Astronomy and Astrophysics – Astronomy
Scientific paper
Feb 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aj....107..565h&link_type=abstract
Astronomical Journal (ISSN 0004-6256), vol. 107, no. 2, p. 565-581
Astronomy and Astrophysics
Astronomy
42
Astronomical Spectroscopy, Giant Stars, Imaging Techniques, Interstellar Gas, Ionized Gases, Kinematics, Magellanic Clouds, Photoionization, Spectral Signatures, Stellar Spectra, Supergiant Stars, Emission Spectra, H Alpha Line, H Ii Regions, Supernova Remnants
Scientific paper
Deep H-alpha images of the Large Magellanic Cloud (LMC) have revealed the presence of numerous supergiant (greater than 300 pc radius) and giant shells of ionized gas. These structures are generally believed to be the result of the action of encircled massive stars on the surrounding interstellar medium. This paper examines the spectral and kinematic signature of this interaction through low and high dispersion spectra obtained for three supergiant and three giant shells in the LMC. One of the giant shells is an x-ray bubble embedded in the 30 Doradus nebula. The emission line ratios, including the lines (O II) lambda-3727, (O III) lambda-5007, (N II) lambda-6584, (S II) lambda-6717,31, in all but the embedded x-ray bubble, are found to be unusual compared to typical H II regions and supernova remnants in the same galaxy. However, the emission lines and surface brightnesses of these structures are generally consistent with models of photoionized gas having a very low ionization parameter due to the large distance between the encircled stars and the gas. Thus, emission from both the supergiant and giant shell structures appears to be dominated by photoionization processes. High dispersion spectra reveal that the profiles of the ionized gas at the edges of supershells are narrow and contain a single velocity component; spectra of the giant shells reveal broad profiles with multiple velocity components.
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