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Astron. Astrophys. 334, 558-570 (1998)

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7. Other short periods?

Using various segments of photometric data prewhitened for variations on timescales of weeks and longer, I checked on the presence of periods in the range from 0 [FORMULA] 4 to 3 [FORMULA] 0. I found that the 1986-1987 observations by Balona et al. (1987) can indeed be best reconciled with a period of 1 [FORMULA] 4749 [FORMULA] 0 [FORMULA] 0029 and a semi-amplitude 0 [FORMULA] 0045 which is only about 1.5 times higher than the semi-amplitudes detected for the constant comparison stars. However, this periodicity cannot be detected in another subset, also from the same phase of strong emission (around HJD 2447900), where a period of 2 [FORMULA] 7428, reminiscent of the period advocated by Clarke (1990), is formally detected.

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© European Southern Observatory (ESO) 1998

Online publication: May 15, 1998

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