Large Magellanic Cloud Planetary Nebula Morphology: Probing Stellar Populations and Evolution.

  title={Large Magellanic Cloud Planetary Nebula Morphology: Probing Stellar Populations and Evolution.},
  author={Stanghellini and Shaw and Balick and Blades},
  journal={The Astrophysical journal},
  volume={534 2},
Planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) offer the unique opportunity to study both the population and evolution of low- and intermediate-mass stars, by means of the morphological type of the nebula. Using observations from our LMC PN morphological survey, and including images available in the Hubble Space Telescope Data Archive and published chemical abundances, we find that asymmetry in PNe is strongly correlated with a younger stellar population, as indicated by the… 
Morphology and Evolution of the Large Magellanic Cloud Planetary Nebulae
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We present the properties of the central stars from a sample of 54 planetary nebulae (PNe) observed in the Large Magellanic Cloud (LMC) with the Hubble Space Telescope Imaging Spectrograph (STIS).
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We used a new generation of asymptotic giant branch (AGB) stellar models that include dust formation in the stellar winds to find the links between evolutionary models and the observed properties of
The Large Magellanic Cloud PN population
  • W. Reid
  • Physics
    Proceedings of the International Astronomical Union
  • 2015
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The results of self-consistent photoionization modeling of 38 Magellanic Cloud PNe are presented and used to construct an H-R diagram for the central stars and to obtain both the nebular chemical
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The morphology of planetary nebulae (PNs) provides an essential tool for understanding their origin and evolution, since it reflects both the dynamics of the gas ejected at the tip of the asymptotic
Hubble Space Telescope Observations of Planetary Nebulae in the Magellanic Clouds. V. Mass Dependence of Dredge-up and the Chemical History of the Large Magellanic Cloud
A photoionization analysis of Hubble Space Telescope UV and ground-based optical spectrophotometry is given for eight more planetary nebulae (PNs) in the Large Magellanic Cloud (LMC). This allows the
Abundances of the heavy elements in the Magellanic Clouds. II - H II regions and supernova remnants
The first consistent abundance analysis of both H II regions and SNRs in the Magellanic Clouds is presented. Detailed modeling of the SNRs results in abundance measures in good agreement with those
Nebular Abundance Errors.
The errors inherent to the use of the standard "ionization correction factor" ("i_CF") method of calculating nebular conditions and relative abundances of H, He, N, O, Ne, S, and Ar in emission line
New theoretical yields of intermediate mass stars
The abundances predicted during the nal stages of the AGB with those observed in planetary nebu- lae in the Galactic disk are compared and show that the model with the aforementioned parameters is in good agreement with the observations.
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Preface Preface to First Edition General Introduction Photoionization Equilibrium Thermal Equilibrium Calculation of Emitted Spectrum Comparison of Theory with Observations Internal Dynamics of
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