Remote sensing of possible plasma density bubbles in the inner Jovian dayside magnetosphere

Farrell, W. M.; Kaiser, M. L.; Kurth, W. S.; Desch, M. D.; Gurnett, D. A.; Hospodarsky, G. B.; MacDowall, R. J.

doi:10.1029/2003ja010130

Cited by 18 publications

(12 citation statements)

References 38 publications

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“…Reiner et al (2000) have found that nKOM events were detected by Ulysses/URAP after a few rotations of Jupiter following strong solar wind ram pressure pulses, and that there was a clear 26 days cadence of nKOM observations. Farrell et al (2004) have interpreted a Jovian broadband kilometric radiation (bKOM) as an Electron–Cyclotron Harmonic radiation originating from a plasma density depletion or plasma bubble at the outer edge of the Io torus.…”

Section: Discussionmentioning

confidence: 99%

“…Thus, Kaiser and MacDowall (1998) have shown that “bullseyes” emission have a tendency to occur after the passage of a solar wind pressure pulse, which crosses the Jovian magnetosphere every 13 or 26 days and the temporal spacing between the centers of the individual “bullseyes” was

\sim 6 %

longer than the Jupiter rotation. Farrell et al (2004) have proposed that “bullseyes” emission can be explained (non-uniquely) as typically nKOM emissions from the radially extended plasma fingers developed in the course of the strong interchange instability which may operate along the outer Io torus edge (Yang et al, 1992, 1994). This instability, which in general can be considered as a competition between cold and energetic plasma components, can be triggered by the strong solar wind impulses.…”

Section: Discussionmentioning

confidence: 99%

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Periodic bursts of Jovian non-Io decametric radio emission

Panchenko

Rücker

Farrell

2013

Planetary and Space Science

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During the years 2000–2011 the radio instruments onboard Cassini, Wind and STEREO spacecraft have recorded a large amount of the Jovian decametric radio emission (DAM). In this paper we report on the analysis of the new type of Jovian periodic radio bursts recently revealed in the decametric frequency range. These bursts, which are non-Io component of DAM, are characterized by a strong periodic reoccurrence over several Jovian days with a period ≈1.5% longer than the rotation rate of the planet's magnetosphere (System III). The bursts are typically observed between 4 and 12 MHz and their occurrence probability has been found to be significantly higher in the sector of Jovian Central Meridian Longitude between 300° and 60° (via 360°). The stereoscopic multispacecraft observations have shown that the radio sources of the periodic bursts radiate in a non-axisymmetric hollow cone-like pattern and sub-corotate with Jupiter remaining active during several planet's rotations. The occurrence of the periodic non-Io DAM bursts is strongly correlated with pulses of the solar wind ram pressure at Jupiter. Moreover the periodic bursts exhibit a tendency to occur in groups every ∼25 days. The polarization measurements have shown that the periodic bursts are right hand polarized radio emission associated with the Northern magnetic hemisphere of Jupiter. We suggest that periodic non-Io DAM bursts may be connected with the interchange instability in Io plasma torus triggered by the solar wind.

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Section: Discussionmentioning

confidence: 99%

\sim 6 %

Section: Discussionmentioning

confidence: 99%

Periodic bursts of Jovian non-Io decametric radio emission

Panchenko

Rücker

Farrell

2013

Planetary and Space Science

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“…In addition to the well known S-bursts, drifting tones and spectral bands were observed within bKOM Lecacheux et al, 2001). A tentative interpretation of the latter in association with plasma density bubbles in the inner jovian dayside magnetosphere was proposed by Farrell et al (2004a).…”

Section: Rpws Observations At Jupitermentioning

confidence: 97%

Radio Wave Emission from the Outer Planets Before Cassini

Zarka

Kurth

2005

Space Sci Rev

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We review observations and theories of radio wave emissions from the outer planets. These include radio emissions from the auroral regions and from the radiation belts, low-frequency electromagnetic emissions, and atmospheric lightning. For each of these emissions, we present in more details our knowledge of the Saturn counterpart, as well as expectations for Cassini. We summarize the capabilities of the radio instrument onboard Cassini, observations performed during the Jupiter flyby, and first (remote) observations of Saturn. Open questions are listed along with the specific observations that may bring responses to them. The coordinated observations (from the ground and from space) that would be valuable to perform in parallel to Cassini measurements are briefly discussed. Finally, we outline future missions and perspectives.

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“…Furthermore, several episodes have been found when periodic non-Io DAM was observed simultaneously with so-called "bullseyes", U-shaped narrowband emissions in the low frequency 20-50 kHz band (Kaiser and MacDowall, 1998), observed by Ulysses/URAP spacecraft. Farrell et al (2004) explained the "bullseyes" emission as Jovian narrowband kilometric emissions (nKOM) generated in the radially extended plasma fingers developed in the course of the interchange instability in the Io torus. These latitudinal extended fingers may be a plasma source which supplies the cyclotron maser in the auroral region.…”

Section: Jupiter Radio Emissionmentioning

confidence: 99%

Planetary radio astronomy: Earth, giant planets, and beyond

2014

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Abstract. The magnetospheric phenomenon of non-thermal radio emission is known since the serendipitous discovery of Jupiter as radio planet in 1955, opening the new field of "Planetary Radio Astronomy". Continuous ground-based observations and, in particular, space-borne measurements have meanwhile produced a comprehensive picture of a fascinating research area. Space missions as the Voyagers to the Giant Planets, specifically Voyager 2 further to Uranus and Neptune, Galileo orbiting Jupiter, and now Cassini in orbit around Saturn since July 2004, provide a huge amount of radio data, well embedded in other experiments monitoring space plasmas and magnetic fields. The present paper as a condensation of a presentation at the Kleinheubacher Tagung 2013 in honour of the 100th anniversary of Prof. Karl Rawer, provides an introduction into the generation mechanism of non-thermal planetary radio waves and highlights some new features of planetary radio emission detected in the recent past. As one of the most sophisticated spacecraft, Cassini, now in space for more than 16 years and still in excellent health, enabled for the first time a seasonal overview of the magnetospheric variations and their implications for the generation of radio emission. Presently most puzzling is the seasonally variable rotational modulation of Saturn kilometric radio emission (SKR) as seen by Cassini, compared with early Voyager observations. The cyclotron maser instability is the fundamental mechanism under which generation and sufficient amplification of non-thermal radio emission is most likely. Considering these physical processes, further theoretical investigations have been started to investigate the conditions and possibilities of non-thermal radio emission from exoplanets, from potential radio planets in extrasolar systems.

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Remote sensing of possible plasma density bubbles in the inner Jovian dayside magnetosphere

Cited by 18 publications

References 38 publications

Periodic bursts of Jovian non-Io decametric radio emission

Periodic bursts of Jovian non-Io decametric radio emission

Radio Wave Emission from the Outer Planets Before Cassini

Planetary radio astronomy: Earth, giant planets, and beyond

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