CO-SPATIAL LONG-SLIT UV/OPTICAL SPECTRA OF TEN GALACTIC PLANETARY NEBULAE WITH HST /STIS. II. NEBULAR MODELS, CENTRAL STAR PROPERTIES, AND He+CNO SYNTHESIS

The goal of the present study is twofold. First, we employ new HST/STIS spectra and photoionization modeling techniques to determine the progenitor masses of eight planetary nebulae (IC 2165, IC 3568, NGC 2440, NGC 3242, NGC 5315, NGC 5882, NGC 7662, and PB 6). Second, for the first time we are able...

Full description

Saved in:
Bibliographic Details
Published in:The Astrophysical journal 2015-11, Vol.813 (2), p.121
Main Authors: Henry, R B C, Balick, B, Dufour, R J, Kwitter, K B, Shaw, R A, Miller, T R, Buell, J F, Corradi, R L M
Format: Article
Language:English
Subjects:
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
CARBON
CARBON MONOXIDE
COMPARATIVE EVALUATIONS
COMPUTERIZED SIMULATION
Dredges
ELEMENT ABUNDANCE
Enrichment
GALAXIES
HELIUM
HYDROGEN
MASS
MASS DISTRIBUTION
Mathematical models
METALLICITY
NITROGEN
PHOTOIONIZATION
PLANETARY NEBULAE
Progenitors (astrophysics)
Spectra
STAR CLUSTERS
STAR EVOLUTION
Stars
SYNTHESIS
WHITE DWARF STARS
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:The goal of the present study is twofold. First, we employ new HST/STIS spectra and photoionization modeling techniques to determine the progenitor masses of eight planetary nebulae (IC 2165, IC 3568, NGC 2440, NGC 3242, NGC 5315, NGC 5882, NGC 7662, and PB 6). Second, for the first time we are able to compare each object's observed nebular abundances of helium, carbon, and nitrogen with abundance predictions of these same elements by a stellar model that is consistent with each object's progenitor mass. Important results include the following: (1) the mass range of our objects' central stars matches well with the mass distribution of other central stars of planetary nebulae and white dwarfs; (2) He/H is above solar in all of our objects, in most cases likely due to the predicted effects of first dredge-up; (3) most of our objects show negligible C enrichment, probably because their low masses preclude third dredge-up; (4) C/O versus O/H for our objects appears to be inversely correlated, which is perhaps consistent with the conclusion of theorists that the extent of atmospheric carbon enrichment from first dredge-up is sensitive to a parameter whose value increases as metallicity declines; (5) stellar model predictions of nebular C and N enrichment are consistent with observed abundances for progenitor star masses [< or =]1.5 M sub([middot in circle]). Finally, we present the first published photoionization models of NGC 5315 and NGC 5882.
ISSN:1538-4357
0004-637X
1538-4357
DOI:10.1088/0004-637X/813/2/121