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 report results from the high resolution spectral analysis of the 107 metalrich (mostly [Fe/H]$\ge$7.67 dex) target stars from the Calan-HertfordshireExtrasolar Planet Search program observed with HARPS. Using our procedure offinding the best fit to the absorption line profiles in the observed spectra,we measure the abundances of Na, Mg, Al, Si, Ca, Ti, Cr, Mn, Fe, Ni, Cu, andZn, and we then compare them with known results from different authors. Most ofour abundances agree with these works at the level of $\pm$0.05 dex or betterfor the stars we have in common. However, we do find systematic differencesthat make direct inferences difficult. Our analysis suggests that the selectionof line lists and atomic line data along with the adopted continuum levelinfluence these differences the most. At the same time, we confirm the positivetrends of abundances versus metallicity for Na, Mn, Ni, and to a lesser degree,Al. A slight negative trend is observed for Ca, whereas Si and Cr tend tofollow iron. Our analysis allows us to determine the positively skewed normaldistribution of projected rotational velocities with a maximum peaking at 3 kms$^{-1}$. Finally, we obtained a Gaussian distribution of microturbulentvelocities that has a maximum at 1.2 km s$^{-1}$ and a full width at halfmaximum $\Delta v_{1/2}=$0.35 km s$^{-1}$, indicating that metal rich dwarfsand subgiants in our sample have a very restricted range in microturbulentvelocity.

The metal rich abundance pattern - spectroscopic properties and abundances for 107 main-sequence stars