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Is HR 9070 Really Pulsating?

Published online by Cambridge University Press:  23 September 2016

Sareyan J.P. ,
Alvarez M. ,
Chauville J. ,
Le Contel J.M. ,
Michel R.  and
Ballereau D.
Sareyan J.P.
Affiliation:
Observatoire de Nice, B.P.139, 06003 Nice Cedex, France
Alvarez M.
Affiliation:
Observatorio Astronomico Nacional, UNAM Apartado Postal 877, 22800 Ensenada, B.C., Mexico
Chauville J.
Affiliation:
Observatoire de Meudon, 92195 MEUDON Principal Cedex, France
Le Contel J.M.
Affiliation:
Observatoire de Nice, B.P.139, 06003 Nice Cedex, France
Michel R.
Affiliation:
Observatorio Astronomico Nacional, UNAM Apartado Postal 877, 22800 Ensenada, B.C., Mexico
Ballereau D.
Affiliation:
Observatoire de Meudon, 92195 MEUDON Principal Cedex, France

Extract

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As Be stars and classical β CMa variables both have a distribution peak at B2, one can wonder if there is a connection between these two phenomena. A way to solve this problem could be to carry out a systematic survey of emission on short periodic B variables,over months and years.

Another way, chosen by our grouns in Nice, Ensenada and Meudon, is to improve time resolution in photometric and spectrographic observations on the Be stars already known to have short time scale variations. Special attention is paid to longitude cooperation, essential to detect or measure longer time constants.

Type
IIA. The Underlying Stars: Observations
Information
International Astronomical Union Colloquium , Volume 92: Physics of Be Stars , August 1987 , pp. 78 - 81
Copyright
Copyright © Cambridge University Press 1987

References

Harmanec, P.(1984). Bull.Astron.Inst. Czechosl. 35, 193.Google Scholar
Percy, J.R.(1983). Astron.J. 88, 427.CrossRefGoogle Scholar