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Astron. Astrophys. 315, L261-L264 (1996)

The central star of the planetary nebula NGC 6302*

S.R. Pottasch1, D. Beintema2, F.J. Dominguez-Rodriguez1, S. Schaeidt3, E. Valentijn2, and B. Vandenbussche4,5

1 Kapteyn Astronomical Institute, P.O. Box 800, 9700 AV Groningen, The Netherlands
2 SRON Laboratory for Space Research, P.O. Box 800, 9700 AV Groningen, The Netherlands
3 Max Planck Institut für Extraterrestrische Physik, Postfach 1603, D-85740 Garching, Germany
4 ISO Science Operations Centre, Astrophysics Division of ESA, P.O. Box 50727, E-28080 Villafranca, Madrid, Spain
5 Sterrenkundig Instituut, K.U. Leuven, Celestijnenlaan 200B, B-3001 Heverlee, Belgium

Received 4 July 1996 / Accepted 2 September 1996

Abstract. Selected results from the ISO spectrum of NGC 6302 are reported. The intensity of the high ionization [Mg VIII] line is given. The controversy concerning the mechanism of ionization of the high ionization stages, and especially the [NeV] lines is discussed. It is concluded that all lines can be reproduced in a photoionization model, if the temperature of the central star is about 380,000 K. The abundances of several elements in the nebula is given, as well as the intensities of the lines involved.

Key words: white dwarfs, planetary nebulae: general, planetary nebulae: individual: NGC 6302

* Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands and the United Kingdom) and with the participation of ISAS and NASA

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Last change: December 16, 1996
© European Southern Observatory (ESO) 1996