Drifting Pulsation Structure at the Very Beginning of the 2017 September 10 Limb Flare

Karlický, M.; Bin, Chen; Gary, Dale E.; Kašparová, J.; Rybák, J.

doi:10.3847/1538-4357/ab63d0

Cited by 19 publications

(12 citation statements)

References 39 publications

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“…Recent studies using EOVSA observations beautifully demonstrate the link between EUV, radio sources in the GHz regime, and the standard model of solar eruptions (Gary et al, 2018;Karlický et al, 2020), as depicted in Figure 1B. EUV and X-ray diagnostics of this system were also provided by Yan et al (2018).…”

Section: Electron Acceleration Sites and Reconnecting Current Sheetsmentioning

confidence: 70%

“…EUV and X-ray diagnostics of this system were also provided by Yan et al (2018). Early in the flare, at the time of drifting pulsation structures observed in the 1-2 GHz range with the Ondrejov radio spectrograph, the EOVSA imaging spectroscopy captured the fast evolution of a radio source below 4 GHz (bifurcation of the radio source seen in Figures 4A,B) in connection with the tearing and ejection of the filament seen in EUV (Karlický et al, 2020). These observations suggest that the radio pulsations are signatures of suprathermal electrons trapped in the rising magnetic rope and flare arcade when flare magnetic reconnection starts.…”

Section: Electron Acceleration Sites and Reconnecting Current Sheetsmentioning

confidence: 96%

“…(D) Detail of the radio dynamic spectrum in the 1,000-1800 MHz range observed at the very beginning of the flare at 15:48-15:49 UT. The pulsations appear mainly in two frequency bands(1,000-1,300 MHz and 1,600-1,800 MHz), which are interconnected by fast drifting bursts (adapted fromKarlický et al (2020), ©AAS, reproduced with permission).…”

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confidence: 99%

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Radio Observations of Coronal Mass Ejection Initiation and Development in the Low Solar Corona

Carley

Vilmer

Vourlidas

2020

Front. Astron. Space Sci.

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Coronal mass ejections (CMEs) are large eruptions of plasma and magnetic field from the low solar corona into the heliosphere. These eruptions are often associated with energetic electrons that produce various kinds of radio emission. However, there is ongoing investigation into exactly where, when, and how the electron acceleration occurs during flaring and eruption, and how the associated radio emission can be exploited as a diagnostic of both particle acceleration and CME eruptive physics. Here, we review past and present developments in radio observations of flaring and eruption, from the destabilization of flux ropes to the development of a CME and the eventual driving of shocks in the corona. We concentrate primarily on the progress made in CME radio physics in the past two decades and show how radio imaging spectroscopy provides the ability to diagnose the locations and kinds of electron acceleration during eruption, which provides insight into CME eruptive models in the early stages of their evolution ( < 10 R ⊙ ). We finally discuss how new instrumentation in the radio domain will pave the way for a deeper understanding of CME physics in the near future.

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Section: Electron Acceleration Sites and Reconnecting Current Sheetsmentioning

confidence: 70%

Section: Electron Acceleration Sites and Reconnecting Current Sheetsmentioning

confidence: 96%

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Radio Observations of Coronal Mass Ejection Initiation and Development in the Low Solar Corona

Carley

Vilmer

Vourlidas

2020

Front. Astron. Space Sci.

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“…The FASR is still not granted for construction yet and the Expanded Owens Valley Solar Array (Gary et al, 2018) has been developed as a pathfinder for the FASR (Nita et al, 2016). The microwave spectral imaging observations of the well known X8.2-class limb flare on 2017 September 10 by EOVSA have been extensively studied to indicate the nonthermal emissions by flareand shock-accelerated electrons (Gary et al, 2018;Fleishman, et al, 2020;Karlický et al, 2020), or the detection of nonthermal emission at conjugate flux rope footpoints showing the solid evidence of particle transport along the erupting magnetic flux rope during the early impulsive phase (Chen et al, 2020).…”

Section: Introductionmentioning

confidence: 99%

Mingantu Spectral Radioheliograph for Solar and Space Weather Studies

Yan

Chen

Wang

et al. 2021

Front. Astron. Space Sci.

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The Chinese Spectral Radioheliograph (CSRH) covering 400 MHz-15 GHz frequency range was constructed during 2009–2016 in Mingantu Observing Station, National Astronomical Observatories, Chinese Academy of Sciences at Zhengxiangbaiqi, Inner Mongolia of China. The CSRH is renamed as MingantU SpEctral Radioheliograph (MUSER) after its accomplishment. Currently, MUSER consists of two arrays spreading over three spiral-shaped arms. The maximum baseline length is ∼3 km in both east-west and north-south directions. The MUSER array configuration is optimized to meet the needs of observing the full-disk Sun over ultrawide wavebands with images of high temporal, spatial and spectral resolutions and high dynamic range. The low frequency array, called MUSER-I, covers 400 MHz-2.0 GHz with 40 antennas of 4.5-m-diameter each and the high frequency array, called MUSER-II, covers 2–15 GHz with 60 antennas of 2-m-diameter each. The MUSER-I can obtain full-disk solar radio images in 64 frequency channels with a time cadence of 25 ms and a spatial resolution of 51.6″ to 10.3″ (corresponding to the frequency range 400 MHz to 2 GHz), whereas the MUSER-II can obtain full-disk solar images in 520 channels with a time cadence of 206.25 ms and a spatial resolution of 10.3″ to 1.3 (corresponding to the frequency range 2 to 15 GHz). A dynamic range of 25 dB can be obtained with snapshot images produced with the MUSER. An extension of MUSER in the further lower frequency range covering 30–400 MHz with an array of 224 logarithm-periodic dipole antennas (LPDAs) has been approved and will be completed during the next 4 years. The MUSER, as a dedicated solar instrument, has the following advantages providing simultaneous images over a wide frequency range with a unique high temporal-spatial-spectral resolutions; high-performing ultrawide-band dual-polarization feeds for wide-band signal collection; advanced high data-rate, large-scale digital correlation receiver for multiple-frequency and faster snapshot observations; and applications of new technologies such as using optical fiber to obtain remote antenna and wide-band analog signal transmission. The MUSER thus provides a unique opportunity to measure solar magnetic fields and trace dynamic evolution of energetic electrons in several radio frequencies, which, in turn, will help to have better understandings of the origin of various solar activities and the basic drivers of space weather.

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“…The coupling of a complex magnetic structure and plasma during a solar flare usually causes a quasi-periodic phenomenon, which is referred to as the quasi-periodic pulsation (QPP, see Nakariakov et al 2019a;Kupriyanova et al 2020, for recent reviews). It is a common oscillatory feature in the light curve of solar flare, which was first detected in X-ray and microwave emission (e.g., Parks & Winckler 1969) and later discovered in nearly all electromagnetic radiation, such as radio (Ning et al 2005;Karlický et al 2020), extreme-ultraviolet (EUV, Shen et al 2019;Yuan et al 2019), X-ray (Ning 2014;A&A proofs: manuscript no. 38398corr riods could depend on the mechanism producing them (e.g., Tan et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Preflare very long-periodic pulsations observed in Halpha emission before the onset of a solar flare

Li,

Feng,

et al. 2020

Preprint

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Context. Very long-periodic pulsations during preflare phases (preflare-VLPs) have been detected in the full-disk solar soft X-Ray (SXR) flux (see Tan et al. 2016). They may be regarded as precursors to solar flares and may help us better understand the trigger mechanism of solar flares. Aims. In this letter, we report a preflare-VLP event prior to the onset of an M1.1 circular-ribbon flare on 2015 October 16. It was simultaneously observed in Hα, SXR, and extreme ultraviolet (EUV) wavelengths. Methods. The SXR fluxes in 1−8 Å and 1−70 Å were recorded by the Geostationary Operational Environmental Satellite (GOES) and Extreme Ultraviolet Variability Experiment (EVE), respectively; the light curves in Hα and EUV 211 Å were integrated over a small local region, which were measured by the 1m New Vacuum Solar Telescope (NVST) and the Atmospheric Imaging Assembly (AIA), respectively. The preflare-VLP is identified as the repeat and quasi-periodic pulses in light curves during preflare phase. The quasi-periodicity can be determined from the Fourier power spectrum with Markov chain Monte Carlo (MCMC)-based Bayesian (e.g., Liang et al. 2020). Results. Seven well-developed pulses are found before the onset of an M1.1 circular-ribbon flare. They are firstly seen in the local light curve in Hα emission and then discovered in full-disk SXR fluxes in GOES 1−8 Å and ESP 1−70 Å, as well as the local light curve in AIA 211 Å. These well-developed pulses can be regarded as the preflare-VLP, which might be modulated by LRC-circuit oscillation in the current-carrying plasma loop. The quasi-period is estimated to be ∼9.3 minutes. Conclusions. We present the first report of a preflare-VLP event in the local Hα line and EUV wavelength, which could be considered a precursor of a solar flare. This finding should therefore prove useful for the prediction of solar flares, especially for powerful flares.

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Drifting Pulsation Structure at the Very Beginning of the 2017 September 10 Limb Flare

Cited by 19 publications

References 39 publications

Radio Observations of Coronal Mass Ejection Initiation and Development in the Low Solar Corona

Radio Observations of Coronal Mass Ejection Initiation and Development in the Low Solar Corona

Mingantu Spectral Radioheliograph for Solar and Space Weather Studies

Preflare very long-periodic pulsations observed in Halpha emission before the onset of a solar flare

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