Analysis of TESS Data !1 Adina Feinstein NSF Graduate Research Fellow University of Chicago Benjamin Montet (UNSW), Megan Ansdell (NASA HQ), Brian Nord (UChicago/KICP/Fermi), Jacob Bean (UChicago), Maximillian Günther (MIT), Michael Gully-Santiago (UT Austin), Joshua Schlieder (NASA GSFC) @afeinstein20 March 306, 2020 ArXiv: 2005.07710 JOSS: 02347
al. (2020) as our training, validation, and test sets. See Max Günther’s iPoster 134.08 on flares in TESS Years 1 & 2! (Feinstein et al. 2020a,b) CNNs are available @ MAST
automated flare detection and does not require major light curve preprocessing. • M dwarfs have consistently high flare rates across the first 800 Myr, while hotter stars have fewer flares over time. at • M dwarfs with Teff < 3200 K have the highest normalized energy flares in the sample. • There is no phase dependence between flares and spot modulation, indicating consistent spot coverage on both hemispheres of these young stars. @afeinstein20 ArXiv: 2005.07710 JOSS: 02347