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[vsnet-rr 30] Re: [vsnet 2128] SV Vul
Dear Mr. Ole Klinting,
I am a researcher of pulsating variable stars including classical
Cepheids, and visited your web site with a great interest.
There are some previous investigations and observations concerning
the period change of classical Cepheids including SV Vul itself.
Usually the period change observed in classical Cepheids are
interpreted as the result of the stellar evolution.
SV Vul is the important star because it is one of the star
near the longest end of the period distribution of the
galactic Cepheids. Here are some examples of investigations
related to the period change of classical Cepheids.
Period change of Cepheid variables:
Szabados, L. 1983, Astrophysics and Space Sciences, Vol. 96, 185.
Observations:
Szabados, L. 1977, Mitt. Sternw. ung. Akad., Budapest, No. 70.
Szabados, L. 1980, Mitt. Sternw. ung. Akad., Budapest, No. 76.
Szabados, L. 1981, Mitt. Sternw. ung. Akad., Budapest, No. 77.
On SV Vul:
Fernie, Demers and Marlborough, 1965, Astronomical Journal, vol. 70, 482.
Fernie, 1979, Astrophysical Journal, vol. 231, 841.
On period change and stellar evolution:
Fernie, 1984, in Observational Tests of the Stellar Evolution Theory,
IAU Symp., 105, p441.
On effect of metal abundance on period change:
Saitou, M. 1989, Astrophysics and Space Sciences, vol. 162, 47.
Period change of Cepheids in LMC:
Takeuti, M. and Saitou, M., 1990, in Confrontation between Stellar
Pulsation and Evolution, ASP Conf. Ser. 11, p232.
I'm afraid that it may be difficult for you to obtain some of the
above references. Actually, I also have no copy for some of the papers
above, partly because this research area is not strictly the same as mine.
Hopefully, you can find an interesting subject in these papers and
references therein.
Cordially,
---
% Toshihito ISHIDA, Ph. D., Astrophysicist e-mail: ishida@nhao.go.jp
% Nishi-Harima Astronomical Observatory, Sayo-cho, Hyogo 679-5313, JAPAN
% Tel: +81-790-82-3886 ext. 142 Telefax: +81-790-82-3514
vsnet-adm@kusastro.kyoto-u.ac.jp