Hostname: page-component-cd9895bd7-7cvxr Total loading time: 0 Render date: 2024-12-23T19:07:41.150Z Has data issue: false hasContentIssue false
  • English
  • Français

On the Structure of the Cepheid Instability Strip

Published online by Cambridge University Press:  14 August 2015

N. N. Yakimova ,
N. S. Nikolov  and
G. R. Ivanov
N. N. Yakimova
Affiliation:
Sternberg Astronomical Institute, Moscow, U.S.S.R.
N. S. Nikolov
Affiliation:
Sternberg Astronomical Institute, Moscow, U.S.S.R.
G. R. Ivanov
Affiliation:
Dept. of Astronomy, Bulgarian Academy of Sciences and University of Sofia, Bulgaria

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Using rich photometric material on the Cepheids in the Galaxy and the Large and Small Magellanic Clouds, the structure of the instability strip in the HR diagram is investigated. The method of the δ-δ diagrams is used, δ being the difference of certain Cepheid characteristics from the means for a given period. The Cepheids in the three galaxies, studied separately, show the same relationship: the light amplitude increases toward the low temperature limit of the instability strip and is also related with the temperature at maximum in the sense that Cepheids with a given period and fixed mean temperature have a greater light amplitude for a higher temperature at maximum. Our results do not coincide with those by Sandage and Tammann, probably because they have studied the Cepheids in the different star systems as one single complex.

Type
Part 3 / Type I (Classical) Cepheids
Information
Symposium - International Astronomical Union , Volume 67: Variable Stars and Stellar Evolution , 1975 , pp. 201 - 222
Copyright
Copyright © Reidel 1975 

References

Arp, H. C.: 1960, Astron. J. 65, 404.Google Scholar
Fernie, J. D.: 1963, Astron. J. 68, 280.Google Scholar
Fernie, J. D.: 1970, Astrophys. J. 161, 679.Google Scholar
Gascoigne, S. C. B.: 1969, Monthly Notices Roy. Astron. Soc. 146, 1.Google Scholar
Genderen van, A. M.: 1969, Bull. Astron. Inst. Neth. Suppl. 3, 221.Google Scholar
Gusseva, N. N. and Tsarevsky, G. S.: 1968, Peremen. Zvezdy 16, 292.Google Scholar
Irwin, I. B.: 1961, Astrophys. J. Suppl. 6, 253.Google Scholar
Ivanov, G. R.: 1974, Dissertation, University of Sofia.Google Scholar
Kraft, R. P.: 1960, Astrophys. J. 131, 330.Google Scholar
Kraft, R. P.: 1961, Astrophys. J. 134, 616.Google Scholar
Kron, G. E. and Svolopoulos, S. N.: 1959, Publ. Astron. Soc. Pacific 71, 126.Google Scholar
Kurochkin, N. E.: 1966, Peremen. Zvezdy 16, 10.Google Scholar
Mianes, P.: 1963, Ann. Astrophys. 26, 1.Google Scholar
Nikolov, N. S.: 1966, Astron. Zh. 43, 785 = Soviet Astron. A. J. 10, 623.Google Scholar
Nikolov, N. S. and Ivanov, G. R.: 1973a, Astron. Zh. 51, 132.Google Scholar
Nikolov, N. S. and Ivanov, G. R.: 1973b, Peremen. Zvezdy 19, 207.Google Scholar
Nikolov, N. S., Kunchev, P. Z., and Ivanov, G. R.: 1973, Bull. Sec. Astron. Bulg. Acad. Sci. 6, 61.Google Scholar
Oke, J. B.: 1961, Astrophys. J. 134, 314.Google Scholar
Sandage, A.: 1958, Astrophys. J. 127, 513.Google Scholar
Sandage, A. and Tammann, G. A.: 1971, Astrophys. J. 167, 293.Google Scholar
Schmidt, E. G.: 1971, Astrophys. J. 165, 335.Google Scholar
Tsarevsky, G. S. and Yakimova, N. N.: 1970, Peremen. Zvezdy 17, 120.Google Scholar
Williams, J. A.: 1966, Astron. J. 71, 615.Google Scholar
Woolley, R. v. d. R., Sandage, A. R., Eggen, O. J., Alexander, J. B., Mather, L., Epps, E., and Jones, S.: 1962, Roy. Observ. Bull. 58, 31.Google Scholar
Yakimova, N. N.: 1970a, Peremen. Zvezdy 17, 253.Google Scholar
Yakimova, N. N.: 1970b, Astron. Circ., No. 594, 3.Google Scholar
Yakimova, N. N.: 1971, Astron. Zh. 48, 1265 = Soviet Astron. A. J. 15, 1006.Google Scholar
Yakimova, N. N.: 1972a, Sternberg Inst. Comm. 177, 19.Google Scholar
Yakimova, N. N.: 1972b, Astron. Zh. 49, 514.Google Scholar