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Simultaneous Multiwavelength Flare Observations of EV Lacertae

2021; IOP Publishing; Volume: 922; Issue: 1 Linguagem: Inglês

10.3847/1538-4357/ac1946

1538-4357

Rishi R. Paudel, Thomas Barclay, Joshua E. Schlieder, Elisa V. Quintana, Emily A. Gilbert, Laura D. Vega, Allison Youngblood, Michele L. Silverstein, Rachel A. Osten, M. A. Tucker, Daniel Huber, A. Do, Kenji Hamaguchi, D. J. Mullan, John E. Gizis, Teresa Monsue, Knicole D. Colón, Patricia T. Boyd, James R. A. Davenport, Lucianne M. Walkowicz,

Stellar, planetary, and galactic studies

Abstract We present the first results of our ongoing project conducting simultaneous multiwavelength observations of flares on nearby active M dwarfs. We acquired data of the nearby dM3.5e star EV Lac using five different observatories: NASA’s Transiting Exoplanet Survey Satellite (TESS), NASA’s Neil Gehrels Swift Observatory (Swift), NASA’s Neutron Interior Composition Explorer (NICER), the University of Hawaii 2.2-meter telescope (UH88), and the Las Cumbres Observatory Global Telescope (LCOGT) Network. During the ∼25 days of TESS observations, we acquired three simultaneous UV/X-ray observations using Swift that total ∼18 ks, 21 simultaneous epochs totaling ∼98 ks of X-ray data using NICER, one observation (∼3 hr) with UH88, and one observation (∼3 hr) with LCOGT. We identified 56 flares in the TESS light curve with estimated energies in the range log E T (erg) = (30.5–33.2), nine flares in the Swift UVM2 light curve with estimated energies in the range log E UV (erg) = (29.3–31.1), 14 flares in the NICER light curve with estimated minimum energies in the range log E N (erg) = (30.5–32.3), and 1 flare in the LCOGT light curve with log E L (erg) = 31.6. We find that the flare frequency distributions (FFDs) of TESS and NICER flares have comparable slopes, β T = −0.67 ± 0.09 and β N = − 0.65 ± 0.19, and the FFD of UVOT flares has a shallower slope ( β U = −0.38 ± 0.13). Furthermore, we do not find conclusive evidence for either the first ionization potential (FIP) or the inverse FIP effect during coronal flares on EV Lac.