Flare event statistics on UV Ceti-type stars |
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| Authors: | K Ishida Mahasen Aputra K Ichimura Y Shimizu |
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| Institution: | (1) Institute of Astronomy, University of Tokyo, Mitaka, Tokyo, Japan;(2) Bosscha Observatory, Institut Teknologi Bandung, Lembang, West Java, Indonesia;(3) National Astronomical Observatory, Mitaka, Tokyo, Japan;(4) Okayama Astrophysical Observatory, National Astronomical Observatory, Kamogata, Okayama, Japan |
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| Abstract: | A statistical study of 228 flares on the three UV Ceti-type stars, i.e., YZ CMi, AD Leo, and EV Lac, is presented. Observations were gathered by Ichimura and Shimizu over a total monitoring time of 907 hours distributed over 18 years (1971 to 1988). Period analysis of flare activity was performed, and no periodicity was detected on the three stars for either the flare number rate or the energy rate in time-scales ranging from a year up to 14 years. Average colour of flares at peak was (U-B)=–0.98±0.17 and (B-V)=0.05±0.13. Cumulative number distributions of flare event time-integrated energies were solved by a least-squares method on a log-log plot for a power-law function to get both the constant of and the gradient  , which were found to be similar among the three stars. The gradient showed that rare large flare events radiate most of the energy released by all the flare events in the monitoring time. The flare number rate and energy rate are similar if the power-law distributions are extended up to a specific maximum energy. In reality, the Kolmogorov-Smirnov test showed that the observed cumulative number distributions of flare event energy were not necessarily a power-law function. The monte-Carlo simulation, however, indicates that the monitoring time and/or the patrol observation time interval may not be long enough to get the average flare number rate and energy rate, especially at the upper energy limits which are statistically unreliable. |
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