Hostname: page-component-77c89778f8-gq7q9 Total loading time: 0 Render date: 2024-07-23T20:12:51.814Z Has data issue: false hasContentIssue false
  • English
  • Français

Infrared Photometry of Be Stars

Published online by Cambridge University Press:  14 August 2015

Alejandro Feinstein
Alejandro Feinstein*
Affiliation:
Observatorio Astronómico, Universidad Nacional de La Plata, 1900 La Plata, Argentina

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.

A photometric study of Be stars in the JHKL system is reported here. Early papers (see Feinstein and Marraco, 1980) about bright southern Be stars observed photoelectrically in the UBVRI system and in the Balmer-lines: Hα, Hβ and Hγ, permit us to derive several conclusions about their light variability, the amount of emission in the α and β indices, and some correlations about these data. On the other hand, we recently found (Feinstein and Marraco, 1981) that the emission strengths of the hydrogen lines are well correlated to the amount of excess radiation in the near-in-frared of the RI system.

Type
IV. Infrared Observations
Information
Symposium - International Astronomical Union , Volume 98: Be Stars , 1982 , pp. 235 - 240
Copyright
Copyright © Reidel 1982 

References

Allen, D. A. 1973, Mon. Not. R. astr. Soc. 161, 145.CrossRefGoogle Scholar
Feinstein, A. and Marraco, H.G. 1980, Astron. J. 84, 1713.CrossRefGoogle Scholar
Feinstein, A. and Marraco, H.G. 1981, Publ. Astron. Soc. Pacific, in press.Google Scholar
Glass, I.S. 1974, Mon. Notes R. Astr. Soc. Sth. Afr. 33, 53.Google Scholar
Whittet, D. C. B. and van Breda, I. G. 1980, Mon. Not. R. astr. Soc. 192, 467.Google Scholar