dc.contributor.author Ivanyuk, Oleksiy M. dc.contributor.author Jenkins, James S. dc.contributor.author Pavlenko, Yakiv V. dc.contributor.author Jones, Hugh R. A. dc.contributor.author Pinfield, David J. dc.date.accessioned 2017-07-13T17:08:18Z dc.date.available 2017-07-13T17:08:18Z dc.date.issued 2017-07-01 dc.identifier.citation Ivanyuk , O M , Jenkins , J S , Pavlenko , Y V , Jones , H R A & Pinfield , D J 2017 , ' The metal rich abundance pattern - spectroscopic properties and abundances for 107 main-sequence stars ' , Monthly Notices of the Royal Astronomical Society , vol. 468 , no. 4 , pp. 4151-4169 . https://doi.org/10.1093/mnras/stx647 dc.identifier.issn 0035-8711 dc.identifier.other PURE: 11839923 dc.identifier.other PURE UUID: 53b41425-c4ce-439e-b745-8eb3b00361d8 dc.identifier.other ArXiv: http://arxiv.org/abs/1703.05077v1 dc.identifier.other ArXiv: http://arxiv.org/abs/1703.05077v1 dc.identifier.uri http://hdl.handle.net/2299/18934 dc.description This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society, ©: 2017 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. dc.description.abstract We report results from the high resolution spectral analysis of the 107 metal rich (mostly [Fe/H]$\ge$7.67 dex) target stars from the Calan-Hertfordshire Extrasolar Planet Search program observed with HARPS. Using our procedure of finding 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, and Zn, and we then compare them with known results from different authors. Most of our abundances agree with these works at the level of $\pm$0.05 dex or better for the stars we have in common. However, we do find systematic differences that make direct inferences difficult. Our analysis suggests that the selection of line lists and atomic line data along with the adopted continuum level influence these differences the most. At the same time, we confirm the positive trends of abundances versus metallicity for Na, Mn, Ni, and to a lesser degree, Al. A slight negative trend is observed for Ca, whereas Si and Cr tend to follow iron. Our analysis allows us to determine the positively skewed normal distribution of projected rotational velocities with a maximum peaking at 3 km s$^{-1}$. Finally, we obtained a Gaussian distribution of microturbulent velocities that has a maximum at 1.2 km s$^{-1}$ and a full width at half maximum $\Delta v_{1/2}=$0.35 km s$^{-1}$, indicating that metal rich dwarfs and subgiants in our sample have a very restricted range in microturbulent velocity. en dc.format.extent 19 dc.language.iso eng dc.relation.ispartof Monthly Notices of the Royal Astronomical Society dc.rights Open dc.subject astro-ph.SR dc.title The metal rich abundance pattern - spectroscopic properties and abundances for 107 main-sequence stars en dc.contributor.institution School of Physics, Astronomy and Mathematics dc.contributor.institution Centre for Astrophysics Research dc.description.status Peer reviewed dc.relation.school School of Physics, Astronomy and Mathematics dc.description.versiontype Final Published version dcterms.dateAccepted 2017-07-01 rioxxterms.version AM rioxxterms.version VoR rioxxterms.versionofrecord https://doi.org/10.1093/mnras/stx647 rioxxterms.type Journal Article/Review herts.preservation.rarelyaccessed true herts.rights.accesstype Open
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