We present an analysis of the correlation between the mid-UV Mg II h and k emission lines and measured rotational periods of G-type stars. Based on IUE and HST high resolution spectra of a sample of 36 stars, we derive an exponential function that best represents the correlation. We found that the variation of the Mg II h + k fluxes is about a factor of 2.5 larger than that of Ca II H+K, indicating that the UV features are more sensitive to the decline of rotational period. The comparison of UV-predicted rotational periods with those derived from empirical Prot - Ca II H+K flux calibrations are consistent, with some scatter at large periods, where the emission are less intense. We present newly derived rotational periods for 15 G-type stars.
@article{arxiv.1310.3890,
title = {Mg II h+k Flux - Rotational Period Correlation for G-type stars},
author = {Manuel Olmedo and Miguel Chávez and Emanuele Bertone and Víctor De la Luz},
journal= {arXiv preprint arXiv:1310.3890},
year = {2015}
}
Comments
9 pages, 5 figures, 4 tables. Accepted for publication in PASP (corrected references)