Modeling the inner Jovian electron radiation belt including non-equatorial particles

Santos-Costa, Daniel; Bourdarie, S.

doi:10.1016/s0032-0633(00)00151-3

Cited by 58 publications

(84 citation statements)

References 31 publications

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“…These belts are believed to be formed by inward radial transport of electrons from a source beyond the orbit of the moon Io (L = 6.6) on the assumption that the first adiabatic invariant remains conserved (Santos-Costa and Bourdarie, 2001;Sicard and Bourdarie, 2004). However, this idea requires a source of electrons in excess of 1 MeV for L > 6.6 ; the first such indications of a source were given in Horne et al (2008).…”

Section: Introductionmentioning

confidence: 99%

Electron acceleration at Jupiter: input from cyclotron-resonant interaction with whistler-mode chorus waves

et al. 2013

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Abstract. Jupiter has the most intense radiation belts of all the outer planets. It is not yet known how electrons can be accelerated to energies of 10 MeV or more. It has been suggested that cyclotron-resonant wave-particle interactions by chorus waves could accelerate electrons to a few MeV near the orbit of Io. Here we use the chorus wave intensities observed by the Galileo spacecraft to calculate the changes in electron flux as a result of pitch angle and energy diffusion. We show that, when the bandwidth of the waves and its variation with L are taken into account, pitch angle and energy diffusion due to chorus waves is a factor of 8 larger at Lshells greater than 10 than previously shown. We have used the latitudinal wave intensity profile from Galileo data to model the time evolution of the electron flux using the British Antarctic Survey Radiation Belt (BAS) model. This profile confines intense chorus waves near the magnetic equator with a peak intensity at ∼ 5 • latitude. Electron fluxes in the BAS model increase by an order of magnitude for energies around 3 MeV. Extending our results to L = 14 shows that cyclotron-resonant interactions with chorus waves are equally important for electron acceleration beyond L = 10. These results suggest that there is significant electron acceleration by cyclotron-resonant interactions at Jupiter contributing to the creation of Jupiter's radiation belts and also increasing the range of L-shells over which this mechanism should be considered.

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Section: Introductionmentioning

confidence: 99%

Electron acceleration at Jupiter: input from cyclotron-resonant interaction with whistler-mode chorus waves

et al. 2013

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“…Conversely, the morphology of the Jovian synchrotron sources is now well explained by a model of Jovian electron radiation belts developed by Santos-Costa and Bourdarie (2001). Variation of the synchrotron emission in conjunction with the solar wind is under study.…”

Section: Philippe Zarkamentioning

confidence: 98%

Commission 16: Physical Study of Planets and Satellites: (Etude Physique Des Planetes Et Des Satellites)

Cruikshank¹,

Courtin²,

Belton³

et al. 2002

Trans. Int. Astron. Union

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“…Modeling of radiation belts at the outer planets has until very recently included only the radial diffusion of electrons [at Jupiter (Goertz et al 1979;Santos-Costa and Bourdarie 2001;Sicard and Bourdarie 2004) and at Saturn (Hood 1983;SantosCosta et al 2003)]. More recently, local acceleration processes due to wave particle interactions have also been included in addition to radial diffusion in the modeling process; at Jupiter (Woodfield et al 2014) and at Saturn (Lorenzato et al 2012).…”

Section: Characteristics Of the Different Bodies On Which The Solar Wmentioning

confidence: 99%

What characterizes planetary space weather?

Lilensten

Coates

Déhant

et al. 2014

Astron Astrophys Rev

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Space weather has become a mature discipline for the Earth space environment. With increasing efforts in space exploration, it is becoming more and more necessary to understand the space environments of bodies other than Earth. This is the background for an emerging aspect of the space weather discipline: planetary space weather. In this article, we explore what characterizes planetary space weather, using some examples throughout the solar system. We consider energy sources and timescales, the characteristics of solar system objects and interaction processes. We

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Modeling the inner Jovian electron radiation belt including non-equatorial particles

Cited by 58 publications

References 31 publications

Electron acceleration at Jupiter: input from cyclotron-resonant interaction with whistler-mode chorus waves

Electron acceleration at Jupiter: input from cyclotron-resonant interaction with whistler-mode chorus waves

Commission 16: Physical Study of Planets and Satellites: (Etude Physique Des Planetes Et Des Satellites)

What characterizes planetary space weather?

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