Predicted and Empirical Radii of RR Lyrae Stars

Abstract

We present new theoretical period-radius-metallicity relations for RR Lyrae stars. Current predictions are based on a large set of nonlinear, convective models that cover a broad range of chemical abundances and input parameters. We also provide new and homogeneous estimates of angular diameters for a sample of field RR Lyrae stars using a recent calibration of the Barnes-Evans surface brightness relation. Predicted and empirical radii are, within the errors, in reasonable agreement, but in the short-period range the latter present a larger scatter. As a working hypothesis we suggest that this discrepancy might be due to the occurrence either of nonlinear features such as bumps or a steep rising branch. A new distance determination for RR Lyr itself is in very good agreement with the Hubble Space Telescope trigonometric parallax and with the pulsation parallax.