Recent Changes in the Nucleus of the Planetary Nebulae LMC-N66

Details Recent Changes in the Nucleus of the Planetary Nebulae LMC-N66 Recent Changes in the Nucleus of the Planetary Nebulae LMC-N66

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...187.8003p&link_type=abstract

American Astronomical Society, 187th AAS Meeting, #80.03; Bulletin of the American Astronomical Society, Vol. 27, p.1401

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Scientific paper

We report recent spectacular changes in the WR spectrum of the central star of the planetary nebula LMC-N66. Before 1987, it showed a weak continuum with a Teff >= 120000 K and Lbol =~ 25000 L_sun. In 1990 the star began an intense mass-loss event and in a short time the continuum increased by a large factor and the absolute visual magnitude of the star changed from +1.24 in 1987 to -2.57 in January 1995. Simultaneously it developed impressive WR features (P-Cygni profiles in NV lambda1240 and CIV lambda1550 lines, wide HeII emission, etc.) typical of a Population I WN4.5 star. The ejecta consisted of highly ionized He- and N-rich material (Pe\ na et al., 1995, ApJ, 441, 343; Pe\ na, 1995, RevMexAASC, 3, 215). These conditions remained with some variations for more than 5 years. Recent optical and UV data obtained by us show that the mass-loss has diminished abruptly in less than three months. The fast optically-thick wind has almost disappeared and the visual brightness of the central object has diminished in 2 magnitudes. Part of the ejected material was detected at much lower velocity, emitting in HeII lambda lambda 6406, 6678, and other lines that disappeared in few days. The possibility of a fast recombination and cooling of the highly ionized ejecta is discussed.

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