Astronomy and Astrophysics, volume 622A, 133-133 (2019/2-1)
Flares in open clusters with K2. I. M 45 (Pleiades), M 44 (Praesepe), and M 67.
ILIN E., SCHMIDT S.J., DAVENPORT J.R.A. and STRASSMEIER K.G.
Abstract (from CDS):
Context. The presence and strength of a stellar magnetic field and activity is rooted in a star's fundamental parameters such as mass and age. Can flares serve as an accurate stellar "clock"?
Aims. To explore if we can quantify an activity-age relation in the form of a flaring-age relation, we measured trends in the flaring rates and energies for stars with different masses and ages.
Methods. We investigated the time-domain photometry provided by Kepler's follow-up mission K2 and searched for flares in three solar metallicity open clusters with well-known ages, M 45 (0.125Gyr), M 44 (0.63Gyr), and M 67 (4.3Gyr). We updated and employed the automated flare finding and analysis pipeline Appaloosa, originally designed for Kepler. We introduced a synthetic flare injection and recovery sub-routine to ascribe detection and energy recovery rates for flares in a broad energy range for each light curve.
Results. We collect a sample of 1761 stars, mostly late-K to mid-M dwarfs and found 751 flare candidates with energies ranging from 4x1032erg to 6x1034erg, of which 596 belong to M 45, 155 to M 44, and none to M 67. We find that flaring activity depends both on Teff, and age. But all flare frequency distributions have similar slopes with α≥2.0-2.4, supporting a universal flare generation process. We discuss implications for the physical conditions under which flares occur, and how the sample's metallicity and multiplicity affect our results.
© ESO 2019
methods: data analysis - stars: activity - stars: flare - stars: low-mass
VizieR on-line data:
<Available at CDS (J/A+A/622/A133): allflare.dat alphabet.dat cparam.dat>
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