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25. The Secondary Maximum of T Coronae Borealis

Published online by Cambridge University Press:  02 August 2017

Livio Gratton

Extract

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T Coronae Borealis is a well-known recurrent nova which has undergone two outbursts: in 1886 and in 1946. In both cases the star declined very fast after maximum and reach in less than two months the premaximum magnitude, shortly afterwards, there a small increase to a secondary very flat maximum followed by a slower decrease.

The symbiotic spectrum observed at minimum is usually interpreted as due to a binary involved in a small nebula; the excitation of the nebular spectrum is provided by shot fainter star, which undergoes the nova outbursts, while the brighter star (a normal ant) is constant in brightness. Sanford(1) has found the radial velocity of the M star 2 variable with a period of 774 days and a semi-amplitude of 21 km./sec.

Type
Part IV Symposia
Information
Transactions of the International Astronomical Union , Volume 8 , September 1954 , pp. 849 - 851
Copyright
Copyright © Cambridge University Press 1954

References

1) Sanford, R. F.: Ap. J 109, 81, 1948.Google Scholar
2) Gratton, L. and Krüger, E. C.: Mem. Soc. Astr It. 20, 197, 1949.Google Scholar
3) Gratton, L.: Astr. Obs. La Plata. Circ. No. 8, p. 17, 1951; an arithmetical error in this paper has been corrected here.Google Scholar
4) Cecchini, G. and Gratton, L.: Le Stelle Nuove, p. 455. Roma, 1941.Google Scholar
5) Hachenberg, O. and Wellman, P.: Z. Ap. 17, 246, 1939.Google Scholar
6) Courant, R. and Friedrichs, K. O.: Supersonic Flow and Shock Wave, ch. III, 1948. Google Scholar
7) Burgers, J M.: Kon. Ned. Akad. Wet. Proc. 5, 262, 332, 442, 1947.Google Scholar
8) Cillié, G. G.: M.N. 92, 820, 1932; 96, 771, 1936; see also H. Zanstra, Astr. Inst. Amst. Circ. No. 1, 1950.Google Scholar