1977-2017: 40 years of decametric observations of Jupiter and the Sun with the Nançay Decameter Array

Lamy, Laurent; Zarka, Philippe; Cecconi, Baptiste; Klein, Lawrence S.; Masson, S.; Denis, Laurent; Coffre, A.; Viou, C.

doi:10.1553/pre8s455

Cited by 10 publications

(9 citation statements)

References 25 publications

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“…The NDA is composed of two sub-arrays of 72 antennae each, sensitive to Right-Handed (RH) and Left-Handed (LH) polarization. The NDA has been observing Jupiter on a quasi-daily basis since January 1978 with receivers of increasingly improved performances, the latest of which was specifically developed to collect observations at very high t-f resolution in support of Juno (Zarka, 2011;Lamy et al, 2017). Here, we focus on survey observations acquired at a 1 s temporal cadence by the swept-frequency Routine receiver over 10-40 MHz, with linearly-spaced frequency channels every 75 kHz.…”

Section: The Nançay Decameter Arraymentioning

confidence: 99%

Determining the beaming of Io decametric emissions : a remote diagnostic to probe the Io-Jupiter interaction

Lamy,

Colomban,

Zarka

et al. 2022

Preprint

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We derive the Io-decametric emission angle θ from Juno, Nançay Decameter Array and NenuFAR data using 3 methods to locate the radiosources • θ(f ) decreases from 75 • −80 • to 70 • −75 • over the range 10−40 MHz and varies as a function of time (or longitude of Io) • The inferred electron energies amplifying Io-decametric waves range from 3 to 16 keV also vary as a function of altitude and time

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Section: The Nançay Decameter Arraymentioning

confidence: 99%

Determining the beaming of Io decametric emissions : a remote diagnostic to probe the Io-Jupiter interaction

Lamy,

Colomban,

Zarka

et al. 2022

Preprint

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“…Solar soft X-ray flux, radio flux and polarization dynamic spectra during the eruptive event are shown in Figure 1. The polarization measurements are provided by the Nançay Decameter Array (NDA) MEFISTO receiver (Boischot et al 1980;Lecacheux 2000;Lecacheux et al 2013;Lamy et al 2018), designed to automatically filter noise. Numerous short duration and low frequency bandwidth spikes are seen.…”

Section: Spike Characteristicsmentioning

confidence: 99%

First Frequency-Time-Resolved Imaging Spectroscopy Observations of Solar Radio Spikes

Clarkson,

Kontar,

Gordovskyy

et al. 2021

Preprint

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Solar radio spikes are short duration and narrow bandwidth fine structures in dynamic spectra observed from GHz to tens of MHz range. Their very short duration and narrow frequency bandwidth are indicative of sub-second small-scale energy release in the solar corona, yet their origin is not understood. Using the LOw Frequency ARray (LOFAR), we present spatially, frequency and time resolved observations of individual radio spikes associated with a coronal mass ejection (CME). Individual radio spike imaging demonstrates that the observed area is increasing in time and the centroid positions of the individual spikes move superluminally parallel to the solar limb. Comparison of spike characteristics with that of individual Type IIIb striae observed in the same event show similarities in duration, bandwidth, drift rate, polarization and observed area, as well the spike and striae motion in the image plane suggesting fundamental plasma emission with the spike emission region on the order of ∼ 10 8 cm, with brightness temperature as high as 10 13 K. The observed spatial, spectral, and temporal properties of the individual spike bursts are also suggesting the radiation responsible for spikes escapes through anisotropic density turbulence in closed loop structures with scattering preferentially along the guiding magnetic field oriented parallel to the limb in the scattering region. The dominance of scattering on the observed time profile suggests the energy release time is likely to be shorter than what is often assumed. The observations also imply that the density turbulence anisotropy along closed magnetic field lines is higher than along open field lines.

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“…They are used as a proxy for the Jovian magnetospheric activity. They were discovered by Burke and Franklin (1955) and have been since studied with ground observatories (e.g., Nançay Decametre Array, Lamy et al, 2017) and space-borne instruments (with, e.g., the Voyager, Galileo, Cassini and Juno space missions).…”

Section: Introductionmentioning

confidence: 99%

Jovian auroral radio source occultation modelling and application to the JUICE science mission planning

Cecconi

Louis

Crego

et al. 2022

Preprint

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Occultations of the Jovian low frequency radio emissions by the Galilean moons have been observed by the PWS (Plasma Wave Science) instrument of the Galileo spacecraft. We show that the ExPRES (Exoplanetary and Planetary Radio Emission Simulator) code accurately models the temporal occurrence of the occultations in the whole spectral range observed by Galileo/PWS. This validates of the ExPRES code. In addition to supporting the analysis of the science observations, the method can be applied for preparing the JUICE moon flyby science operation planning.

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1977-2017: 40 years of decametric observations of Jupiter and the Sun with the Nançay Decameter Array

Cited by 10 publications

References 25 publications

Determining the beaming of Io decametric emissions : a remote diagnostic to probe the Io-Jupiter interaction

Determining the beaming of Io decametric emissions : a remote diagnostic to probe the Io-Jupiter interaction

First Frequency-Time-Resolved Imaging Spectroscopy Observations of Solar Radio Spikes

Jovian auroral radio source occultation modelling and application to the JUICE science mission planning

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