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The radius and the pulsation constant of the primary of Spica*

Published online by Cambridge University Press:  03 August 2017

M. Jerzykiewicz  and
C. Sterken
M. Jerzykiewicz
Affiliation:
Wroclaw University Observatory ul. Kopernika 11 51-622 Wroclaw, Poland
C. Sterken
Affiliation:
Astrophysical Institute Vrije Universiteit Brussel Pleinlaan 2 1050 Brussel, Belgium

Extract

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In the late sixties, Spica (α Virginia, a 4.01454-day SB2 and interferometric binary, with a B1 IV primary component) was showing a light variation that consisted of two periodic terms. One term had the form of a double wave with the above-mentioned orbital period, the other was sinusoidal in shape and had a period equal to 0.1738 days. The double-wave term was clearly an ellipsoidal variation, caused by aspect changes of the tidally distorted primary, whereas the short-period term could only be explained as due to the primary's β Cephei-type pulsations. However, in 1972 these pulsations became undetectable.

Type
Chapter 4: Asteroseismology: Results and Prospects
Information
Symposium - International Astronomical Union , Volume 123: Advances In Hello- and Asteroseismology , 1988 , pp. 273 - 276
Copyright
Copyright © Reidel 1988 

References

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