Hostname: page-component-848d4c4894-nmvwc Total loading time: 0 Render date: 2024-06-23T17:32:42.714Z Has data issue: false hasContentIssue false
  • English
  • Français

Two PopII Cepheids in the Globular Cluster M10

Published online by Cambridge University Press:  12 April 2016

C. Clement ,
H. Sawyer Hogg  and
K. Lake
C. Clement
Affiliation:
David Dunlap Observatory, Univ. of Toronto, Toronto M5S 1A7
H. Sawyer Hogg
Affiliation:
David Dunlap Observatory, Univ. of Toronto, Toronto M5S 1A7
K. Lake
Affiliation:
Dept. of Physics, Queen's University at Kingston, Ont.K7L 3N6

Extract

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.

The globular cluster Messier 10 has three known variables. The first two of these were discovered by one of us (Sawyer 1933) and the third by Arp (1955). Two of the variables, V2 (P=18.7226) and V3 (P=7.831), are population II cepheids while V1 appears to be an irregular variable. Another star which lies in the Schwarzschild gap on the horizontal branch is a suspected variable (Voroshilov 1971).

In this investigation, we examine the variations in the periods of the two cepheids over the interval 1912 to 1983 (for V2) and 1931 to 1983 (for V3). The study is based on photographs obtained with seven different telescopes - the Mt.Wilson 100-inch and 60-inch (1912 to 1919), the Dominion Astrophysical Observatory 72-inch, the David Dunlap 74-inch and 19-inch, the 16-inch at the University of Toronto downtown campus and the University of Toronto 24-inch at the Las Campanas Observatory of the Carnegie Institution of Washington. Some of our magnitudes have already been published (Sawyer 1938) and the remaining ones will be submitted to the Astronomical Journal for publication. We have also included material published by Arp (1955, 1957) in our study.

Type
Part IV. Population II Cepheids
Information
International Astronomical Union Colloquium , Volume 82: Cepheids: Theory and Observations , 1985 , pp. 260 - 261
Copyright
Copyright © Cambridge University Press 1985

References

Arp, H. C. (1955). Astron.J. 60, 1–17.CrossRefGoogle Scholar
Arp, H. C. (1957). Astron.J. 62, 129–36.10.1086/107483CrossRefGoogle Scholar
Clement, C. and Sawyer Hogg, H. (1977). J.Roy.Astron.Soc.Can.71, 281–97.Google Scholar
Norris, J. and Zinn, R. (1975). Astrophys.J. 202, 335–45.CrossRefGoogle Scholar
Sawyer, H. B. (1933). Pubi. Amer. Astron. Soc.7, 185–6.Google Scholar
Sawyer, H. B. (1938). David Dunlap Publ.1, 59–68.Google Scholar
Schwarzschild, M. and Harm, R. (1970). Astrophys.J. 160, 341.CrossRefGoogle Scholar
Strom, S. E.,Strom, K. M.,Rood, R. T.,and Iben, I. Jr. (1970). Astron. And Astrophys. 8, 243–50.Google Scholar
Voroshilov, Y. V. (1971). Astron.Circ. 623, 7–8.Google Scholar