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Rapid variability of Hα emission line in Be stars

Published online by Cambridge University Press:  26 May 2016

B. G. Anandarao ,
A. Chakraborty ,
R. Swaminathan  and
B. Lokanadham
B. G. Anandarao
Affiliation:
Physical Research Laboratory, Ahmedabad - 380009, India
A. Chakraborty
Affiliation:
Physical Research Laboratory, Ahmedabad - 380009, India
R. Swaminathan
Affiliation:
Osmania University, Hyderabad - 500007, India
B. Lokanadham
Affiliation:
Osmania University, Hyderabad - 500007, India

Extract

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We have initiated an observational campaign on some bright Be stars in order to investigate the rapid variability in emission lines using a Fabry-Perot spectrometer(λ/δλ = 104; FSR = 21.3Å) at the Nasmyth focus of the 1.22 m JRO telescope at Hyderabad, India. The PMT dark counts were 1 – 2sec-1. Here we report our first observations on four stars.

Type
5. Be Stars: Spectroscopy and Photometry
Information
Symposium - International Astronomical Union , Volume 162: Pulsation, Rotation and Mass Loss in Early-Type Stars , 1994 , pp. 254 - 256
Copyright
Copyright © Kluwer 1994 

References

Baade, D., Vol.36, 59.Google Scholar
Hanuschik, R.W. et al, 1993, A&A, 274, 356.Google Scholar
Smith, M.A., 1991, in ESO Workshop on Rapid Variability of OB stars, Ed.Google Scholar