Jovian <i>S</i> burst generation by Alfvén waves

Hess, S.; Mottez, Fabrice; Zarka, Philippe

doi:10.1029/2006ja012191

Cited by 54 publications

(103 citation statements)

References 30 publications

(51 reference statements)

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“…Recent works have been specifically devoted to non-MHD effects [Tsiklauri et al, 2005;McClements and Fletcher, 2009;Bian and Kontar, 2011]. There are also observational evidences that Alfvén waves can accelerate electrons in the vicinity of Io and Jupiter [Hess et al, 2007] sometimes combined with other acceleration structures [Hess et al, 2009]. However, in the Jovian case, it is not obvious that the plasma cavities are the sources of the inertial effects [Mottez et al, 2010] and it is possible that they result from wave filamentation at the border of the Io plasma torus .…”

Section: Influence Of the Ion To Electron Mass Ratiomentioning

confidence: 99%

Electron acceleration by an Alfvénic pulse propagating in an auroral plasma cavity

Mottez

Génot

2011

J. Geophys. Res.

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[1] With the help of a 2.5-D particle-in-cell simulation code, we investigate the physics of the acceleration of auroral electrons, through the interaction of an isolated Alfvén wave packet with a plasma density cavity. The cavity is edged by density gradients perpendicular to the magnetic field. We show that a single passing of an isolated wave packet over a (infinite) cavity creates an electron beam. It triggers local current and beam-plasma instabilities and small-scale coherent electric structures. The energy flux of downgoing electrons is significantly increased, whereas upgoing electrons are also accelerated, even if no beam is formed. Accelerated electrons remain after the passage of the Alfvénic pulse, allowing the observation of energetic particles without any significant electromagnetic perturbation. The dependence of this process on the electron to ion mass ratio is consistent with its control by inertial effects.Citation: Mottez, F., and V. Génot (2011), Electron acceleration by an Alfvénic pulse propagating in an auroral plasma cavity, J. Geophys. Res., 116,

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Section: Influence Of the Ion To Electron Mass Ratiomentioning

confidence: 99%

Electron acceleration by an Alfvénic pulse propagating in an auroral plasma cavity

Mottez

Génot

2011

J. Geophys. Res.

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“…This perturbation propagates along the field lines as Alfvén waves [Neubauer, 1980;Goertz, 1983;Saur, 2004] from the satellite to the planet ionosphere, where it generates emissions spanning the spectrum from low-frequency radio to UVs [Bigg, 1964;Connerney et al, 1993;Clarke et al, 1996;Prangé et al, 1996;Clarke et al, 2002;Grodent et al, 2009;Wannawichian et al, 2010]. Alfvén waves accelerate electrons that excite the auroral emissions [Jones and Su, 2008;Swift, 2007;Hess et al, 2007Hess et al, , 2010. In the Io case, Hess et al [2010] showed that the turbulent filamentation of the Alfvén wave close to the satellite, seen by Chust et al [2005], is necessary to explain the observed power of the emissions.…”

Section: Introductionmentioning

confidence: 99%

Comparative study of the power transferred from satellite-magnetosphere interactions to auroral emissions

et al. 2011

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[1] Io's interaction with the Jovian magnetosphere generates a power of about 10 12 W which propagates as Alfvén waves along the magnetic field lines and is partly transferred to electrons, resulting in intense auroral emissions. A recent study of the power transmission along the Io flux tube and of the electron acceleration at high latitudes showed that the power of the observed emissions is well explained by assuming filamentation of the Alfvén waves in the torus and the acceleration of the electrons at high latitude. At Jupiter, UV footprints related to Europa and Ganymede have also been observed. At Saturn recent observations revealed a weak UV footprint of Enceladus. We apply the Io interaction model to the Europa and Enceladus interactions. We show that the Alfvén wave filamentation leads to a precipitating electron power consistent with the power of the observed UV footprints.Citation: Hess, S. L. G., P. A. Delamere, V. Dols, and L. C. Ray (2011), Comparative study of the power transferred from satellite-magnetosphere interactions to auroral emissions,

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“…Small-scale Alfvén waves are trapped in the wings, which cause particle acceleration (Su et al 2003;Ergun et al 2006) and decametric radiation (Hess et al 2007(Hess et al , 2008(Hess et al , 2009). In the highly relativistic pulsar wind, the acceleration and emission process may be quite different from those arising in the vicinity of Jupiter, but the current A125, page 3 of 8 A&A 555, A125 (2013) neutron star I A certainly constitutes an important source of free energy for radio emissions.…”

Section: Radio Emissionsmentioning

confidence: 99%

Towards a theory of extremely intermittent pulsars

Mottez¹,

Bonazzola²,

Heyvaerts³

2013

A&A

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Aims. We investigate whether one or many companions are orbiting the extremely intermittent pulsar PSR B1931+24. Methods. We constrained our analysis on previous observations of eight fundamental properties of PSR B1931+24. The most puzzling properties are the intermittent nature of the pulsar's activity, with active and quiet phases that alternate quasi-periodically; the variation of the slowing-down rate of its period between active and quiet phases; and because there are no timing residuals, it is highly unlikely that the pulsar has a massive companion. Here, we examine the effects that one putative companion immersed in the magnetospheric plasma or the wind of the pulsar might have, as well as the associated electric current distribution. We analysed several possibilities for the distance and orbit of this hypothetical companion and the nature of its interaction with the neutron star. Results. We show that if the quasi-periodic behaviour of PSR B1931+24 was caused by a companion orbiting the star with a period of 35 or 70 days, the radio emissions, usually considered to be those of the pulsar would in that specific case be emitted in the companion's environment. We analysed four possible configurations and conclude that none of them would explain the whole set of peculiar properties of PSR 1931+24. We furthermore considered a period of 70 days for the precession of the periastron associated to an orbit very close to the neutron star. This hypothesis is analysed in a companion paper.

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Jovian S burst generation by Alfvén waves

Cited by 54 publications

References 30 publications

Electron acceleration by an Alfvénic pulse propagating in an auroral plasma cavity

Electron acceleration by an Alfvénic pulse propagating in an auroral plasma cavity

Comparative study of the power transferred from satellite-magnetosphere interactions to auroral emissions

Towards a theory of extremely intermittent pulsars

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