Multi-wavelength Monitoring of Stellar Flares in the Active Eclipsing Binary CU Cancri
Authors/Creators
- 1. College of Physics, Guizhou University, Guiyang 550025, People's Republic of China
- 2. State Key Laboratory of Public Big Data \& Guizhou Radio Astronomical Observatory, Guizhou University, Guiyang 550025, PR China
- 3. Department of Physics and Astronomy and SARA, Butler University, Indianapolis, IN 46208, USA
- 4. School of Earth and Space Sciences, Peking University, Beijing 100871, PR China
- 5. ASTRON, Netherlands Institute for Radio Astronomy, 7991~PD Dwingeloo, The Netherlands
- 6. Kapteyn Astronomical Institute, University of Groningen, 9700~AV Groningen, The Netherlands
- 7. National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, PR China
Description
CU Cancri_85cm_UBV.csv——Log of UBV-band photometric observations of CU~Cnc obtained with the 85-cm telescope at Xinglong Observatory.Columns are:
(1) file name of the U-band image; (2) observation time in UTC for the U band;
(3) normalised flux in the U band; (4) uncertainty of the normalised U-band flux;
(5) file name of the B-band image; (6) observation time in UTC for the B band;
(7) normalised flux in the B band; (8) uncertainty of the normalised B-band flux;
(9) file name of the V-band image; (10) observation time in UTC for the V band;
(11) normalised flux in the V band; and (12) uncertainty of the normalised V-band flux.
Flares_Parameters.csv——This table summarises the parameters of 532 flare events detected on CU Cancri. Columns are:
(1) event index; (2)–(3) flare start and end times. All flares were detected in Kepler/K2 data and are given in Kepler spacecraft time (BKJD = BJDTDB − 2454833), in units of days. Flares 1–520 were identified from the short-cadence data, whereas flares 521–532 were identified from the long-cadence data. (4) equivalent duration (ED), in seconds; (5) flare amplitude, in relative flux units; (6) flare duration, in days; and (7) estimated bolometric flare energy, in erg. For the long-cadence flares (Nos 521–532), bolometric flare energies were not calculated, and the corresponding entries in column (7) are therefore left blank.