A Model of Zebra Patterns in Solar Radio Emission

Chernov, G. P.; Фомичев, В. В.; Сыч, Р. А.

doi:10.1134/s0016793218030040

Cited by 11 publications

(6 citation statements)

References 21 publications

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“…Zebra patterns (ZPs), appearing as regular stripes in emission and absorption in the dynamic spectra of solar radio bursts, are commonly known, and their observed characteristics and their models have been described in many papers (Slottje 1972;Kuijpers 1975;Zheleznyakov & Zlotnik 1975;Chernov 1976Chernov , 1990LaBelle et al 2003;Kuznetsov 2005;Bárta & Karlický 2006;Ledenev et al 2006;Tan 2010;Karlický 2013;Zlotnik 2013;Tan et al 2014;Chernov et al 2018), see also the reviews by Chernov (2011Chernov ( , 2014. The most frequently discussed mechanism in the literature is that based on the double plasma-resonance (DPR) instability (Kuijpers 1975(Kuijpers , 1980Zheleznyakov & Zlotnik 1975;Mollwo 1983Mollwo , 1988Winglee & Dulk 1986;Yasnov & Karlický 2004;Kuznetsov & Tsap 2007;Chen et al 2011;Karlický & Yasnov 2015;Yasnov et al 2016Yasnov et al , 2017Benáček et al 2017).…”

Section: Introductionmentioning

confidence: 99%

Double plasma-resonance surfaces in flare loops and radio zebra emission

Karlický

Yasnov

2018

A&A

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Aims. The zebra structures observed in radio waves during solar flares are some of the most important structures used as diagnostics of solar flare plasmas. We here not only analyze the so-called double plasma-resonance (DPR) surfaces, but also estimate the effects of their form on the size of the zebra sources and brightness temperature. Methods. To compute the DPR surfaces, we used numerical and analytical methods. Results. We found that except for the case of a constant magnetic field across the loop, the DPR surfaces deviate from the constant plasma density surfaces. We found that the regime with a finite height scale has three forms of resonance surfaces depending on the magnetic field variation across the loop. This magnetic field variation also determines if in the generated zebra structure, an increase in gyro-harmonic number leads to an increase or decrease of the zebra stripe frequency. In the case with an infinite height scale, the resonance surfaces are parallel to the loop axis. Furthermore, we found that for highly polarized zebra structures that are generated at DPR surfaces close to the plasma frequency, the zebra emission is limited to the narrow escaping cone and the emitting source area increases with increasing viewing angle compared to the loop axis. Moreover, with increasing deviation of the DPR surfaces from those of constant density surfaces, the frequency bandwidth of the DPR emission increases and can cause the zebra stripes to overlap, which limits the zebra generation. For the zebra structures observed on 14 February 1999, 6 June 2000, and 1 August 2010 and the observed view perpendicular to the loop axis, we estimated that the brightness temperature is 3.67 × 1014 K, 6.58 × 1013 K, and 7.35 × 1015 K, respectively. These brightness temperatures are much lower than those derived for the view along the loop axis (up to 1017 K), and thus are more realistic. The area of the emitting source for coronal loops in the view perpendicular to the loop axis can be larger by several orders of magnitude than that in the view along the loop axis.

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Section: Introductionmentioning

confidence: 99%

Double plasma-resonance surfaces in flare loops and radio zebra emission

Karlický

Yasnov

2018

A&A

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“…There are more than a dozen proposed theoretical models to explain the formation of ZP structures, including the Bernstein wave models (Rosenberg, 1972;Chiuderi et al, 1973;Zaitsev and Stepanov, 1983, etc. ), whistler wave models (Kuijpers, 1975;Chernov et al, 2018), double plasma resonance models (DPR model, Winglee and Dulk, 1986;Zlotnik et al, 2003;Yasnov and Karlicky, 2004;Kuznetsov and Tsap, 2007;Li et al, 2021), but so far, there is no universally accepted model, the fundamental reason is that we still do not know the exact location and spatial structure of the ZP source region. They found that the apparent ZP source size is around 3500, the source centroid drifts 8-900 irregularly in time and in the direction across the six stripes from high to low frequency at a fixed time.…”

Section: The Main Solar Physical Problems Faced By Spectral Imaging O...mentioning

confidence: 99%

The physics of solar spectral imaging observations in dm-cm wavelengths and the application on space weather

Tan

Yan

Huang

et al. 2023

Advances in Space Research

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“…This kind of emission can be produced by natural means, with different mechanisms that have been proposed. The source of such emission is located in the solar atmosphere at the eruptive event's environments as described by Altyntsev et al [2005], Ledenev et al [2006] andChernov et al [2018]. Nevertheless, another cause of this type of radio signatures is due to electronic-device inference near the instrument of detection, as signalized in the common radio signals catalog of Monstein [2011].…”

Section: Noise At Mexart Facilitiesmentioning

confidence: 99%

First Solar Radio Burst Observations by the Mexican Array Radio Telescope (MEXART) at 140 MHz

Huipe-Domratcheva,

De la Luz,

Casillas-Perez

et al. 2022

Preprint

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The National Laboratory of Space Weather in Mexico (Laboratorio Nacional de Clima Espacial: LANCE) coordinates instrumentation for monitoring the space-weather impact over Mexico. Two of these instruments are the Mexican Array Radio Telescope (MEXART) and Compound Astronomical Low frequency Low cost Instrument for Spectroscopy and Transportable Observatory (CALLISTO) station from the e-CALLISTO network (CALLMEX). Both instruments are located at the same facility (Coeneo Michoacan, Mexico) and share a spectral band centered at 140 MHz. In this work we show the capabilities of the e-CALLISTO network as support to identify a solar radio burst in the signal of the MEXART radiotelescope. We identify 75 solar radio bursts in the MEXART signal: five events of Type II and 70 of Type III between September 2015 and May 2019. The analysis of solar radio bursts in the MEXART signal provide us valuable information about the development of the radio event due their high sensitivity, time resolution, and isotropic response. For the case of Type III solar radio events, we identify three characteristic phases in the dynamical evolution of the signal at 140 MHz: a pre-phase, a main peak, a decay phase, and a post-event phase. A Morlet wave transform was done of MEXART signals in the Type III solar radio busts; in their spectra it was identified a pine tree structure preceding the main event in the time series. These characteristics are not observable in the data from the e-Callisto network.

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A Model of Zebra Patterns in Solar Radio Emission

Cited by 11 publications

References 21 publications

Double plasma-resonance surfaces in flare loops and radio zebra emission

Double plasma-resonance surfaces in flare loops and radio zebra emission

The physics of solar spectral imaging observations in dm-cm wavelengths and the application on space weather

First Solar Radio Burst Observations by the Mexican Array Radio Telescope (MEXART) at 140 MHz

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