2019
DOI: 10.3847/1538-4357/ab1d64
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Abstract: Quasi-periodic pulsations (QPPs) are frequently observed in solar flares, which may reveal some essential characteristics of both thermal and nonthermal energy releases. This work presents multi-wavelength imaging observations of an M8.7 flare in active region AR 12242 on 2014 December 17. We found that there were three different QPPs: UV QPPs with a period of about 4 minutes at 1600 Å images near the center of the active region lasting from the preflare phase to the impulsive phase; EUV QPPs with a period of … Show more

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Cited by 46 publications
(43 citation statements)
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“…Veronig & Polanec 2015), and the formation of circular or quasi-circular ribbons (e.g. Reid et al 2012;Joshi et al 2015;Hernandez-Perez et al 2017;Li et al 2018b;Zhong et al 2019;Hou et al 2019;Chen et al 2019;Zhang et al 2019). However, although rarely reported in literature, some confined flares occasionally exhibit features similar to those observed in eruptive flares.…”
Section: Introductionmentioning
confidence: 99%
“…Veronig & Polanec 2015), and the formation of circular or quasi-circular ribbons (e.g. Reid et al 2012;Joshi et al 2015;Hernandez-Perez et al 2017;Li et al 2018b;Zhong et al 2019;Hou et al 2019;Chen et al 2019;Zhang et al 2019). However, although rarely reported in literature, some confined flares occasionally exhibit features similar to those observed in eruptive flares.…”
Section: Introductionmentioning
confidence: 99%
“…The data processing code has been made available at https://github.com/astroitlab/museros (Mei et al, 2018). A brief introduction of the pipeline for data processing was discussed in Mei et al (2018) and Chen et al (2019). Next, we will present three typical solar radio burst events observed by MUSER.…”
Section: Muser Observationsmentioning
confidence: 99%
“…121s from the wavelet analysis; 4) the size of the radio source varies from small to large and then small at a given intensity and frequency, which corresponds to the evolutions of radio emission processes; 5) the radio sources locate in the middle of the active region, over the positive magnetic field; 6) the radio sources at six frequencies line up nicely and move along the similar expanding direction of flaring loop. The detailed data processing of spectral and imaging observations of the radio source, the main features and complicated interactions among different loops, and the physical relationships from various multi-wavelength observations to the possible mechanisms of QPPs have been presented in Chen et al (2019).…”
Section: A Radio Burst Event On 17 December 2014mentioning
confidence: 99%
“…In the context of the collisional thick-target flare model, high-energy electrons stream downward into the cool and dense chromosphere where electrons are stopped by Coulomb collisions and lose energy, heating the localized plasma to ∼10 7 K and driving chromospheric evaporation (Brown 1971;Fisher et al 1985). Emissions at the flare ribbons or kernels increase dramatically in optical, ultraviolet (UV), extreme-ultraviolet (EUV), hard X-ray (HXR), and microwave wavelengths (e.g., Krucker et al 2011;Fletcher et al 2013;Sharykin & Kosovichev 2014;Jing et al 2016;Chen et al 2019b). After reaching the peak value, the ribbon brightness begins to decrease as a result of conductive and radiative cooling (Cargill et al 1995).…”
Section: Introductionmentioning
confidence: 99%