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Electromagnetic pulse from supernovaeUpper and lower limits to the radiated electromagnetic pulse from a supernova are calculated assuming that the mass fraction of the matter expanding inside the dipole magnetic field shares energy and maintains the pressure balance in the process. A supernova model is described in which the explosion occurs in old low-mass stars containing less than 10% hydrogen in their ejecta and a remnant neutron star is produced. The analysis indicates that although the surface layer of a star of 1 g/cu thickness may be shock-accelerated to an energy factor of about 100 and may expand into the vacuum with an energy factor approaching 10,000, the equatorial magnetic field will retard this expansion so that the inner, more massive ejecta layers will effectively accelerate the presumed canonical dipole magnetic field to greater velocities than would the surface layer alone. A pulse of 10 to the 46th power ergs in a width of about 150 cm will result which will not be affected by circumstellar matter or electron self-radiation effects. It is shown that interstellar matter will attenuate the pulse, but that charge separation may reduce the attenuation and allow a larger pulse to escape.
Document ID
19750051597
Document Type
Reprint (Version printed in journal)
External Source(s)
Authors
Colgate, S. A. (New Mexico Institute of Mining and Technology Socorro, N. Mex., United States)
Date Acquired
August 8, 2013
Publication Date
June 1, 1975
Publication Information
Publication: Astrophysical Journal
Volume: 198
Subject Category
ASTROPHYSICS
Funding Number(s)
CONTRACT_GRANT: NSF GP-34875
CONTRACT_GRANT: NGR-06-018-001
Distribution Limits
Public
Copyright
Other