached eclipsing binaries AD Boo, VZ Hya, and WZ Oph andperform a detailed comparison with results from recent stellar evolutionarymodels. uvby light curves and standard photometry were obtained at ESO,radialvelocity observations at CfA facilities, and high-resolution spectra with ESO'sFEROS spectrograph. State-of-the-art methods were applied for the analyses.Masses and radii that are precise to 0.5-0.7% and 0.4-0.9%, respectively, havebeen established for the components, which span the ranges of 1.1 to 1.4 M_sunand 1.1 to 1.6 R_sun. The [Fe/H] abundances are from -0.27 to +0.10, withuncertainties between 0.07 and 0.15 dex. We find indications of a slightalpha-element overabundance of [alpha/Fe] ~ +0.1$ for WZ Oph. The secondarycomponent of AD Boo and both components of WZ Oph appear to be slightly active.Yale-Yonsai and Victoria-Regina evolutionary models fit the components of ADBoo and VZ Hya almost equally well, assuming coeval formation, at ages of about1.75/1.50 Gyr (AD Boo) and 1.25/1.00 Gyr (VZ Hya). BaSTI models, however,predict somewhat different ages for the primary and secondary components. ForWZ Oph, the models from all three grids are significantly hotter than observed.A low He content, decreased envelope convection coupled with surface activity,and/or higher interstellar absorption would remove the discrepancy, but itscause has not been definitively identified. We have demonstrated the power oftesting and comparing recent stellar evolutionary models using eclipsingbinaries, provided their abundances are known. The strongest limitations andchallenges are set by T_eff and interstellar absorption determinations, and bytheir effects on and correlation with abundance results.

astronomy and astrophysics

Absolute dimensions of eclipsing binaries. XXVI. Setting a new standard:  Masses, radii, and abundances for the F-type systems AD Bootis, VZ Hydrae,  and WZ Ophiuchi