Abstract
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
find 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 Prot. 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 (see Olmedo et al. 2013).
Original language | English |
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Journal | Search for Life Beyond the Solar System. Exoplanets, Biosignatures & Instruments |
Publication status | Published - 1 Mar 2014 |
Externally published | Yes |