On the long-term correlation between the flux in the Ca II H & K and Halpha lines for FGK stars

Abstract

The re-emission in the cores of the Ca II H & K and H$\alpha$ lines, are well known proxies of stellar activity. However, these activity indices probe different activity phenomena, the first being more sensitive to plage variation, while the other one being more sensitive to filaments. In this paper we study the long-term correlation between $\log R_{HK}^{\prime }$ and $\log I_{H\alpha }$, two indices based on the Ca II H & K and H$\alpha$ lines respectively, for a sample of 271 FGK stars using measurements obtained over a $\sim$9 year time span. Because stellar activity is one of the main obstacles to the detection of low-mass and long-period planets, understanding further this activity index correlation can give us some hints about the optimal target to focus on, and ways to correct for these activity effects. We found a great variety of long-term correlations between $\log R_{HK}^{\prime }$ and $\log I_{H\alpha }$. Around 20% of our sample has strong positive correlation between the indices while about 3% show strong negative correlation. These fractions are compatible with those found for the case of early-M dwarfs. Stars exhibiting a positive correlation have a tendency to be more active when compared to the median of the sample, while stars showing a negative correlation are more present among higher metallicity stars. There is also a tendency for the positively correlated stars to be more present among the coolest stars, a result which is probably due to the activity level effect on the correlation. Activity level and metallicity seem therefore to be playing a role on the correlation between $\log R_{HK}^{\prime }$ and $\log I_{H\alpha }$. Possible explanations based on the influence of filaments for the diversity in the correlations between these indices are discussed in this paper.

18 pages, 13 figures, 4 tables, accepted for publication in Astronomy and Astrophysics

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