Pulsars and X-ray-emitting supernova remnants
Pulsars in supernova remnants emitting X rays
Holt, S. S.↗
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Statistical mechanics of supernovae
Galactic cosmic rays origin in terms of statistical mechanical model of supernova explosions
Jones, F. C.↗
An X-ray survey of the Cassiopeia region and its implications concerning supernova remnants and the galactic source distribution
Sounding rocket X ray survey of Cassiopeia region for supernova remnants and galactic source distribution
Giacconi, R.↗
X-ray characteristics of three supernova remnants
X ray spectrum analysis for Crab, Cas A and SN 1572 supernova remnants
Gorenstein, P.↗
Search for short pulses of energetic photons from supernovae using the atmospheric fluorescence
Atmospheric fluorescence observation of supernova energetic photon short pulse burst, using photomultiplier
Bertsch, D.↗
Interstellar absorption of X-rays emitted by supernova remnants
Cas A and SN 1572 supernova remnant radio sources X ray spectra, investigating absorption by interstellar medium
Gorenstein, P.↗
Ionization and heating of the Gum Nebula by energetic particles from the Vela X supernova
Model for ionization and heating of Gum Nebula by energetic particles from Vela X supernova
Boldt, E. A.↗
The Gum Nebula - Fossil Stroemgren sphere of the Vela X supernova
Gum Nebula-fossil Stromgren sphere of Vela X supernova, deriving ionization model from interstellar measurements
Brandt, J. C.↗
Nucleosynthesis in neutron rich supernova ejecta
Nucleosynthesis in neutron rich supernova ejecta, performing statistical equilibrium calculations at freeze out temperature and density
Cameron, A. G. W.↗
Supernovae and the extinction of the dinosaurs
Supernova explosion or solar outburst theory of climatic effects on mass extinction of organisms at Cretaceous-Tertiary boundary
Russell, D.↗
Nucleosynthesis in supernova models. II - The C12 detonation model
Supernovae detonation model, examining nucleosynthesis for solar system abundances
Arnett, W. D.↗
A blast-wave model for the Vela X supernova remnant and the origin of the Gum Nebula
Vela X supernova remnant blast wave model and Gum Nebula formation, discussing kinetic and rotational energy transformation into radiation
Tucker, W. H.↗
Fossil Stroemgren spheres from supernova explosions
H II region formation from type II supernovae explosion, detecting with fluorescence model
Kafatos, M. C.↗
Multiple pulsar ejection in supernova events
Multiple pulsar ejection in supernova core collapse and neutron star formation energy loss
Michel, F. C.↗
Ionization and heating of the Gum Nebula by energetic particles from the Vela X supernova
Gum Nebula ionization and heating by energetic particles from Vela X supernova
Boldt, E. A.↗
Identification of the Gum nebula as the fossil Stroemgren sphere of the Vela X supernova
Evidence is presented for the production of the Gum nebula by the Vela X supernova, as opposed to its ionization by gamma Velorum and zeta Puppis. A model for the excitation of the nebula is proposed.
Brandt, J. C.↗
The velocity and composition of supernova ejecta
In case of the Gum nebula, a pulsar - a presumed neutron star - is believed to be a relic of the supernova explosion. Regardless of the mechanism of the explosion, the velocity distribution and composition of the ejected matter will be roughly the same. The reimploding mass fraction is presumed to be neutron rich. The final composition is thought to be roughly 1/3 iron and 2/3 silicon, with many small fractions of elements from helium to iron. The termination of helium shell burning occurs because the shell is expanded and cooled by radiation stress. The mass fraction of the helium burning shell was calculated.
Colgate, S. A.↗
The early evolution of giant H II regions formed by supernova explosions
The evolution of a giant H II region, which cools after an initial ionization, is discussed. The discussion is applied to the Vela X and Tycho supernovae. Other giant H II regions might not be as easily detectable as the Vela X region. The Tycho region may be just detectable in the O(II) or O(III) optical lines or as a hole in the 21-cm emission line profiles, as is suggested in the data. These giant H II regions last appreciably longer than the continuum radio sources within them.
Kafatos, M. C.↗