Signal Detection of the Solar Radio Burst Type III Based on the CALLISTO System Project Management

Hamidi, Zety Sharizat; Zainol, N. H.; Ali, M. O.; Sabri, S. N. U.; Shariff, N.N.M.; Faid, M. S.; Husien, Nurulhazwani; Monstein, C.

doi:10.1109/icimsa.2016.7504031

“…Here we present the results of these observations and their calculated burst parameters. Other type III SRBs have also been characterized by relying on similar e-CALLISTO stations (Ansor et al 2019;Hamidi et al 2019Hamidi et al , 2016Ali et al 2016;Ramli et al 2015).…”

Section: Introductionmentioning

confidence: 99%

CALLISTO facilities in Peru: spectrometer commissioning and observations of type III solar radio bursts

Rengifo

¹

,

Loaiza-Tacuri

²

,

Bazo

³

et al. 2021

Res. Astron. Astrophys.

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The Astrophysics Directorate of CONIDA has installed two radio spectrometer stations belonging to the e-CALLISTO network in Lima, Peru. Given their strategic location near the Equator, it is possible to observe the Sun evenly throughout the whole year. The receiver located at Pucusana, nearby the capital city of Lima, took data from October 2014 until August 2016 in the metric and decimetric bands looking for radio bursts. During this period, this e-CALLISTO detector was unique in its time-zone coverage. To asses the suitability of the sites and the performance of the antennas, we analyzed the radio ambient background and measured their radiation pattern and beamwidth. To demonstrate the capabilities of the facilities for studying solar dynamics in these radio frequencies, we have selected and analyzed type III Solar Radio Bursts. The study of this kind of burst helps to understand the electron beams traversing the solar corona and the solar atmospheric density. We have characterized the most common radio bursts with the following mean values: a negative drift rate of –25.8 ± 3.7 MHz s−1, a duration of 2.6 ± 0.3 s and 35 MHz bandwidth in the frequency range of 114 to 174 MHz. In addition, for some events, it was possible to calculate a global frequency drift which on average was 0.4 ± 0.1 MHz s−1.

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“…Here we show the results of these observations and their calculated burst parameters. Other type III SRBs have also been characterized using similar e-CALLISTO stations ( [6][7][8][9][10]).…”

Section: Introductionmentioning

confidence: 99%

Commissioning of CALLISTO spectrometers in Peru and observations of type III Solar Radio Bursts

Alba¹,

Rengifo²,

Veronica³

et al. 2021

Proceedings of 37th International Cosmic Ray Conference — PoS(ICRC2021)

0

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Two radio spectrometer stations belonging to the e-CALLISTO network were installed in Peru by the Astrophysics Directorate of CONIDA. Given their strategic location near the Equator, it was possible to observe the Sun evenly throughout the whole year and the detector was unique in its time-zone coverage. The receiver located nearby the capital city of Lima took data in the metric and decimetric bands looking for radio bursts. To assess the suitability of the sites and the performance of the antennas, we analysed the radio ambient background and measured their radiation pattern and beam-width. To show the capabilities of the facilities to study solar dynamics in these radio frequencies we have selected and analysed type III Solar Radio Bursts. We have characterised the most common radio bursts with the following mean values: a negative drift rate of -25.8 ± 3.7 MHz/s, a duration of 2.6 ± 0.3 s and 35 MHz bandwidth in the frequency range of 114 to 174 MHz. In addition, for some events, it was possible to calculate a global frequency drift, which on average was 0.4 ± 0.1 MHz/s.

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“…Currently, there are more instruments covering this time zone. Similar stations have been deployed elsewhere (Zavvari et al (2016); Prasert et al (2019)) and other type III SRBs have also been characterized and analyzed using e-CALLISTO stations (Ansor, Hamidi, and Shariff (2019); Hamidi, Ramli, and Shariff (2019); Hamidi et al (2016); Ali et al (2016); Ramli et al (2015)). frequency interference background in both sites and the measurement of the radiation pattern and beamwidth to characterize the antennas.…”

Section: Introductionmentioning

confidence: 99%

CALLISTO Facilities in Peru: Spectrometers Commissioning and Observations of Type III Solar Radio Bursts

Rengifo,

Loaiza-Tacuri,

Bazo

et al. 2020

Preprint

0

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The Astrophysics Directorate of CONIDA has installed two radio spectrometer stations belonging to the e-CALLISTO network in Lima, Peru. Given their strategic location near the Equator, it is possible to observe the Sun evenly throughout the whole year. To calibrated the antennas we analyzed the radio ambient background and measured their radiation pattern and beam-width. The stations took data from 2014 until 2016 in the metric and decimetric bands looking for radio burst. To understand the solar dynamics in these radio frequencies we have selected and analyzed type III Solar Radio Bursts candidates. The study of these bursts helps to understand the electron beams traversing the solar corona and the solar atmospheric density. We have obtained standard mean values for the associated plasma parameters with a starting negative frequency drift rate JARengifo

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Signal Detection of the Solar Radio Burst Type III Based on the CALLISTO System Project Management

Cited by 6 publications

References 8 publications

CALLISTO facilities in Peru: spectrometer commissioning and observations of type III solar radio bursts

CALLISTO facilities in Peru: spectrometer commissioning and observations of type III solar radio bursts

Commissioning of CALLISTO spectrometers in Peru and observations of type III Solar Radio Bursts

CALLISTO Facilities in Peru: Spectrometers Commissioning and Observations of Type III Solar Radio Bursts

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