Spectroscopic survey of Kepler stars - II. FIES/NOT observations of A- and F-type stars

被引：0

作者：

Niemczura E. ^{[1
]}

Polińska M. ^{[2
]}

Murphy S.J. ^{[3
,4
]}

Smalley B. ^{[5
]}

Kołaczkowski Z. ^{[1
]}

Jessen-Hansen J. ^{[6
]}

Uytterhoeven K. ^{[7
,8
]}

Lykke J.M. ^{[9
]}

Triviño Hage A. ^{[7
,8
]}

Michalska G. ^{[1
]}

机构：

[1] Instytut Astronomiczny, Uniwersytet Wroclawski, Kopernika 11, Wroclaw

[2] Astronomical Observatory Institute, Faculty of Physics, A. Mickiewicz University, Sloneczna 36, Poznań

[3] Sydney Institute for Astronomy (SIfA), School of Physics, University of Sydney, 2006, NSW

[4] Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Aarhus C

[5] Astrophysics Group, Keele University, Staffordshire

[6] Stellar Astrophysics Centre, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, Aarhus C

[7] Instituto de Astrofisica de Canarias, La Laguna, Tenerife

[8] Departamento de Astrofisica, Universidad de La Laguna, La Laguna, Tenerife

[9] Centre for Star and Planet Formation, Niels Bohr Institute and Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, Copenhagen K

来源：

| 1600年 / Oxford University Press卷 / 470期

关键词：

Stars: abundances; Stars: chemically peculiar; Stars: general; Stars: rotation;

D O I：

10.1093/MNRAS/STX1256

中图分类号：

学科分类号：

摘要：

We have analysed high-resolution spectra of 28 A and 22 F stars in the Kepler field, observed using the Fibre-Fed Échelle Spectrograph at the Nordic Optical Telescope.We provide spectral types, atmospheric parameters and chemical abundances for 50 stars.Balmer, Fe I and Fe II lines were used to derive effective temperatures, surface gravities and microturbulent velocities.We determined chemical abundances and projected rotational velocities using a spectrum synthesis technique. Effective temperatures calculated by spectral energy distribution fitting are in good agreement with those determined from the spectral line analysis. The stars analysed include chemically peculiar stars of the Am and λ Boo types, as well as stars with approximately solar chemical abundances. The wide distribution of projected rotational velocity, vsin i, is typical for A and F stars. The microturbulence velocities obtained are typical for stars in the observed temperature and surface gravity ranges. Moreover, we affirm the results of Niemczura et al. that Am stars do not have systematically higher microturbulent velocities than normal stars of the same temperature. © 2017 The Authors.

引用

页码：2870 / 2889

页数：19

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