Classification and Properties of Supershort Solar Radio Bursts

Magdalenić, Jasmina; Vršnak, Bojan; Zlobec, P.; Hillaris, A.; Messerotti, M.

doi:10.1086/504521

Cited by 29 publications

(28 citation statements)

References 15 publications

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“…More details are given in Chernov, Yan, and Fu (2003). Sych et al (2006) reports similar zebra structures that were recorded by the Ondřejov and the Brazilian spectrograph on 5 August 2003 in the range 1000 -2250 MHz during 12:45:10 and 12:48:14 UT when an M1.7 flare was occurring in active region AR 0424 located at S18E39. Thanks to the use of a new method of dynamic wavelet filtration, based on the distribution of the harmonics of global wavelet spectra for each frequency profile, two significant features were recognized: (a) broadband decimetric subsecond pulses (of frequency width between 0.43 and 0.56 GHz, with an average of 0.48 GHz) and (b) narrowband spike-like bursts (of frequency width between 0.08 and 0.18 GHz, with an average of 0.13 GHz), which were arranged in zebra lines.…”

Section: Introductionsupporting

confidence: 73%

“…In the present paper we extend the study made by Sych et al (2006) by analyzing the 5 August 2003 zebra-superfine structure using the 1420-MHz Trieste observations with very high time resolution (1 ms).…”

Section: Introductionmentioning

confidence: 70%

“…Using the radio spectra quoted by Sych et al (2006) and the polarimetric data recorded at 1420 MHz (at the Trieste Solar Radio System of the Italian National Institute of Astronomy and Astrophysics -INAF -Trieste Astronomical Observatory) with high time resolution (1 ms), we attempted to determine the parameters that are specific for these narrowband spike-like bursts. In the single-frequency records at 1420 MHz the aforementioned spiky activity appears divided into the following four intervals: .…”

Section: Observationsmentioning

confidence: 99%

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Spike-like Bursts as Fine Structure of Zebras

Zlobec

Karlický

2007

Sol Phys

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We studied the characteristics of the zebra-associated spike-like bursts that were recorded with high time resolution at 1420 MHz in four intervals (from 12:45 to 12:48 UT) during 5 August 2003. Our detailed analysis is based on the selection of more than 500 such spike-like bursts and it is, at least to our knowledge, the first study devoted to such short-lived bursts. Their characteristics are different from those pertinent to "normal" spike bursts, as presented in the paper by Güdel and Benz (Astron. Astrophys. 231, 202, 1990); in particular, their duration (about 7.4 ms at half power) is shorter, so they should be members of the SSS (super short structures) family (Magdalenić et al., Astrophys. J. 642, L77, 2006). The bursts were generally strongly R-polarized; however, during the decaying part of interval I a low R-polarized and L-polarized bursts were also present. This change of polarization shows a trend that resembles the peculiar form of the zebra lines in the spectral dominion ("V" like). A global statistical analysis on the bursts observed in the two polarimetric channels shows that the highest cross-correlation coefficient (about 0.5) was pertinent to interval I. The zebras and the bursts can be interpreted by the same double plasma resonance process as proposed by Karlický (Astron. Astrophys. 379, 1045, 2001) and Karlický et al. (Astron. Astrophys. 375, 638, 2001); in particular, the spikes are generated by the interruption of this process by assumed turbulence (density or magnetic field variations). This process should be present in the region close to the reconnection site (e.g., in the plasma reconnection outflows) where the density and the magnetic field vary strongly.

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Section: Introductionsupporting

confidence: 73%

Section: Introductionmentioning

confidence: 70%

Section: Observationsmentioning

confidence: 99%

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Spike-like Bursts as Fine Structure of Zebras

Zlobec

Karlický

2007

Sol Phys

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“…They include the classical narrowband spike clusters (Benz 1986;Fleishman & Melnikov 1998), supershort structures (SSSs; Magdalenić et al 2006), and some types of spiky zebra bursts (Altyntsev et al 2005;Chernov 2006). It is currently unclear whether they represent versions of basically the same or different physical phenomena.…”

Section: Introductionmentioning

confidence: 99%

Spike Decomposition Technique: Modeling and Performance Tests

Nita

Fleishman

Gary

2008

Astrophysical Journal

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We develop an automated technique for fitting the spectral components of solar microwave spike bursts, which are characterized by narrowband spectral features. The algorithm is especially useful for periods when the spikes occur in densely packed clusters, where the algorithm is capable of decomposing overlapping spike structures into individual spectral components. To test the performance and applicability limits of this data reduction tool, we perform comprehensive modeling of spike clusters characterized by various typical bandwidths, spike densities, and amplitude distributions. We find that, for a wide range of favorable combinations of input parameters, the algorithm is able to recover the characteristic features of the modeled distributions within reasonable confidence intervals. Having model-tested the algorithm against spike overlap, broadband spectral background, noise contamination, and possible malfunction of some spectral channels, we apply the technique to a spike cluster recorded by the Chinese Purple Mountain Observatory (PMO) spectrometer, operating above 4.5 GHz. We study the variation of the spike distribution parameters, such as amplitude, bandwidth, and related derived physical parameters, as a function of time. The method can be further applied to observations from other instruments and to other types of fine structures.

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“…As the observation technologies have improved, a variety of spectral fine structures have been observed in solar radio bursts such as spike bursts (Güdel and Benz, 1990;Magdalenic et al, 2006;Benz et al, 2009b), type I bursts (Sundaram and Subramanian, 2005 and references therein), and fiber bursts or zebras in type IV bursts (Aurass et al, 2003;Chernov, 2006). More detailed analyses of their spectral structures are thought to be important in understanding particle dynamics in the solar corona.…”

Section: Introductionmentioning

confidence: 99%

IPRT/AMATERAS: A New Metric Spectrum Observation System for Solar Radio Bursts

et al. 2012

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A new radio spectropolarimeter for solar radio observation has been developed at Tohoku University and installed on the Iitate Planetary Radio Telescope (IPRT) at the Iitate observatory in Fukushima prefecture, Japan. This system, named AMATERAS (the Assembly of Metric-band Aperture TElescope and Real-time Analysis System), enables us to observe solar radio bursts in the frequency range between 150 and 500 MHz. The minimum detectable flux in the observation frequency range is less than 0.7 SFU with an integration time of 10 ms and a bandwidth of 61 kHz. Both left and right polarization components are simultaneously observed in this system. These specifications are accomplished by combining the large aperture of IPRT with a high-speed digital receiver. Observational data are calibrated and archived soon after the daily observation. The database is available online. The high-sensitivity observational data with the high time and frequency resolutions from AMATERAS will be used to analyze spectral fine structures of solar radio bursts.

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Classification and Properties of Supershort Solar Radio Bursts

Cited by 29 publications

References 15 publications

Spike-like Bursts as Fine Structure of Zebras

Spike-like Bursts as Fine Structure of Zebras

Spike Decomposition Technique: Modeling and Performance Tests

IPRT/AMATERAS: A New Metric Spectrum Observation System for Solar Radio Bursts

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