The variation of the Hβ emissions of YY Gem has been monitored for the period of 1978 - 1984. The short-time scale quasi-periodic variation of an amplitude up to a factor two is interpreted as the result of rotation modulation of double, quadruple, or higher-order sectorial structures of active longitude, where the coronal and chromospheric Hβ emission is intensified. The long-term variation of the mean intensity of Hβ emission remained less than by a factor two within the past seven years. The sectorial structures seem to be subject to temporal variations with a time-scale of a few months.
Flare Stars and Related Objects
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