Hubble Space Telescope observations of planetary nebulae in the magellanic clouds. 2: SMP 85, a young planetary

Details Hubble Space Telescope observations of planetary nebulae in the magellanic clouds. 2: SMP 85, a young planetary Hubble Space Telescope observations of planetary nebulae in the magellanic clouds. 2: SMP 85, a young planetary

May 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...426..150d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 426, no. 1, p. 150-158

Astronomy and Astrophysics

Astronomy

13

Abundance, Astronomical Models, Cosmic Dust, Emission Spectra, Magellanic Clouds, Oxygen, Planetary Nebulae, Stellar Evolution, Stellar Mass Ejection, Ultraviolet Astronomy, Asymptotic Giant Branch Stars, H Beta Line, Hubble Space Telescope, Stellar Luminosity, Stellar Mass, Stellar Temperature, Ultraviolet Spectrophotometers

Scientific paper

We have obtained Hubble Space Telescope Planetary Camera images in the (O III) lambda 5007 A emission line, and Faint Object Spectrograph (FOS) UV spectrophotometry of the low-excitation planetary nebula SMP 85 in the Large Magellanic Cloud. By combining these results with existing optical spectrophotometry, absolute flux measurements, and dynamical and density information, we have been able to construct a fully self-consistent nebular model. This proves that SMP 85 is a dense, young, carbon-rich object which started to be ionized about 500-1000 years ago, and which contains a substantial inner reservoir of atomic or molecular gas, probably in the form of many small cloudlets. These cloudlets have been ejected at a velocity not exceeding 6 km/s, a result which, together with the morphology is an important clue to mass loss during late asymptotic giant branch (AGB) evolution. We have directly detected the central star through its UV continuum emission, and from both Zanstra techniques and nebular modeling derive a stellar temperature of 46000 +/- 2000 K, a stellar luminosity of 7300 +/- 700 solar luminosity, and a core mass of 0.63-0.67 solar mass. The nebular analysis also demonstrates that there is severe depletion of the nebular gases onto dust grains, most likely of the calcium magnesium silicate variety; a surprising result in view of the carbon-rich nature of the ionized nebula.

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