Simultaneous radio and optical observations of UV Ceti-type flare stars
The UV Ceti-type stars, YZ Canis Minoris, AD Leonis, and Wolf 524 AB, were monitored for 57.8 hours in the time interval 1974 January 15 to February 22 using the 1000 foot (305 m) radio telescope at Arecibo, Puerto Rico, and the 91 or 76 cm reflector at McDonald Obervatory of the University of Texas. Radio observations were made at frequencies of 430, 318, and 196 MHz, and optical monitoring was done in the Johnson U or B band, the Stromgren u band, or white light. During the period of simultanous observations, 62 optical flares were detected. A total of 13 radio frequency flares were independently identified, of which 10 reached maximum flux within 10 min of the peak time of an optical flare. Using times of optical flare events as reference data, we identified an additional 15 cases of radio enhancements associated with optical flares. The most probable delay interval between the optical flare maximum and 318 MHz radio peak was found to be 0 to 5 min with the optical flare occurring first. Aside from this statistical delay of peak occurrence and a general tendency for radio and optical flares to be associated, no systematic correlations of optical and radio amplitudes or morphology were found. The possible consequences of the radio emission being due to a coherent process are discussed. (AIP)
- Research Organization:
- Department of Physics and Astronomy, University of Iowa
- OSTI ID:
- 7194990
- Journal Information:
- Astrophys. J.; (United States), Vol. 203:2
- Country of Publication:
- United States
- Language:
- English
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