Chemical abundances of solar neighbourhood RR Lyrae stars

We have analysed a sample of 18 RR Lyrae stars (17 fundamental-mode -- RRab -- and one first overtone -- RRc) and three Population II Cepheids (two BL Her stars and one W Vir star), for which high-resolution (R greater than or equal to 30 000), high signal-to-noise (S/N greater than or equal to 30) spectra were obtained with either SARG at the Telescopio Nazionale Galileo (La Palma, Spain) or UVES at the European Southern Observatory Very Large Telescope (Paranal, Chile). Archival data were also analysed for a few stars, sampling greater than or equal to 3 phases for each star. We obtained atmospheric parameters (T sub(eff), log g, v sub(t), and [M/H]) and abundances of several iron-peak and alpha -elements (Fe, Cr, Ni, Mg, Ca, Si, and Ti) for different pulsational phases, obtaining = +0.31 plus or minus 0.19 dex over the entire sample covering -2.2 < [Fe/H] < -1.1 dex. We find that silicon is indeed extremely sensitive to the phase, as reported by previous authors, and cannot be reliably determined. Apart from this, metallicities and abundance ratios are consistently determined, regardless of the phase, within 0.10-0.15 dex, although caution should be used in the range 0 less than or equal to phi less than or equal to 0.15. Our results agree with literature determinations for both variable and non-variable field stars, obtained with very different methods, including low- and high-resolution spectroscopy. W Vir and BL Her stars, at least in the sampled phases, appear indistinguishable from RRab from the spectroscopic analysis point of view. Our large sample, covering all pulsation phases, confirms that chemical abundances can be obtained for RR Lyrae with the classical equivalent-width -based technique and static model atmospheres, even rather close to the shock phases.