EDP Sciences
Free access
Volume 429, Number 3, January III 2005
Page(s) 1051 - 1055
Section Stellar atmospheres
DOI http://dx.doi.org/10.1051/0004-6361:20041629

A&A 429, 1051-1055 (2005)
DOI: 10.1051/0004-6361:20041629

On the potassium-rotation connection in late-type Alpha Persei stars

E. L. Martín1, 2, A. Magazzù3, R. J. García López1, S. Randich4 and D. Barrado y Navascués5

1  Instituto de Astrofísica de Canarias, 38200 La Laguna, Spain
    e-mail: ege@iac.es
2  University of Central Florida, Department of Physics, PO Box 162385, Orlando, FL 32816-2385, USA
    e-mail: ege@physics.ucf.edu
3  Centro Galileo Galilei, Apartado 565, 38700 Santa Cruz de La Palma, Spain
    e-mail: magazzu@tng.iac.es
4  Osservatorio Astrofisico de Arcetri, Largo Fermi 5, 50125 Firenze, Italy
    e-mail: randich@arcetri.astro.it
5  Laboratorio de Astrofísica Espacial y Física Fundamental, INTA, Apartado Postal 50727, 28080 Madrid, Spain
    e-mail: barrado@laeff.esa.es

(Received 9 July 2004 / Accepted 14 September 2004 )

We present measurements of the $\ion{K}{i}$ $\lambda 7699$ line from spectra of 19 late-type members of the $\alpha$Persei cluster obtained with the Intermediate Dispersion Spectrograph at the Isaac Newton Telescope. These stars span a narrow range of Teff, from 5091 K to 4771 K, and a wide range of $v \sin i$ values (9 $\mathrm{km\,s}^{-1}$-170  $\mathrm{km\,s}^{-1}$). For a given star, we find empirically that larger rotational broadening apparently increases the equivalent width of $\ion{K}{i}$ $\lambda 7699$ linearly for $v \sin i$ values from 15 $\mathrm{km\,s}^{-1}$ to 75  $\mathrm{km\,s}^{-1}$. This correlation breaks down for $v \sin i >$ 75 $\mathrm{km\,s}^{-1}$. After correction for this effect, we show that the potassium line equivalent widths do not really correlate with $v \sin i$.

Key words: line: formation -- stars: atmospheres -- stars: abundances -- stars: activity -- stars: late-type -- Galaxy: open clusters and associations: alpha Per

SIMBAD Objects

© ESO 2005