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.
|Journal||Publications of the Astronomical Society of the Pacific|
|Publication status||Published - 1 Dec 2013|
Olmedo, M., Chávez, M., Bertone, E., & De la Luz, V. (2013). Mg II h + k Flux—Rotational Period Correlation for G-type Stars. Publications of the Astronomical Society of the Pacific, 125(934), 1436. https://doi.org/10.1086/674332