Flux, power, energy and polarization of Jovian S-bursts

Queinnec, Julien; Zarka, Philippe

doi:10.1016/s0032-0633(00)00157-4

Cited by 35 publications

(32 citation statements)

References 20 publications

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“…7 with SNR N ¼ 2:6: In Fig. 7 the bursts (signal) occupy approximately 25% of the observational time, which is consistent with the typical value of Sburst ''filling factor'' in the time-frequency plane Z ¼ 0:26 AE 0:1 (Queinnec and Zarka, 2001). Throughout this paper we make a distinction between two parameters, N and Z; defining the principal characteristics of the analyzed time series, i.e.…”

Section: Appendix a Signal Detection With An Ideal Receiversupporting

confidence: 73%

“…If we take into account the overall beaming of Jupiter S-bursts (bursts are detected 10% of the time by a fixed observer) together with the filling factor of the pulses in the time-frequency plane during a typical S-burst storm ($25%, Queinnec and Zarka, 2001), one obtains a longterm average of the filling factor of about 0.025, i.e. close to that for which peak detection algorithm is more efficient than mere integration.…”

Section: Time Series Analysis Detection Diagramsmentioning

confidence: 95%

“…Note, for example, that in formulas (1), and (2) it is assumed that the flux of intensity I is received permanently, whereas it is well known that planetary radio emissions are very sporadic so that time averaging reduces the average flux density by orders of magnitude. Recent results on the intensity distribution of individual Sbursts (Queinnec and Zarka, 2001) indicate that the peak flux level I J % 10 À16 W m À2 Hz À1 is rarely reached, whereas most of the time pulse intensity is in the range 10 À17 -10 À18 W m À2 Hz À1 . Time averaging over an interval of duration about 3 s decreases the average flux densities down to 10 À19 -10 À20 W m À2 Hz À1 due to low (20-30%) filling factor of the time-frequency plane and to the abundance of low intensity bursts.…”

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confidence: 99%

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Search of exoplanetary radio signals in the presence of strong interference: enhancing sensitivity by data accumulation

Ryabov¹,

Zarka²,

Ryabov³

2004

Planetary and Space Science

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We develop a statistical approach aimed at the detection of weak sporadic pulses on the noise background. The results are applied to modeling the observational time series where pulsed radio emissions have to be recognized against the sky background fluctuations. The proposed methodology demonstrates the efficiency of using the statistics of peak values (integrated tail of probability distribution function of the intensity) for the purpose of signal detection. It is established that the highest sensitivity is reached with this method at low values of the filling factor (duty cycle) of the pulsed signals. If in addition the pulses have sufficiently high intensity, the discussed approach performs better than simple integration over the observational time. Then we discuss the possibility of detecting radio pulses from exoplanetary magnetospheres, especially from known ''hot Jupiters'' found by radial velocity measurements in the visible and we report our results from extensive observations of several candidate exoplanets with the world largest decameter telescope UTR-2. Although no detection of pulsed emission from exoplanets has been found to date, the analysis demonstrates the feasibility of detection with more stable receivers and longer observational time. r

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Section: Appendix a Signal Detection With An Ideal Receiversupporting

confidence: 73%

Section: Time Series Analysis Detection Diagramsmentioning

confidence: 95%

mentioning

confidence: 99%

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Search of exoplanetary radio signals in the presence of strong interference: enhancing sensitivity by data accumulation

Ryabov¹,

Zarka²,

Ryabov³

2004

Planetary and Space Science

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“…2a was recorded in a time window located at the edge of a high-probability S bursts occurrence area in the Io phase -CML (central meridian longitude) diagram (see Fig. 2 in Queinnec & Zarka 2001). The CML was about 75…”

Section: Slow S Bursts Accompanying L Emissionmentioning

confidence: 99%

Fast and slow frequency-drifting millisecond bursts in Jovian decametric radio emissions

Ryabov

Zarka

Hess

et al. 2014

A&A

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We present an analysis of several Jovian Io-related decametric radio storms recorded in 2004−2012 at the Ukrainian array UTR-2 using the new generation of baseband digital receivers. Continuous baseband sampling within sessions lasting for several hours enabled us to study the evolution of multiscale spectral patterns during the whole storm at varying time and frequency resolutions and trace the temporal transformation of burst structures in unprecedented detail. In addition to the well-known frequency drifting millisecond patterns known as S bursts we detected two other classes of events that often look like S bursts at low resolution but reveal a more complicated structure in high resolution dynamic spectra. The emissions of the first type (LS bursts, superposition of L and S type emissions) have a much lower frequency drift rate than the usual quasi linearly drifting S bursts (QS) and often occur within a frequency band where L emission is simultaneously present, suggesting that both LS and at least part of L emissions may come from the same source. The bursts of the second type (modulated S bursts called MS) are formed by a wideband frequency-modulated envelope that can mimic S bursts with very steep negative (or even positive) drift rates. Observed with insufficient time-frequency resolution, MS look like S bursts with complex shapes and varying drifts; MS patterns often occur in association with (i) narrowband emission; (ii) S burst trains; or (iii) sequences of fast drift shadow events. We propose a phenomenological description for various types of S emissions, that should include at least three components: high-and low-frequency limitation of the overall frequency band of the emission, fast frequency modulation of emission structures within this band, and emergence of elementary S burst substructures, that we call "forking" structures. All together, these three components can produce most of the observed spectral structures, including S bursts with apparently very complex time-frequency structures.

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“…Zarka and Queinnec (2001) demonstrated that its low frequency limit implies that the Io-controlled DAM emission must be produced on field-lines which intersect the dense plasma wake downstream of lo (and incidently that the HOM emissions originate from further out in the lo torus), whereas Queinnec and Zarka (2001) analyzed the flux, power, energy and polarization of Jovian S-bursts originating from the lo flux tube and studied their physical properties as a function of Io's longitude.…”

Section: Renee Prangementioning

confidence: 99%

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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Flux, power, energy and polarization of Jovian S-bursts

Cited by 35 publications

References 20 publications

Search of exoplanetary radio signals in the presence of strong interference: enhancing sensitivity by data accumulation

Search of exoplanetary radio signals in the presence of strong interference: enhancing sensitivity by data accumulation

Fast and slow frequency-drifting millisecond bursts in Jovian decametric radio emissions

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

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