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Jupiter’s radio spectrum from 74 MHz up to 8 GHz |
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| Authors: | Imke de Pater BJ Butler R Strom MJ Klein O Funke R Maddalena M Kesteven R Hunstead |
| Institution: | a Department of Astronomy, and Department of Earth and Planetary Science, 601 Campbell Hall, University of California, Berkeley, CA 94720, USA b National Radio Astronomy Observatory, Socorro, NM 87801, USA c Mullard Radio Astronomy Observatory, Cavendish Laboratory, Madingley Rd, Cambridge CB3 0HE, UK d Astron, P.O. Box 2, 7990 AA Dwingeloo, and Astronomical Institute “A. Pannekoek,” Univ. of Amsterdam, the Netherlands e Physics Department, University of California, Berkeley, CA 94720, USA f Jet Propulsion Laboratory, Pasadena, CA 91109, USA g Radioastron. Inst., Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany h Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany i National Radio Astronomy Observatory, Green Bank, WV 24944, USA j CSIRO, Epping, NSW 2121, Australia k Dept. of Mathematics, Applied Mathematics and Astronomy, PO Box 392, UNISA, 0003 South Africa l School of Physics, University of Sydney, NSW 2006, Australia |
| Abstract: | We carried out a brief campaign in September 1998 to determine Jupiter’s radio spectrum at frequencies spanning a range from 74 MHz up to 8 GHz. Eleven different telescopes were used in this effort, each uniquely suited to observe at a particular frequency. We find that Jupiter’s spectrum is basically flat shortwards of 1-2 GHz, and drops off steeply at frequencies greater than 2 GHz. We compared the 1998 spectrum with a spectrum (330 MHz-8 GHz) obtained in June 1994, and report a large difference in spectral shape, being most pronounced at the lowest frequencies. The difference seems to be linear with log(ν), with the largest deviations at the lowest frequencies (ν).We have compared our spectra with calculations of Jupiter’s synchrotron radiation using several published models. The spectral shape is determined by the energy-dependent spatial distribution of the electrons in Jupiter’s magnetic field, which in turn is determined by the detailed diffusion process across L-shells and in pitch angle, as well as energy-dependent particle losses. The spectral shape observed in September 1998 can be matched well if the electron energy spectrum at L = 6 is modeled by a double power law E−a (1+(E/E0))−b, with a = 0.4, b = 3, E0 = 100 MeV, and a lifetime against local losses τ0 = 6 × 107 s. In June 1994 the observations can be matched equally well with two different sets of parameters: (1) a = 0.6, b = 3, E0 = 100 MeV, τ0 = 6 × 107 s, or (2) a = 0.4, b = 3, E0 = 100 MeV, τ0 = 8.6 × 106 s. We attribute the large variation in spectral shape between 1994 and 1998 to pitch angle scattering, coulomb scattering and/or energy degradation by dust in Jupiter’s inner radiation belts. |
| Keywords: | Jupiter Magnetosphere Radio observations |
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