A World-Wide Net of Solar Radio Spectrometers: e-CALLISTO

Benz, A. O.; Monstein, C.; Meyer, Hansueli; Manoharan, P. K.; Ramesh, R.; Altyntsev, A. T.; Lara, A.; Páez, Jorge; Cho, K.-S.

doi:10.1007/s11038-008-9267-6

Cited by 154 publications

(100 citation statements)

References 2 publications

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“…We studied the multiple type II bursts observed with the Culgoora radio spectrograph on December 31, 2007. A first identification of the multiple bursts was made by one of e-CALLISTO network installed in the Republic of Korea (Bong et al 2009) as an activity of IHY2007 for 24-h monitoring of solar radio emissions throughout the world (Benz et al 2009). One advantage of our dataset is that the multiple type II-associated CME was observed by the SECCHI/COR1, which makes it possible to determine the 3D kinematics of the CME in the low corona and inspect the relationship between the CME and the multiple type II bursts in detail.…”

Section: Introductionmentioning

confidence: 99%

Relationship between multiple type II solar radio bursts and CME observed by STEREO/SECCHI

Cho

Bong

Moon

et al. 2011

A&A

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Aims. Two or more type II bursts are occasionally observed in close time sequence during solar eruptions, which are known as multiple type II bursts. The origin of the successive burst has been interpreted in terms of coronal mass ejections (CMEs) and/or flares. Detailed investigations of the relationship between CMEs and the bursts enable us to understand the nature of the multiple type II bursts. In this study, we examine multiple type II bursts and compare their kinematics with those of a CME occurring near the time of the bursts. Methods. To do this, we selected multiple type II bursts observed by the Culgoora radiospectrographs and a limb CME detected in the low corona field of view (1.4−4 R s ) of a STEREO/SECCHI instrument on December 31, 2007. To determine the 3D kinematics of the CME, we applied the stereoscopic technique to the STEREO/SECCHI data. Results. Our main results are as follows: (1) the multiple type II bursts occurred successively at ten minute intervals and displayed various emission structures and frequency drifting rates; (2) near the time of the bursts, the CME was observed by STEREO and SOHO simultaneously, but no evidence of other CMEs was detected; (3) inspection of the 3D kinematics of the CME using the stereoscopic observation by STEREO/SECCHI revealed that the CME propagated along the eastward radial direction as viewed from the Earth; (4) very close time and height associations were found between the CME nose and the first type II burst, and between CME-streamer interaction and the second type II burst. Conclusions. On the basis of these results, we suggest that a single shock in the leading edge of the CME could be the source of the multiple type II bursts and support the notion that the CME nose and the CME-streamer interaction are the two main mechanisms able to generate the bursts.

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Section: Introductionmentioning

confidence: 99%

Relationship between multiple type II solar radio bursts and CME observed by STEREO/SECCHI

Cho

Bong

Moon

et al. 2011

A&A

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“…Para avaliação de sua eficiência, utilizou-se de séries temporais associadas a rádio emissões solares tipo I e tipo III, registradas pelo espectrógrafo BLEN7M da rede e-CALLISTO (BENZ et al, 2005;BENZ et al, 2009). …”

Section: Metodologiaunclassified

Aplicação De Wavelets Na Analise De Rádio Emissões Solares

2016

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“…With these solar instruments in radio wavelength, a more accurate determination of the specific frequency of energy become feasible due to high time resolution [235]. CALLISTO was considered as a global network of spectrometer system with the purpose to observe the Sun's activities located in different regions of the Earth [236]. ETH Zurich has developed a number of solar radio spectrometers since 1980s [237,238].…”

Section: Callisto Spectrometermentioning

confidence: 99%

“…At the preliminary stage, the construction of LPDA and installation of CALLISTO system has successfully done by 22 nd February 2012 [242]. The e-CALLISTO network has had its first success in December 2006, when the last large flares of the present cycle occurred [243]. Meanwhile, the CALLISTO system was successfully installed at the National Space Centre, Banting Selangor located at (3°5′00″N 101°32′00″E).…”

Section: Callisto Configuration and Malaysia Solar Spectrum Coveragementioning

confidence: 99%

Probability of Solar Flares Turn out to Form a Coronal Mass Ejections Events due to the Characterization of Solar Radio Burst Type II and III

Hamidi

2014

ILCPA

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The solar flare and Coronal Mass Ejections (CMEs) are well known as one of the most massive eruptions which potentially create major disturbances in the interplanetary medium and initiate severe magnetic storms when they collide with the Earth's magnetosphere. However, how far the solar flare can contribute to the formation of the CMEs is still not easy to be understood. These phenomena are associated with II and III burst it also divided by sub-type of burst depending on the physical characteristics and different mechanisms. In this work, we used a Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy in Transportable Observatories (CALLISTO) system. The aim of the present study is to reveal dynamical properties of solar burst type II and III due to several mechanisms. Most of the cases of both solar radio bursts can be found in the range less that 400 MHz. Based on solar flare monitoring within 24 hours, the CMEs that has the potential to explode will dominantly be a class of M1 solar flare. Overall, the tendencies of SRBT III burst form the solar radio burst type III at 187 MHz to 449 MHz. Based on solar observations, it is evident that the explosive, short time-scale energy release during flares and the long term, gradual energy release expressed by CMEs can be reasonably understood only if both processes are taken as common and probably not independent signatures of a destabilization of pre-existing coronal magnetic field structures. The configurations of several active regions can be sourced regions of CMEs formation. The study of the formation, acceleration and propagation of CMEs requires advanced and powerful observational tools in different spectral ranges as many 'stages' as possible between the photosphere of the Sun and magnetosphere of the Sun and magnetosphere of the Earth. In conclusion, this range is a current regime of solar radio bursts during CMEs events.

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A World-Wide Net of Solar Radio Spectrometers: e-CALLISTO

Cited by 154 publications

References 2 publications

Relationship between multiple type II solar radio bursts and CME observed by STEREO/SECCHI

Relationship between multiple type II solar radio bursts and CME observed by STEREO/SECCHI

Aplicação De Wavelets Na Analise De Rádio Emissões Solares

Probability of Solar Flares Turn out to Form a Coronal Mass Ejections Events due to the Characterization of Solar Radio Burst Type II and III

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