Untitled

Ma, Yuanyuan; Xie, R. X.; Zheng, Xingming; Huang, Guangli

doi:10.1023/a:1024283017972

Cited by 9 publications

(4 citation statements)

References 16 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Microwave pulsating events have previously been observed by Young et al (1961), Thompson & Maxwell (1962), Chiu (1970), Gotwols (1972), Elgary (1986), Fu et al (1990), and Ma et al (2003), among others. All the available results and reports of observations show that pulsations appear widely in periods (from several minutes to subseconds) and emission frequency (from meter, decimeter, and centimeter waves).…”

Section: Introductionmentioning

confidence: 82%

The Microwave Pulsations and the Tearing Modes in the Current‐Carrying Flare Loops

Tan

Yan

Liu

2007

ApJ

View full text Add to dashboard Cite

Solar microwave observations of the X3.4 Flare/CME event observed in Chinese solar broadband radiospectrometer (SBRS/Huairou) on 2006 December 13 show a series of very short period pulsations (VSP) with the period of <1.0 s in the frequency range of 2.60Y3.80 GHz. Many pulsating events have the period of only several tens of milliseconds. These pulsations are quasi-periodic, broad bandwidth, and ubiquitous during all the phases of the flare/CME event.Based on theoretical analysis of the temporal behavior of the resistive tearing mode in the electric current-carrying flare loops, we propose that microwave pulsations are a result of the modulation of the tearing-mode oscillations in the current-carrying flare loops. Our calculation of the period of the tearing-mode oscillations are in good agreement with the observations.

show abstract

Section: Introductionmentioning

confidence: 82%

The Microwave Pulsations and the Tearing Modes in the Current‐Carrying Flare Loops

Tan

Yan

Liu

2007

ApJ

View full text Add to dashboard Cite

show abstract

“…Nevertheless, there are also several studies of sub-second pulsations, for example, in the period range 0.025-0.055 s , Ma et al 2003, 0.1 s (Karlicky et al 2010), 0.07-0.08 s (Fleishman et al 1994), and 0.16-0.18 s (Fu et al, 1990). There are rather exceptional observations at microwave frequencies (e.g., in the frequency range 5380-6250 MHz in Fu et al, 1990).…”

Section: Introductionmentioning

confidence: 99%

Broadband microwave sub-second pulsations in an expanding coronal loop of the 2011 August 10 flare

Mészárosová

Rybák

Kashapova

et al. 2016

A&A

View full text Add to dashboard Cite

“…In these bursts, solar radio spikes appear as very short and bright structures in the spectrum, which have been followed with interest for many years [16][17][18][19][20][21][22][23][24]. The spikes are recorded in a very broad frequency band from 0.01 MHz to 8.4 GHz.…”

Section: Introductionmentioning

confidence: 99%

Clusters of Solar Radio Spikes Modulated by Quasi-Periodic Pulsations in a Confined Flare

et al. 2022

View full text Add to dashboard Cite

Spikes are typical radio bursts in solar flares, which are proposed to be the signal of energy release in the solar corona. The whole group of spikes always shows different spectral patterns in the dynamic spectrum. Here, we present a special new feature at 0.6–2 GHz in a confined flare. Each group of spikes is composed of many quasi-periodic sub-clusters, which are superposed on the broadband quasi-periodic pulsations (QPPs). The quasi-periodic cluster of spikes (QPSs) have very intense emissions, and each cluster includes tens of individual spikes. When the intensity of background pulsation is increased, the intensity, duration and bandwidth of the spike cluster are also enlarged. There are 21 groups of QPSs throughout the confined flare. The central frequency of the whole group shifts from 1.9 to 1.2 GHz, and the duration of each cluster shows a negative exponential decay pattern. We propose that nonthermal electron beams play a crucial role in emitting both pulsations and spikes. The tearing-mode oscillations of a confined flux rope produce periodic accelerated electron beams. These electron beams travel inside the closed magnetic structure to produce frequency drifting pulsations via plasma emission and scattered narrowband spikes by electron-cyclotron maser emission (ECME). The slow rise of flux rope makes the source region move upward, and thus, QPSs shift towards low frequency. We propose that the confined flux rope may provide the essential conditions for the formation of QPSs.

show abstract

Untitled

Cited by 9 publications

References 16 publications

The Microwave Pulsations and the Tearing Modes in the Current‐Carrying Flare Loops

The Microwave Pulsations and the Tearing Modes in the Current‐Carrying Flare Loops

Broadband microwave sub-second pulsations in an expanding coronal loop of the 2011 August 10 flare

Clusters of Solar Radio Spikes Modulated by Quasi-Periodic Pulsations in a Confined Flare

Contact Info

Product

Resources

About