Electron Cyclotron Maser Emission in Coronal Arches and Solar Radio Type v Bursts

Tang, Ji; Wu, D. J.; Tan, Cuiyan

doi:10.1088/0004-637x/779/1/83

Cited by 9 publications

(6 citation statements)

References 33 publications

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“…The starting times of the radio burst were consistent with the HXR peak times of the flare. Since the type III radio emissions result from the cyclotron maser instability of the nonthermal electron beams that are accelerated and ejected into the interplanetary space along open magnetic field lines during the flare (Tang et al 2013), the type III radio burst observed by STEREO and WIND provides indirect and supplementary evidence that open magnetic field lines exist near the flare site.…”

Section: Resultsmentioning

confidence: 99%

Multiwavelength Observations of a Partially Eruptive Filament on 2011 September 8

Zhang

Ning

Guo

et al. 2015

ApJ

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In this paper, we report our multiwavelength observations of a partial filament eruption event in NOAA active region 11283 on 2011 September 8. A magnetic null point and the corresponding spine and separatrix surface are found in the active region. Beneath the null point, a sheared arcade supports the filament along the highly complex and fragmented polarity inversion line. After being activated, the sigmoidal filament erupted and split into two parts. The major part rose at the speeds of 90−150 km s −1 before reaching the maximum apparent height of ∼115 Mm. Afterwards, it returned to the solar surface in a bumpy way at the speeds of 20−80 km s −1 . The rising and falling motions were clearly observed in the extreme-ultravoilet (EUV), UV, and Hα wavelengths. The failed eruption of the main part was associated with an M6.7 flare with a single hard X-ray source. The runaway part of the filament, however, separated from and rotated around the major part for ∼1 turn at the eastern leg before escaping from the corona, probably along large-scale open magnetic field lines. The ejection of the runaway part resulted in a very faint coronal mass ejection (CME) that propagated at an apparent speed of 214 km s −1 in the outer corona. The filament eruption also triggered transverse kink-mode oscillation of the adjacent coronal loops in the same AR. The amplitude and period of the oscillation were 1.6 Mm and 225 s. Our results are important for understanding the mechanisms of partial filament eruptions and provide new constraints to theoretical models. The multiwavelength observations also shed light on space weather prediction.Subject headings: Sun: corona -Sun: coronal mass ejections (CMEs) -Sun: flares -Sun: filaments Online-only material: animations, color figures -22 -4. The runaway part, however, separated from and rotated around the major part for ∼1 turn before escaping outward from the corona at the speeds of 125−255 km s −1 , probably along the large-scale open magnetic field lines as evidenced by the PFSS modelling and the type III radio burst. The ejected part of the filament led to a faint CME. The angular width and apparent speed of the CME in the FOV of C2 are 37 • and 214 km s −1 . The propagation directions of the escaping filament observed by SDO/AIA and STA/EUVI are consistent with those of the CME observed by LASCO/C2 and STA/COR1, respectively. 5. The partial filament eruption also triggered transverse oscillation of the neighbouring coronal loops in the same AR. The amplitude and period of the kink-mode oscillation were 1.6 Mm and 225 s. We also performed diagnostics of the plasma density and temperature of the oscillating loops.The authors thank the referee for valuable suggestions and comments to improve the quality of this article. We gratefully acknowledge for inspiring and constructive discussions. SDO is a mission of NASA's Living With a Star Program. AIA and HMI data are courtesy of the NASA/SDO science teams. STEREO/SECCHI data are provided by a consortium of US,

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Section: Resultsmentioning

confidence: 99%

Multiwavelength Observations of a Partially Eruptive Filament on 2011 September 8

Zhang

Ning

Guo

et al. 2015

ApJ

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“…Authors also pointed out that growth rates of X mode are considerably higher than those of O mode. Although other works were carried out to explore this new ECME via introducing a loss cone or temperature anisotropy in the distribution function, results always suggest that the fastest growth mode is the X mode (Tang & Wu 2009;Tang et al 2011Tang et al , 2013.…”

Section: Discussionmentioning

confidence: 99%

Cyclotron Maser Emission From Power-Law Electrons With Strong Pitch-Angle Anisotropy

Zhao

Feng

et al. 2016

ApJ

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Energetic electrons with power-law spectrum are most commonly observed in astrophysics. This paper investigates electron cyclotron maser emission (ECME) from the power-law electrons, in which strong pitch-angle anisotropy is emphasized. The electron distribution function proposed in this paper can describe various types of pitch-angle anisotropy. Results show that the emission properties of ECME, including radiation growth, propagation, and frequency properties, depend considerably on the types of electron pitch-angle anisotropy, and different wave modes show different dependences on the pitch angle of electrons. In particular, the maximum growth rate of X2 mode rapidly decreases with respect to the electron pitch-angle cosine µ 0 at which the electron distribution peaks, while the growth rates for other modes (X1, O1, O2) initially increase before decreasing as µ 0 increases. Moreover, the O mode as well as the X mode can be the fastest growth mode, in terms of not only the plasma parameter but also the type of electron pitch-angle distribution. This result presents a significant extension of the recent researches on ECME driven by the lower-energy cutoff of power-law electrons, in which the X mode is generally the fastest growth mode.

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“…One explanation of type V emission is low energy electrons travelling along different magnetic field lines or a variation of the beaming of emission changes the position of the centroids . Another explanation given for type V emission is the electron-cyclotron maser instability (Winglee & Dulk, 1986;Tang et al, 2013).…”

Section: Type V Burstsmentioning

confidence: 99%

A review of solar type III radio bursts

Reid

Ratcliffe

2014

Res. Astron. Astrophys.

339

217

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Solar type III radio bursts are an important diagnostic tool in the understanding of solar accelerated electron beams. They are a signature of propagating beams of nonthermal electrons in the solar atmosphere and the solar system. Consequently, they provide information on electron acceleration and transport, and the conditions of the background ambient plasma they travel through. We review the observational properties of type III bursts with an emphasis on recent results and how each property can help identify attributes of electron beams and the ambient background plasma. We also review some of the theoretical aspects of type III radio bursts and cover a number of numerical efforts that simulate electron beam transport through the solar corona and the heliosphere.

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Electron Cyclotron Maser Emission in Coronal Arches and Solar Radio Type v Bursts

Cited by 9 publications

References 33 publications

Multiwavelength Observations of a Partially Eruptive Filament on 2011 September 8

Multiwavelength Observations of a Partially Eruptive Filament on 2011 September 8

Cyclotron Maser Emission From Power-Law Electrons With Strong Pitch-Angle Anisotropy

A review of solar type III radio bursts

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