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The Binary-Star Hypothesis for the Nucleus of NGC 1514

Published online by Cambridge University Press:  14 August 2015

L. Kohoutek
L. Kohoutek*
Affiliation:
Astronomical Institute, Czechoslovak Academy of Sciences, Czechoslovakia

Extract

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It is well known that the central star of the planetary nebula NGC 1514 (α50 = 4h06m.1, δ50 = +30°39'; lII= 165·5, bII = −15·3) differs from the other planetary nuclei by its high brightness (relative to the nebula) and late-type spectrum. The difference B∗ – Bn = 1m.9, and especially the A0-spectral type (Chopinet, 1963) are quite atypical for central stars. For these reasons we began a complex study of this object (Kohoutek, 1967; Kohoutek and Hekela, 1967) on the basis of the following sources of observational material:

  1. (1) Palomar Sky-Survey prints (Schmidt-camera, Palomar Observatory);

  2. (2) direct photographs in UBV system with the 2-m Schmidt-camera in Tautenburg (1962);

  3. (3) photoelectric UBV photometry with the 65-cm reflector at Ondřejov (1964–65),

  4. (4) (4) spectrograms of the central star using the 122-cm reflector in Asiago (1965), and relatively infrequent observational data from the older literature.

Type
Session V – Central Stars
Information
Symposium - International Astronomical Union , Volume 34: Planetary Nebulae , 1968 , pp. 324 - 328
Copyright
Copyright © Reidel 1968 

References

Chopinet, M. (1963) Publ. Obs. Haute Provence, 6, No. 34.Google Scholar
Harman, R.J., Seaton, M.J. (1966) Mon. Not. R. astr. Soc., 132, 15.Google Scholar
Khromov, G.S., Kohoutek, L. (1968) in the present volume, p. 227.Google Scholar
Kohoutek, L. (1967) Bull. astr. Inst. Csl., 18, 103.Google Scholar
Kohoutek, L., Hekela, J. (1967) Bull. astr. Inst. Csl., 18, 203.Google Scholar
Lawrence, G.M., Ostriker, J.P., Hesser, J.E. (1967) Astrophys. J., 148, L161.CrossRefGoogle Scholar
Seaton, M.J. (1966) Mon. Not. R. astr. Soc., 132, 113.CrossRefGoogle Scholar