Hostname: page-component-586b7cd67f-tf8b9 Total loading time: 0 Render date: 2024-11-23T21:07:04.175Z Has data issue: false hasContentIssue false
  • English
  • Français

The Temperature and Continuum of the N Stars

Published online by Cambridge University Press:  25 April 2016

M. S. Bessell  and
Lee Youngbom
M. S. Bessell
Affiliation:
Mount Stromlo and Siding Spring Observatories The Australian National University
Lee Youngbom
Affiliation:
Mount Stromlo and Siding Spring Observatories The Australian National University
Get access Rights & Permissions [Opens in a new window]

Extract

On the basis of (R — I) colours it has been suggested that the N stars (the cool carbon stars) occupy a very restricted region in the Mb01 — log Te diagram (Te = 3300 to 3500 K) Mb01 ~ —3), falling on the normal giant sequence, but hotter than the M variables. This appeared somewhat puzzling in view of the variability of many of the carbon stars and their large range of periods, which suggested that the N stars ought perhaps to have similar temperatures to the variable M stars. In order to compare the continua of the M stars and N stars within the range of the R and I filters, and also to determine the continuum between the molecular bands, photometric observations were made of 20 M and N stars at carefully chosen wavelengths with 30Å resolution.

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 2 , Issue 3 , October 1972 , pp. 154 - 155
Copyright
Copyright © Astronomical Society of Australia 1972

Access options

Get access to the full version of this content by using one of the access options below. (Log in options will check for institutional or personal access. Content may require purchase if you do not have access.)

References

1 Eggen, O. J., Astrophys. J., 174, 45 (1972).Google Scholar
2 Wing, R., Ph.D. thesis, University of California Berkeley (1967).Google Scholar
3 Hyland, A. R., (private communication) (1972).Google Scholar
4 Hyland, A. R., and Gingold, R. A., Proc. A.S.A. 2, (1972).Google Scholar
5 Johnson, H. L., Ann. Rev. Ast. Ap., 4, 193 (1966).Google Scholar
6 Mendoza, E. E. V., and Johnson, H. L., Astrophys. J. 141, 161 (1965).CrossRefGoogle Scholar
7 Reeves, H. R., Stellar Evolution and Nucleosynthesis: Gordon and Breach, London, p. 41 (1968).Google Scholar