Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· On-line Data
· References in the article
· Citations to the Article (19) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (7)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
IUE spectra and optical imaging of the oxygen-rich supernova remnant N132D
Authors:
Blair, William P.; Raymond, John C.; Long, Knox S.
Affiliation:
AA(Department of Physics and Astronomy, Johns Hopkins University, 34th & Charles Streets, Baltimore, MD 21218), AB(Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138), AC(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218)
Publication:
The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 423, no. 1, p. 334-343 (ApJ Homepage)
Publication Date:
03/1994
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Astronomical Models, Interstellar Matter, Magellanic Clouds, Supernova Remnants, Ultraviolet Spectra, Abundance, Heao 2, Iue, Nuclear Fusion, Photoionization
DOI:
10.1086/173811
Bibliographic Code:
1994ApJ...423..334B

Abstract

We present new optical Charge Coupled Devices (CCD) interference filter imagery and International Ultraviolet Explorer (IUE) spectroscopy for the oxygen-rich supernova remnant N132D in the Large Magellanic Cloud. The optical images show a wealth of structure, and comparison with an archival Einstein High Resolution Imager (HRI) X-ray image shows that a few optical features have X-ray counter-parts, but in general there is little correlation between X-ray and optical features. The IUE spectra at two positions show strong lines of carbon and oxygen, with lines of neon, magnesium, silicon, and helium also present and variable in relative intensities. We use optical data for N132D from Dopita & Tuohy (1984) with our UV observations to compare with shock models (both with and without thermal conduction) and X-ray photoionization model calculations. While none of the model fits is entirely satisfactory, the generally weak UV emission relative to optical disagrees with the general character of shock model predictions and indicates that photoionization is the dominant excitation mechanism for the UV/optical emission. This conclusion is similar to what was found for E0102 - 7219, the oxygen-rich remnant in the Small Magellanic Cloud. We derive rough abundances for the emitting material in N132D, compare to stellar nucleosynthesis models, and discuss the implications for its precursor. A precursor near 20 solar mass is consistent with the data.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences


More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints