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The origin of the Gum nebulaObsrvations and theoretical investigations of the Gum nebula (GN) since about 1971 are reviewed. Direct observations of the GN, the Vela X supernova remnant (SNR), the Vela pulsar, and other stars in or near the GN are discussed with those of related phenomena such as the radio loops and known SNRs; the emphasis is on studies of the interstellar absorption lines, the evidence for hot gas in the GN, and the extended diffuse emission. The four basic models proposed for the GN are considered: a fossil Stromgren sphere, an old SNR, an H II region, or a superbubble. The GN physical parameters predicted by each model are listed in a table and compared. A minimum explanation which attributes the 36 x 36-deg filamentary structure and the 125-pc radius structure to the action of the stellar winds from Zeta Pup and Gamma-2 Vel (and perhaps the effect of a Vel X supernova explosion 20,000 years ago) is found most appropriate, at least until the questions of the net expansion rate of the GN (about 20 km/sec or about zero?) and the existence of the diffuse emission beyond the filamentary structure are resolved by observations.
Document ID
19840027468
Acquisition Source
Legacy CDMS
Document Type
Reprint (Version printed in journal)
Authors
Bruhweiler, F. C.
(Catholic University of America, Washington, DC, United States)
Kafatos, M.
(George Mason University Fairfax, VA, United States)
Brandt, J. C.
(NASA Goddard Space Flight Center Laboratory for Astronomy and Solar Physics, Greenbelt, MD, United States)
Date Acquired
August 12, 2013
Publication Date
September 1, 1983
Publication Information
Publication: Comments on Modern Physics, Part C - Comments on Astrophysics
Volume: 10
ISSN: 0146-2970
Subject Category
Astrophysics
Accession Number
84A10255
Distribution Limits
Public
Copyright
Other

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