K2 Ultracool Dwarfs Survey. I. Photometry of an L Dwarf Superflare

• Published in: The Astrophysical journal Vol. 838; no. 1; pp. 22 - 27
• Main Authors: Gizis, John E., Paudel, Rishi R., Schmidt, Sarah J., Williams, Peter K. G., Burgasser, Adam J.
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 20-03-2017; IOP Publishing
• Subjects: Astrophysics; Bolometers; Cooling; Hydrogen; Light curve; Photometry; Photosphere; stars: activity; stars: chromospheres; stars: flare; stars: individual (SDSSp J005406.55-003101.8); stars: low-mass; Stellar flares; Time constant; White light
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/aa6197

We report on K2 Campaign 8 measurements of a huge white light flare on the L1 dwarf SDSSp J005406.55-003101.8 (EPIC 220186653). The source is a typical L1 dwarf at a distance of ∼50 pc, probably an old hydrogen-burning star rather than a young brown dwarf. In the long (30-minute) cadence photometry, the flare peak is 21 times the flux of the stellar photosphere in the broad optical Kepler filter, which we estimate corresponds to ΔV −7.1. The total equivalent duration of the flare is 15.4 hr. We estimate that the total bolometric energy of the flare was 4 × 1033 erg, more powerful than the previously reported Kepler white light flares for the L1 dwarf WISEP J190648.47+401106.8, but weaker than the ΔV = −11 L0 dwarf superflare ASASSN-16ae. The initial (impulsive) cooling phase is too rapid to resolve with our 30-minute cadence data, but after 1 hour the gradual cooling phase has an exponential time constant of 1.8 hr. We use template fitting to estimate that the full time-width-at-half-amplitude of the light curve is <10 minutes and that the true flare maximum reached ∼70 times the stellar photosphere, or ΔV −8. This flare is comparable to the most powerful Kepler flares observed on the active M4 dwarf GJ 1243.