An emission mechanism for the Io-independent Jovian decameter radiation

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1979ApJ___230__261G.pdf (1.35 MB)

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https://ui.adsabs.harvard.edu/abs/1979ApJ...230..261G/abstract

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http://hdl.handle.net/11603/30508

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UMBC Goddard Planetary Heliophysics Institute (GPHI)

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https://orcid.org/0000-0002-5317-988X

Date

1979-05

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journal articles
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Citation of Original Publication

Goldstein, M. L., and A. Eviatar. “An Emission Mechanism for the Io-Independent Jovian Decameter Radiation.” The Astrophysical Journal 230 (May 1, 1979): 261–73. https://doi.org/10.1086/157083.

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This work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
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Abstract

A theory of the Io-independent decameter radiation is developed. The radiation results from excitation of the electromagnetic loss-cone instability by keV electrons, stably trapped near L = 6. The radiation is excited in band III of the extraordinary mode. When the effects of refraction are estimated, it is shown that above 10 MHz radiation is beamed into the equatorial plane in a wide, but thin, conical sheet. When the instability analysis is coupled with one of the octopole models of the Jovian magnetic field, the maximum convective growth of the instability occurs in the directions of the non-Io A, B, and C sources. The shape of the peak radio flux frequency spectrum is found to be a consequence of the loss-cone shape of the electron distribution function.