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The Be Phenomenon in Pleione

  • Ryuko Hirata (a1), Michihiro R. Shimada (a1), Seiji Masuda (a1) and Jun-ichi Katahira (a2)

Abstract

The spectral change of Pleione in the present Be phase (1988-1999) is briefly described. The Hα emission reached its maximum in 1995-1999. The V/R values of Hγ and metallic lines changed from V/R < 1 in 1995 to V/R > 1 in 1998-1999. The broad component of Mg II λ4481 line further weakened in Be phase.

The long-term variation in 1968-1999 is shown for several observational quantities. These quantities which reflect various levels from the photosphere up to the outer envelope did not change in a parallel way. The basic unsolved problems are pointed out.

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References

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Hirata, R. 1995, PASJ 47, 195
Hirata, R., Okazaki, A.T. 2000, this colloquium
Limber, D.N. 1969, ApJ 157, 785
Peters, G.J. 1976, in IAU Symp. 70, Be and Shell Stars, Slettebak, A., Ed., Reidel, Dordrecht, p.69
Sharov, A.S., Lyutyi, V.M. 1997, Astronomy Letters 23, 93

The Be Phenomenon in Pleione

  • Ryuko Hirata (a1), Michihiro R. Shimada (a1), Seiji Masuda (a1) and Jun-ichi Katahira (a2)

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