Abstract
ABSTRACT We present the detection of high-energy white-light flares from pre-main-sequence stars associated with the Orion Complex, observed as part of the Next Generation Transit Survey (NGTS). With energies up to 5.2 × 1035 erg these flares are some of the most energetic white-light flare events seen to date. We have used the NGTS observations of flaring and non-flaring stars to measure the average flare occurrence rate for 4 Myr M0–M3 stars. We have also combined our results with those from previous studies to predict average rates for flares above 1 × 1035 erg for early M stars in nearby young associations.
Highlights
The pre-main sequence represents the most active period in a star’s lifetime, something reflected in their lightcurves
We present the detection of high energy white-light flares from pre-main sequence stars associated with the Orion complex, observed as part of the Generation Transit Survey (NGTS)
From an analysis of 83 stars associated with the Orion complex which were observed with Next Generation Transit Survey (NGTS) we detected 26 flares from 17 stars. 16 of these 17 flare stars had effective temperatures from our Spectral Energy Distribution (SED) fits or the Kounkel et al (2018) sample, which corresponded to spectral types between G3 and M3
Summary
The pre-main sequence represents the most active period in a star’s lifetime, something reflected in their lightcurves. Studies of open clusters and associations of known ages have shown this occurs in a mass-dependent fashion, with higher mass stars spinning down first (e.g. Epstein & Pinsonneault 2014; Matt et al 2015; Douglas et al 2019) This spin down is expected to affect the internal dynamo weakening it and the magnetic field it generates. In this work we report the detection of white-light flares from pre-main sequence stars in the Orion Complex with the Generation Transit Survey (NGTS) These stars have a weighted average age of 4.0 ± 0.2 Myr (Kounkel et al 2018). We compare our occurrence rates to those of Pleiades and Praesepe from Ilin et al (2019) and predict upper limits on flare occurrence rates for nearby young associations
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