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The Crab Nebula Revisited [PDF]
Astrophysics and Space Science, 1994 The evolution of pulsar driven supernova remnants is briefly reviewed with special reference to the Crab Nebula. Simple models account for the integral properties of the Nebula. New data on the optical synchrotron continuum show strong spectral variations over the Nebula which will require more complex models of the particle diffusion.
L. Woltjer, M. P. Véron-Cetty
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Nature Physical Science, 1971 WE have reported the results of observations of the Crab Nebula at 10 µm which indicated a flux of 170 ± 50 f.u. (probable errors) compared with 30 f.u. to be expected from the usual synchrotron model1. We consider here the implications of this excess, based on the assumption at λ=1.2 mm of (1) a very large flux (16,000 f.u.)2 and (2) what appears to ...
P. G. Polden, David K. Aitken
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Nature, 1982
The initial mass of the Crab Nebula's progenitor star is estimated by comparing the observed nebular chemical abundances with detailed evolutionary calculations for 2.4- and 2.6-solar-mass helium cores of stars with masses of 8 to 10 solar masses. The results indicate that the mass of the Crab's progenitor was between the upper limit of about 8 solar ...
Theodore R. Gull +5 more
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The initial mass of the Crab Nebula's progenitor star is estimated by comparing the observed nebular chemical abundances with detailed evolutionary calculations for 2.4- and 2.6-solar-mass helium cores of stars with masses of 8 to 10 solar masses. The results indicate that the mass of the Crab's progenitor was between the upper limit of about 8 solar ...
Theodore R. Gull +5 more
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Spectroscopy of the Crab nebula
Publications of the Astronomical Society of the Pacific, 1978Detailed inspection of a spectrogram of the Crab nebula covering wavelengths 4450-6100 reveals the presence of faint forbidden lines of iron and nitrogen, most of which have not been observed before in the Crab. Only some filaments showed these emission features which are of low ionization and are emitted near the high density cores of filaments.
Roger A. Chevalier +2 more
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