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GCVS Team
v sin i = 300 km/s; VB(0.3"; possibly also 0.05" - according to speckle-interferometric data). Shell spectrum appeared and disappeared several times since 1890. Different authors attributed the star to EB type. According to [E.H.Olsen, AsAp 20, 167, 1972.], The changes of light may be explained also by intrinsic variations of a single shell star. They are represented by elements: Min I = 2439470.628 + 1.0185d*E. According to [H.Schmidt, ZsAp 48, 249, 1959.], Min I = 2436174.430 + 1.5998398d*E. The periodogram analysis shows a stable peak at P ~0.84d [M.BossI, G.Guerrero, L.Mantegazza, AsAp Suppl 29, 327, 1977.]. A possible shell event was observed late in 1975.
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