Spectrophotometry of Selected Planetary Nebulae of Type I in the Magellanic Clouds

Abundances in Magellanic Cloud planetary nebulae

Symposium - International Astronomical Union ◽

10.1017/s0074180900200612 ◽

1991 ◽

Vol 148 ◽

pp. 291-298 ◽

Cited By ~ 3

Author(s):

M. J. Barlow

Keyword(s):

Planetary Nebulae ◽

Magellanic Cloud ◽

Magellanic Clouds ◽

Type I ◽

The Third

The enhanced nitrogen abundances in planetary nebulae (PN) show the effects of CN-cycle processing at the time of the first dredge-up, while their very enhanced carbon abundances show the effects of the third dredge-up. The efficiency of both the first and third dredge-ups increases with decreasing initial metallicity. ON-cycle depletion of oxygen via the second dredge-up does not appear to have been significant in LMC Type I planetary nebulae (those with N/O > 0.5) – these nebulae have experienced the third dredge-up and envelope-burning, giving enhanced C+N abundances. The LMC Type I PN show enhanced Ne/O ratios. Enrichment rates in nitrogen and carbon by PN are estimated for the ISM s of the Magellanic Clouds.

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Hubble Space Telescope Observations of Planetary Nebulae in the Magellanic Clouds. I. The Extreme Type I SMP 83/WS 35

The Astrophysical Journal ◽

10.1086/173437 ◽

1993 ◽

Vol 418 ◽

pp. 804 ◽

Cited By ~ 26

Author(s):

Michael A. Dopita ◽

Holland C. Ford ◽

Ralph Bohlin ◽

Ian N. Evans ◽

Stephen J. Meatheringham

Keyword(s):

Hubble Space Telescope ◽

Planetary Nebulae ◽

Magellanic Clouds ◽

Type I ◽

Space Telescope ◽

Extreme Type

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Chemical Abundances in Magellanic Cloud Planetary Nebulae

Symposium - International Astronomical Union ◽

10.1017/s0074180900138732 ◽

1989 ◽

Vol 131 ◽

pp. 354-354

Author(s):

D. J. Monk ◽

M. J. Barlow ◽

R. E. S. Clegg

Keyword(s):

Spectroscopic Data ◽

Planetary Nebulae ◽

Magellanic Cloud ◽

Magellanic Clouds ◽

Type I ◽

Chemical Abundances ◽

Special Groups

Optical spectroscopic data for 71 Planetary Nebulae (PN) in the Large and Small Magellanic Clouds have been analysed. The line fluxes have been used to determine nebular temperatures, densities, and the abundances of He, N, O, Ne and Ar, relative to H. In our sample there are 12 nebulae with N/O ≥ 0.5, resembling Peimbert's Type I PN; 6 low excitation (LE) objects (1 ≤ I(5007)/I(Hβ) ≤ 4); and 4 very-low-excitation (VLE) nebulae (I(Hβ) > I(5007), similar to the Galactic VLE class. Mean abundances have been calculated for the nebulae not in these special groups.

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Spectrophotometry of Selected Planetary Nebulae of Type I in the Magellanic Clouds

Symposium - International Astronomical Union ◽

10.1017/s0074180900172584 ◽

1993 ◽

Vol 155 ◽

pp. 584-584 ◽

Cited By ~ 3

Author(s):

S. Torres-Peimbert ◽

M. Peimbert ◽

M.T. Ruitz ◽

M. Peña

Keyword(s):

Wavelength Range ◽

Planetary Nebulae ◽

Magellanic Clouds ◽

Type I ◽

Chemical Abundances ◽

Spectroscopic Observations ◽

Physical Conditions

We carried out spectroscopic observations of N67 (in the SMC), and N66, N97 and N102 (in the LMC) with the 4-m telescope of CTIO. The wavelength range is λλ 3500–7400. From these we obtained physical conditions and chemical abundances of these objects.

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Abundances and nebular and central star masses for Magellanic Cloud planetary nebulae

Symposium - International Astronomical Union ◽

10.1017/s0074180900200727 ◽

1991 ◽

Vol 148 ◽

pp. 334-336 ◽

Cited By ~ 4

Author(s):

N. A. Walton ◽

M. J. Barlow ◽

D. J. Monk ◽

R.E.S. Clegg

Keyword(s):

Energy Balance ◽

Planetary Nebulae ◽

Central Star ◽

Magellanic Clouds ◽

Optical Data ◽

Type I ◽

Density Plot ◽

Elemental Abundances ◽

The Mean ◽

Hydrogen Mass

We present the results of a spectroscopic study of planetary nebulae (PN) in the Magellanic Clouds. The optical survey of He, N, O, and Ne abundances by Monk et al. (1988) has been updated by higher S/N AAT optical data. In addition, carbon and other elemental abundances have been derived from the IUE spectra of 38 PN. Ionized nebular masses have been derived for 80 PN. The ionised mass versus nebular electron density plot shows that planetary nebulae become optically thin when their electron densities drop below 4500 cm--3. Below this density, the mean nebular hydrogen mass found for non-Type I PN is 0.22±0.08 M⊙. Using Zanstra and energy-balance methods, the mean central star mass found for 14 SMC and LMC PN is 0.59±0.02 M⊙.

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