Hostname: page-component-78c5997874-v9fdk Total loading time: 0 Render date: 2024-11-19T01:17:50.210Z Has data issue: false hasContentIssue false
  • English
  • Français

A Generalization of the Cors Method to Determine Cepheid Radii: Theory and Application

Published online by Cambridge University Press:  12 April 2016

B. Caccin ,
B. Buonaura ,
A. Onnembo ,
G. Russo ,
A. M. Sambuco  and
C. Sollazzo
B. Caccin
Affiliation:
Istituto di Fisica Sperimentale dell‘Universita’, Pad. 20 Mostra d’Oltremare, 80125 Napoli, Italy
B. Buonaura
Affiliation:
Istituto di Fisica Sperimentale dell‘Universita’, Pad. 20 Mostra d’Oltremare, 80125 Napoli, Italy
A. Onnembo
Affiliation:
Istituto di Fisica Sperimentale dell‘Universita’, Pad. 20 Mostra d’Oltremare, 80125 Napoli, Italy
G. Russo
Affiliation:
Osservatorio Astronomico di Capodimonte, via Moiariello 16, 80131 Napoli, Italy
A. M. Sambuco
Affiliation:
Consiglio Nazionale delle Ricerche, Roma, Italy
C. Sollazzo
Affiliation:
Physics Department, University of Victoria, Canada and Osservatorio Astrofisico, Catania, Italy

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.

The CORS method for the empirical determination of the radii of pulsating variables (Caccin et al., 1981; Sollazzo et al., 1981) is discussed in the framework of the quasistatlc approximation to the variations of the atmospheric parameters (Unno, 1965) and reformulated in a way that does not make direct use of theoretical calibrations of the photometric system in terms of model atmospheres. The radii calculated with this approach are in good agreement with those previously obtained by means of Pel's calibrations of the VBLUW system (Sollazzo et al.,1981) which lead to a period-radius relation coinciding, within the errors, with the theoretical one (Cogan, 1978) and, consequently, mass determinations consistent with pulsational masses (Cox, 1979). The method can be immediately applied to any other multicolour system, and very promising preliminary results are obtained by using recent UBV data by Gieren (1982).

Type
Part I. Fundamental Parameters
Information
International Astronomical Union Colloquium , Volume 82: Cepheids: Theory and Observations , 1985 , pp. 43 - 47
Copyright
Copyright © Cambridge University Press 1985

References

Caccin, B., Onnembo, A., Russo, G., Sollazzo, C. (1981), Astron. Astrophys. 97, 104 Google Scholar
Cogan, B. C. (1978), Astrophys. J. 221, 635 CrossRefGoogle Scholar
Cox, A. N. (1979), Astrophys. J. 229, 212 CrossRefGoogle Scholar
Gieren, W. (1982), Astrophys. J. Suppl. 49, 1 CrossRefGoogle Scholar
Ledoux, P., Whitney, C. (1961), IAU Symp. No. 12, ed Thomas, R. N. (Balogna) P. 131 Google Scholar
Onnembo, A., Buonaura, B., Caccin, B., Russo, G., Sambuco, A. M., Sollazzo, C. (1984), submittedGoogle Scholar
Pel, J. W. (1976), Astron. Astrophys. Suppl. 24, 413 Google Scholar
Pel, J. W. (1978), Astron. Astrophys. 62, 75 Google Scholar
Sollazzo, C., Russo, G., Onnembo, A., Caccin, B. (1981), Astron. Astrophys. 99, 66 Google Scholar
Unno, W. (1965), Pub. Astron. Soc. Japan 17, 205 Google Scholar