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Linear Pulsation Periods of the Post-AGB Stars

Published online by Cambridge University Press:  07 August 2017

M. Takeuti ,
R. Takano  and
S. Tamura
M. Takeuti
Affiliation:
Astronomical Institute, Tôhoku University, Sendai, Japan
R. Takano
Affiliation:
Astronomical Institute, Tôhoku University, Sendai, Japan
S. Tamura
Affiliation:
Astronomical Institute, Tôhoku University, Sendai, Japan

Extract

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There may exist stars during and just after the asymptotic giant branch (AGB) stage. V441 (89) is a candidate star. Fernie and Sasselov (1989) have discussed the evolutionary changes of the pulsation periods based on those of the effective temperature, to compare those with observational data. They used Worell's theorical results (Worell 1986) and have found that the observational changes of the period and the colors are too small compared with the theorical values. To examine the effect of opacities on the pulsations periods, we calculate the periods based on new opacities (OPAL, Iglesias and Rogers 1991), and compare them with the data reported previously.

Type
IV. Planetary Nebulae Connection: Evolution from the AGB
Information
Symposium - International Astronomical Union , Volume 155: Planetary Nebulae , 1993 , pp. 366
Copyright
Copyright © Kluwer 1993 

References

Fernie, J.D. 1991, PASP, 105, 1087 Google Scholar
Fernie, J.D. and Sasselov, D.D. 1989, PASP, 101, 513 Google Scholar
Iglesias, C.A. and Rogers, F.J. 1991, Ap. J., 371, L73 Google Scholar
Worell, J.K. 1986 M.N.R.A.S., 223, 787 Google Scholar