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 present dense grids of stellar models suitable for comparison withobservable quantities measured with great precision, such as those derived frombinary systems or planet-hosting stars. We computed new Geneva models withoutrotation at metallicities Z=0.006, 0.01, 0.014, 0.02, 0.03 and 0.04 (i.e.[Fe/H] from -0.33 to +0.54) and with mass in small steps from 0.5 to 3.5 Msun.Great care was taken in the procedure for interpolating between tracks in orderto compute isochrones. Several properties of our grids are presented as afunction of stellar mass and metallicity. Those include surface properties inthe Hertzsprung-Russell diagram, internal properties including mean stellardensity, sizes of the convective cores, and global asteroseismic properties. Wechecked our interpolation procedure and compared interpolated tracks withcomputed tracks. The deviations are less than 1% in radius and effectivetemperatures for most of the cases considered. We also checked that the presentisochrones provide nice fits to four couples of observed detached binaries andto the observed sequences of the open clusters NGC 3532 and M67. Includingatomic diffusion in our models with M<1.1 Msun leads to variations in thesurface abundances that should be taken into account when comparing withobservational data of stars with measured metallicities. For that purpose,iso-Zsurf lines are computed. These can be requested for download from adedicated web page together with tracks at masses and metallicities within thelimits covered by the grids. The validity of the relations linking Z and FeH isalso re-assessed in light of the surface abundance variations in low-massstars.

Stellar mass and age determinations - I. Grids of stellar models from Z=0.006 to 0.04 and M=0.5 to 3.5 Msun