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Stellar flares detected with the Next Generation Transit Survey

Authors :: James A. G. Jackman
Jack S. Acton
Michael R. Goad
Rosanna H. Tilbrook
Didier Queloz
Edward Gillen
Sarah L. Casewell
Boris T. Gänsicke
Samuel Gill
Simon Hodgkin
Maximilian N. Günther
David R. Anderson
Richard G. West
Liam Raynard
Beth A. Henderson
Joshua T. Briegal
Chloe E. Pugh
Daniel Bayliss
Matthew R. Burleigh
James S. Jenkins
Peter J. Wheatley
Christopher A. Watson
Queloz, Didier [0000-0002-3012-0316]
Apollo - University of Cambridge Repository
Source :: Jackman, J A G, Wheatley, P J, Acton, J S, Anderson, D R, Bayliss, D, Briegal, J T, Burleigh, M R, Casewell, S L, Gänsicke, B T, Gill, S, Gillen, E, Goad, M R, Günther, M N, Henderson, B A, Hodgkin, S T, Jenkins, J S, Pugh, C, Queloz, D, Raynard, L, Tilbrook, R H, Watson, C A & West, R G 2021, ' Stellar flares detected with the Next Generation Transit Survey ', Monthly Notices of the Royal Astronomical Society, vol. 504, no. 3, pp. 3246-3264 . https://doi.org/10.1093/mnras/stab979
Publication Year :: 2021
Publisher :: Oxford University Press (OUP), 2021.
Abstract: We present the results of a search for stellar flares in the first data release from the Next Generation Transit Survey (NGTS). We have found 610 flares from 339 stars, with spectral types between F8 and M6, the majority of which belong to the Galactic thin disc. We have used the 13 second cadence NGTS lightcurves to measure flare properties such as the flare amplitude, duration and bolometric energy. We have measured the average flare occurrence rates of K and early to mid M stars and present a generalised method to measure these rates while accounting for changing detection sensitivities. We find that field age K and early M stars show similar flare behaviour, while fully convective M stars exhibit increased white-light flaring activity, which we attribute to their increased spin down time. We have also studied the average flare rates of pre-main sequence K and M stars, showing they exhibit increased flare activity relative to their main sequence counterparts.<br />21 pages, 13 figures, 5 tables. Accepted for publication in the Monthly Notices of the Royal Astronomical Society