A type III radio burst automatic analysis system and statistic results for a half solar cycle with Nançay Decameter Array data

Zhang, Peijin; Wang, Chuanbing; Ye, L.

doi:10.1051/0004-6361/201833260

Cited by 40 publications

(34 citation statements)

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“…Our primary motivation is to use the database prepared using the algorithm described in the paper, and develop an automated classifier which would classify various types of individual bursts. So far, there have attempts to automatically identify specific type of bursts (Lobzin et al, 2009(Lobzin et al, , 2010Lobzin, Cairns, and Zaslavsky, 2014;Salmane et al, 2018;Zhang, Wang, and Ye, 2018). However, automatic recognition of all types of bursts was never reported in the literature to the best of our knowledge.…”

Section: Introductionmentioning

confidence: 99%

Automated Detection of Solar Radio Bursts Using a Statistical Method

et al. 2019

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Radio bursts from the solar corona can provide clues to forecast space weather hazards. After recent technology advancements, regular monitoring of radio bursts has increased and large observational data sets are produced. Hence, manual identification and classification of them is a challenging task. In this paper, we describe an algorithm to automatically identify radio bursts from dynamic solar radio spectrograms using a novel statistical method. We used e-CALLISTO radio spectrometer data observed at Gauribidanur observatory near Bangalore in India during 2013 -2014. We have studied the classifier performance using the receiver operating characteristics. Further, we studied type III bursts observed in the year 2014 and found that 75% of the observed bursts were below 200 MHz. Our analysis shows that the positions of the flare sites which are associated with the type III bursts with upper frequency cut-off 200 MHz

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Section: Introductionmentioning

confidence: 99%

Automated Detection of Solar Radio Bursts Using a Statistical Method

et al. 2019

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“…Using the relationship between the plasma frequency and electron density [f pe [kHz] = 9 n e [cm −3 ]] , one can estimate the heliocentric distance of the wave excitation position with an assumption of the solar and interplanetary background electron density model (e.g. Zhang, Wang, and Ye, 2018).…”

Section: Introductionmentioning

confidence: 99%

Forward Modeling of the Type III Radio Burst Exciter

Zhang

Wang

et al. 2019

Sol Phys

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In this work, we propose a forward modeling method to study the trajectory and speed of the interplanetary (IP) Type-III radio burst exciter. The model assumes that the source of an IP Type-III radio burst moves outward from the Sun following the Parker spiral field line. Using the arrival time of the radio waves at multiple spacecraft, we are able to determine the trajectory of the radio source in the Ecliptic plane, and its outward speed, as well as the injection time and longitude of the associated electron beam near the solar surface that triggers the Type-III radio burst. For the application of this method, we design a system to gather the arrival time of the radio wave from the radio dynamic spectra observed by Solar Terrestrial Relations Observator (STEREO)/WAVES and Wind /WAVES. Then, the system forward models the trajectory and speed of the radio burst exciter iteratively according to an evaluation function. Finally, we present a survey of four Type-III radio bursts that are well discussed in the literature. The modeled trajectories of the radio source are consistent with the previous radio-triangulation results, the longitude of the associated active region, or the location of Langmuir waves excited by the electron beam.

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“…Figure 6 shows a scatter plot of the frequency drift rates, highlighting the huge spread in values between different radio bursts. If we assume that the background electron density was similar for all studies, as was the proportion of fundamental to harmonic emission then Zhang et al (2018) observed more electron beams with lower bulk velocities than the other studies. Lower velocity beams take longer to travel from one frequency to another and hence the frequency drift rate is smaller in magnitude.…”

Section: Low Frequency Burstsmentioning

confidence: 82%

“…One quintessential property of type III radio bursts is the frequency drift rate, typically attributed to the bulk speed of the electron beam traveling through the solar plasma. The enhanced spectral resolution from LOFAR and the MWA allows drift rates to be more accurately measured and has been statistically sampled recently by a number of radio spectroscopic studies by and Reid and Kontar (2018a) that used LOFAR, by Zhang et al (2018) that used the Nançay Decametre Array (NDA, Lecacheux, 2000), and by Stanislavsky FIGURE 5 | Left: LOFAR contours of a U-burst tracing out a large coronal magnetic loop. The co-temporal X-ray source is shown with a background of the 171 Angstroms Sun.…”

Section: Low Frequency Burstsmentioning

confidence: 99%