Io Jupiter interaction, millisecond bursts and field-aligned potentials
TL;DR: In this paper, the authors performed an automated analysis of 230 high-resolution dynamic spectra of S-bursts, providing 5 × 10 6 frequency drift measurements and confirmed over a large number of measurements that the frequency drift d f / d t (f ) is in average negative and decreases (in absolute value) at high frequencies, as predicted by the adiabatic theory.
About: This article is published in Planetary and Space Science.The article was published on 2007-01-01. It has received 61 citations till now. The article focuses on the topics: Jupiter & Jovian.
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TL;DR: The electron-cyclotron maser is a process that generates coherent radiation from plasma as mentioned in this paper, and it has gained increasing attention as a dominant mechanism of producing high-power radiation in natural high-temperature magnetized plasmas.
Abstract: The electron–cyclotron maser is a process that generates coherent radiation from plasma. In the last two decades, it has gained increasing attention as a dominant mechanism of producing high-power radiation in natural high-temperature magnetized plasmas. Originally proposed as a somewhat exotic idea and subsequently applied to include non-relativistic plasmas, the electron–cyclotron maser was considered as an alternative to turbulent though coherent wave–wave interaction which results in radio emission. However, when it was recognized that weak relativistic corrections had to be taken into account in the radiation process, the importance of the electron–cyclotron maser rose to the recognition it deserves. Here we review the theory and application of the electron–cyclotron maser to the directly accessible plasmas in our immediate terrestrial and planetary environments. In situ access to the radiating plasmas has turned out to be crucial in identifying the conditions under which the electron–cyclotron maser mechanism is working. Under extreme astrophysical conditions, radiation from plasmas may provide a major energy loss; however, for generating the powerful radiation in which the electron–cyclotron maser mechanism is capable, the plasma must be in a state where release of susceptible amounts of energy in the form of radiation is favorable. Such conditions are realized when the plasma is unable to digest the available free energy that is imposed from outside and stored in its particle distribution. The lack of dissipative processes is a common property of collisionless plasmas. When, in addition, the plasma density becomes so low that the amount of free energy per particle is large, direct emission becomes favorable. This can be expressed as negative absorption of the plasma which, like in conventional masers, leads to coherent emission even though no quantum correlations are involved. The physical basis of this formal analogy between a quantum maser and the electron–cyclotron maser is that in the electron–cyclotron maser the free-space radiation modes can be amplified directly. Several models have been proposed for such a process. The most famous one is the so-called loss-cone maser. However, as argued in this review, the loss-cone maser is rather inefficient. Available in situ measurements indicate that the loss-cone maser plays only a minor role. Instead, the main source for any strong electron–cyclotron maser is found in the presence of a magnetic-field-aligned electric potential drop which has several effects: (1) it dilutes the local plasma to such an extent that the plasma enters the regime in which the electron–cyclotron maser becomes effective; (2) it generates energetic relativistic electron beams and field-aligned currents; (3) it deforms, together with the magnetic mirror force, the electron distribution function, thereby mimicking a high energy level sufficiently far above the Maxwellian ground state of an equilibrium plasma; (4) it favors emission in the free-space RX mode in a direction roughly perpendicular to the ambient magnetic field; (5) this emission is the most intense, since it implies the coherent resonant contribution of a maximum number of electrons in the distribution function to the radiation (i.e., to the generation of negative absorption); (6) it generates a large number of electron holes via the two-stream instability, and ion holes via the current-driven ion-acoustic instability which manifest themselves as subtle fine structures moving across the radiation spectrum and being typical for the electron–cyclotron maser emission process. These fine structures can thus be taken as the ultimate identifier of the electron–cyclotron maser. The auroral kilometric radiation of Earth is taken here as the paradigm for other manifestations of intense radio emissions such as the radiation from other planets in the solar system, from exoplanets, the Sun and other astrophysical objects.
358 citations
Cites background from "Io Jupiter interaction, millisecond..."
...Recently, Zarka et al. (2005) argued that S-bursts are the result of loss-cone maser activity inside the Io flux tube....
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...…extrasolar planets has immediately stimulated the idea that in analogy to the strongly magnetized planets in the solar system, exoplanets could also radiate in the radio band, possibly emitting maser radiation (Farrell et al. 1999; Bastian et al. 2000; Zarka et al. 2001b; Winterhalter et al. 2005)....
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...Application to Jupiter and radiation from the other magnetized planets followed, and speculations about radiation emitted from extrasolar planets when they are magnetized strongly enough have been published as well (Bastian et al. 2000; Zarka et al. 2001a,b)....
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...Searches have been going on at the Very Large Array (VLA) in New Mexico (Bastian et al. 2000) and a comparable array UTR-2 in Kharkov (Ukraine) (Zarka et al. 2001b)....
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...From the knowledge of the emissivities of Earth and Jupiter under solar-wind conditions, one may scale emissivities up to exoplanets of the family of ‘hot Jupiters’ close to their mother stars (Zarka et al. 2001b)....
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University of Colorado Boulder1, INAF2, Southwest Research Institute3, University of Texas at San Antonio4, University of Liège5, University of Leicester6, Goddard Space Flight Center7, Planetary Science Institute8, University of Iowa9, Jet Propulsion Laboratory10, Johns Hopkins University11, University of California, Los Angeles12, Centre national de la recherche scientifique13
TL;DR: Junior as discussed by the authors is the first spacecraft to enter polar orbit of Jupiter and venture deep into unexplored polar territories of the magnetosphere, where it carries a range of instruments that take particles and fields measurements, remote sensing observations of auroral emissions at UV, visible, IR and radio wavelengths, and detect microwave emission from Jupiter's radiation belts.
Abstract: In July 2016, NASA’s Juno mission becomes the first spacecraft to enter polar orbit of Jupiter and venture deep into unexplored polar territories of the magnetosphere. Focusing on these polar regions, we review current understanding of the structure and dynamics of the magnetosphere and summarize the outstanding issues. The Juno mission profile involves (a) a several-week approach from the dawn side of Jupiter’s magnetosphere, with an orbit-insertion maneuver on July 6, 2016; (b) a 107-day capture orbit, also on the dawn flank; and (c) a series of thirty 11-day science orbits with the spacecraft flying over Jupiter’s poles and ducking under the radiation belts. We show how Juno’s view of the magnetosphere evolves over the year of science orbits. The Juno spacecraft carries a range of instruments that take particles and fields measurements, remote sensing observations of auroral emissions at UV, visible, IR and radio wavelengths, and detect microwave emission from Jupiter’s radiation belts. We summarize how these Juno measurements address issues of auroral processes, microphysical plasma physics, ionosphere-magnetosphere and satellite-magnetosphere coupling, sources and sinks of plasma, the radiation belts, and the dynamics of the outer magnetosphere. To reach Jupiter, the Juno spacecraft passed close to the Earth on October 9, 2013, gaining the necessary energy to get to Jupiter. The Earth flyby provided an opportunity to test Juno’s instrumentation as well as take scientific data in the terrestrial magnetosphere, in conjunction with ground-based and Earth-orbiting assets.
192 citations
TL;DR: In this paper, it was shown that the Alfven waves need to be filamented by a turbulent cascade process and accelerate the electrons at high latitude in order to explain the observations and to form a consistent scheme of the Io-Jupiter interaction.
Abstract: [1] Io's motion relative to the Jovian magnetic field generates a power of about 1012 W, which is thought to propagate as an Alfven wave along the magnetic field line. This power is transmitted to the electrons, which will then precipitate and generate the observed auroral phenomena from UV to radio wavelengths. A more detailed look at this hypothesis shows some difficulties: Can the Alfven waves escape the torus or are they trapped inside? Where and how are the particles accelerated? In which direction? Is there enough power transmitted to the particles to explain the strong brightness of the auroral emissions in UV, IR, visible, and radio? In other words, can we make a global, consistent model of the Io-Jupiter interaction that matches all the observations? To answer these questions, we review the models and studies that have been proposed so far. We show that the Alfven waves need to be filamented by a turbulent cascade process and accelerate the electrons at high latitude in order to explain the observations and to form a consistent scheme of the Io-Jupiter interaction.
98 citations
TL;DR: In this article, the ionospheric response to auroral precipitation at the giant planets is reviewed, using models and observations The emission processes for aurorae at radio, infrared, visible, ultraviolet, and X-ray wavelengths are described, and exemplified using ground-and space-based observations Comparisons between the emissions at different wavelengths are made, where possible, and interpreted in terms of precipitating particle characteristics or atmospheric conditions.
Abstract: The ionospheric response to auroral precipitation at the giant planets is reviewed, using models and observations The emission processes for aurorae at radio, infrared, visible, ultraviolet, and X-ray wavelengths are described, and exemplified using ground- and space-based observations Comparisons between the emissions at different wavelengths are made, where possible, and interpreted in terms of precipitating particle characteristics or atmospheric conditions Finally, the spatial distributions and dynamics of the various components of the aurorae (moon footprints, low-latitude, main oval, polar) are related to magnetospheric processes and boundaries, using theory, in situ, and remote observations, with the aim of distinguishing between those related to internally-driven dynamics, and those related to the solar wind interaction
95 citations
TL;DR: In this article, a good fit of arcs t-f location and shape is obtained for loss-cone driven (oblique) emission beamed in a hollow cone of half-angle ≥ 80° around the source magnetic field, closing at high frequencies, and of cone thickness ≤ 1°.
Abstract: [1] The electrodynamic interaction between Io and Jupiter causes electron acceleration in/near the Io flux tube (IFT), which in turn produces intense radio emissions in the hecto-decameter range, displaying arc shapes in the time-frequency plane. The shapes depend on the hemisphere of origin of the emission and on the Io-Jupiter-observer geometry. Assuming radio wave generation by the cyclotron-maser instability, we simulate t-f arc shapes as a function of emission beaming, lead angle between the radio emitting field line and the instantaneous Io field line, and electron energy. A good fit of arcs t-f location and shape is obtained for loss-cone driven (oblique) emission beamed in a hollow cone of half-angle ≥80° around the source magnetic field, closing at high frequencies, and of cone thickness ≤1°. The lead angle is found between a few degrees and ∼40° in both hemispheres. Resonant electron energies are about a few keV. Implications on the absence of a plasma cavity at IFT footprints and on Jupiter's internal magnetic field model are discussed.
73 citations
References
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TL;DR: In this article, a review of the main results on electrostatic double layers obtained from theory and laboratory and space experiments up to the spring of 1977 is given, among other things, necessary criteria for existence and stability, quantitative estimates of charge separation and thickness, and some probable cause of DL-formation in terms of an instability.
Abstract: A review is given of the main results on electrostatic double layers (sometimes called ‘space charge layers’ or ‘sheaths’) obtained from theory and laboratory and space experiments up to the spring of 1977. The paper begins with a definition of double layers in terms of potential drop, electric field, and charge separation. Then a review is made of the theoretical results obtained so far. This covers, among other things, necessary criteria for existence and stability, quantitative estimates of charge separation and thickness, and some probable cause of DL-formation in terms of an instability. Next, experimental results obtained in the laboratory are compared with the theoretical results. Due to recent progress in experimental technique, the interior of a double layer can now be studied in much more detail than was possible before. By means of barium jets and satellite probes, double layers have now been found at the altitudes that were previously predicted theoretically. The general potential distribution above the auroral zone, suggested by inverted V-events and electric field reversals, is corroborated.
315 citations
"Io Jupiter interaction, millisecond..." refers background or result in this paper
...They are attributed to the presence of electrostatic double layers along the flux tubes (Block, 1978). The presence of potential drops in IFT was expected, due to previous simulations showing abrupt variations of the potential near Jupiter. Solving the Vlasov and Poisson equations along the IFT, Su et al. (2003) found a potential drop of about 5 keV was found at 1:5RJ....
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...They are attributed to the presence of electrostatic double layers along the flux tubes (Block, 1978)....
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01 Jan 1983
TL;DR: The radio spectrum of Jupiter has been observed over 24 octaves of the radio spectrum, from about 0.01 MHz to 300,000 MHz, and three distinct types of radiation are responsible for this radio spectrum: thermal emission from the atmosphere accounts for virtually all the radiation at the high frequency end as mentioned in this paper.
Abstract: Jupiter has now been observed over 24 octaves of the radio spectrum, from about 0.01 MHz to 300,000 MHz. Its radio emissions fill the entire spectral region where interplanetary electromagnetic propagation is possible at wavelengths longer than infrared. Three distinct types of radiation are responsible for this radio spectrum. Thermal emission from the atmosphere accounts for virtually all the radiation at the high frequency end. Synchrotron emission from the trapped high-energy particle belt deep within the inner magnetosphere is the dominant spectral component from about 4000 to 40 MHz. The third class of radiation consists of several distinct components of sporadic low frequency emission below 40 MHz. The decimeter wavelength emission is considered, taking into account the discovery of synchrotron emission, radiation by high-energy electrons in a magnetic field, and the present status of Jovian synchrotron phenomenology. Attention is also given to the decameter and hectometer wavelength emission, and emissions at kilometric wavelengths.
281 citations
TL;DR: In this paper, a nonlocal theory based on a simplified model of the ionospheric Alfven resonator (IAR) is presented, which indicates that wave acceleration of electrons should occur at and above the altitude where the quasi-static potential drops form.
Abstract: [1] Recent observations have indicated that in addition to the classical “inverted-V” type electron acceleration, auroral electrons often have a field-aligned distribution that is broad in energy and sometimes shows time dispersion indicating acceleration at various altitudes up the field line. Such acceleration is not consistent with a purely electrostatic potential drop and suggests a wave heating of auroral electrons. Alfven waves have been observed on auroral field lines carrying sufficient Poynting flux to provide energy for such acceleration. Calculations based on the linear kinetic theory of Alfven waves indicate that Landau damping of these waves can efficiently convert this Poynting flux into field-aligned acceleration of electrons. At high altitudes along auroral field lines that map into the plasma sheet boundary layer (PSBL), the plasma gradients are relatively weak and the local kinetic theory can describe this wave–particle interaction. At lower altitudes, the gradient in the Alfven speed becomes significant, and a nonlocal description must be used. A nonlocal theory based on a simplified model of the ionospheric Alfven resonator (IAR) is presented. For a given field-aligned current (FAC), the efficiency of the wave–particle interaction increases with the ratio of the thermal velocity of the electrons to the Alfven speed at high altitudes. These calculations indicate that wave acceleration of electrons should occur at and above the altitude where the quasi-static potential drops form.
117 citations
"Io Jupiter interaction, millisecond..." refers background in this paper
...The acceleration may be due, for instance, to small-scale Alfve´ n waves (Ge´ not et al., 2004) encountering plasma density gradients, or to larger scale trapped Alfve´ n waves ( Lysak and Song, 2003 )....
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TL;DR: A large array of antennae has been built at the Radioastronomy Observatory, Nancay, France, to study solar and planetary decametric emissions as discussed by the authors, which has a high gain in a broad range of frequencies and is steerable through a large part of the sky.
116 citations
"Io Jupiter interaction, millisecond..." refers methods in this paper
...They were recorded with an acousto-optical spectrograph at the Nancay decameter array ( Boischot et al., 1980 ) in 1995 and 1996....
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TL;DR: In this article, the authors analyzed the frequency-time shape of nine radio arcs, corresponding to four observation geometries (A,B, C,D) and detected over their full frequency extent in joint Nancay and Wind data.
Abstract: The motion of the satellite Io in Jupiter's magnetic field results in an electrodynamic circuit, approximately fixed in Io's frame, revealed by ultraviolet and infrared spots at the footprints of Io's flux tube (IFT) as well as prominent (so-called “Io-controlled”) decameter radio arcs. We analyze the frequency-time shape of nine such arcs, corresponding to four observation geometries (A,B,C,D) and detected over their full frequency extent in joint Nancay and Wind data. We compute the radio beaming angle as a function of frequency and lag of the radio-emitting flux tube(s) relative to the IFT. No a priori assumption is made regarding the radio source beaming, and its location is only constrained by the emission occurring near the local electron gyrofrequency. We find northern sources for A and B arcs and southern sources for C and D arcs. The shape of all Io arcs is consistent with an origin at a single flux tube (in Io's frame), shifted by an average of 10° (in the south) and 25° (in the north) with respect to the IFT. This lag must be accumulated before Io's magnetic perturbation reaches the radio emission region, at high latitudes, at altitudes ≤ 1 RJ above the Jovian surface. Radio emission is found to be beamed in a hollow cone of average half-apex angle 70°–75° and thickness ≈1 °. Arc shapes are fully determined by the geometry of observation. Radio fringes preceding the main Io B arcs are well explained by multiple reflections of the magnetic perturbation between Jupiter's ionosphere and Io's torus. The weak trailing part of Io- B arcs may be accounted for through double beaming of the radio emission or through a frequency-dependent lag of the corresponding radio source. The latter explanation suggests an emission scenario in which electron acceleration “leaks” from the magnetic perturbation on its way to Jupiter. Jovian magnetic field models are compared and evaluated in the analysis.
103 citations
"Io Jupiter interaction, millisecond..." refers background or methods in this paper
...The Io phase and the central meridian longitude (CML) during the records correspond to the so-called ‘‘Io-B’’ source (Carr et al., 1983; Queinnec and Zarka, 1998 )....
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...Observer–planet–satellite angle) (Carr et al., 1983) and are due to the Io–Jupiter interaction ( Queinnec and Zarka, 1998; Saur et al., 2004)....
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