A Type II Radio Burst Driven by a Blowout Jet on the Sun

Hou, Zhenyong; Su, Weiyi; Madjarska, M. S.; Chen, Hechao; Zheng, Ruisheng; Bai, Xianyong; Deng, Yuanyong

doi:10.3847/1538-4357/ace31b

Cited by 14 publications

(7 citation statements)

References 92 publications

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“…Alternatively, it is possible that the EUV jets themselves can drive the generation of shock waves, thereby accelerating the energetic electrons, which in turn can excite radio bursts. This is similar to the type II bursts associated with blowout jets reported by Hou et al (2023). Further research is needed to study the relationship between EUV jets and type III bursts in conjunction with radio imaging observations to better understand them.…”

Section: Conclusion and Discussionsupporting

confidence: 77%

Solar Type J Radio Bursts and the Associated Coronal Loop

Feng,

Xie,

Misawa

2024

ApJ

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The solar type J radio burst is a variant of type III bursts, which are a probe for understanding solar energetic electrons and local electron density. This study investigates a type J burst event on 2017 September 9. We have combined the data from the extreme-ultraviolet (EUV) imaging and the EUV Imaging Spectrometer (EIS) to analyze the event. Within 4 minutes several type J bursts with similar morphology occur. Two of them, with clear fundamental and second harmonic bands, are studied in detail. We find a delay of 2 ± 0.5 s between their different harmonic bands. During type J bursts, only one coronal loop brightens significantly at its northern footpoint, in correlation with the continuous injection of erupting jets into the loop. The EUV intensity of the brightening footpoint is correlated with the radio flux at 245 and 410 MHz, with correlation coefficients of 0.2 and 0.4, respectively. These observations suggest that the type J bursts should originate from this coronal loop. By analyzing the electron number density distribution along the coronal loop diagnosed from the EIS data and the time evolution of the plasma frequency calculated from the type J burst, we determine that the velocities of the energetic electrons exciting the two type Js are 0.10 ± 0.02c and 0.12 ± 0.02c. Our results confirm previous studies on type J bursts.

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Section: Conclusion and Discussionsupporting

confidence: 77%

Solar Type J Radio Bursts and the Associated Coronal Loop

Feng,

Xie,

Misawa

2024

ApJ

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“…Since our purpose is to obtain global distributions of coronal plasma parameters within a relatively short period of time and since fine structures are not our priority, we decided to adopt a moderate resolution of ∼8″ (pixel size ∼4″ in both Solar X and Y directions, slit width ∼4″). With this resolution typical coronal structures, such as EUV bright points, coronal plumes, and AR loops, can be relatively well sampled, which has been demonstrated by recent observations (e.g., Hou et al 2022;Bai et al 2023;Hou et al 2023) from EUV imagers with a similar resolution, e.g., the Solar X-ray Extreme Ultraviolet Imager (Song et al 2022) onboard the Fengyun-3E satellite and the Solar Upper Transition Region Imager (Bai et al 2023) onboard the Space Advanced Technology demonstration satellite. In addition, our pixel size (4″ × 4″) is comparable to that of COSIE, which is 9 3 × 3 1.…”

Section: Description Of the Proposed Instrumentmentioning

confidence: 78%

Global Coronal Plasma Diagnostics Based on Multislit Extreme-ultraviolet Spectroscopy

Chan 陳,

Tian,

Liu

et al. 2024

ApJ

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Full-disk spectroscopic observations of the solar corona are highly desired to forecast solar eruptions and their impact on planets and to uncover the origin of solar wind. In this paper, we introduce a new multislit design (five slits) to obtain extreme-ultraviolet (EUV) spectra simultaneously. The selected spectrometer wavelength range (184–197 Å) contains several bright EUV lines that can be used for spectral diagnostics. The multislit approach offers an unprecedented way to efficiently obtain the global spectral data but the ambiguity from different slits should be resolved. Using a numerical simulation of the global corona, we primarily concentrate on the optimization of the disambiguation process, with the objective of extracting decomposed spectral information of six primary lines. This subsequently facilitates a comprehensive series of plasma diagnostics, including density (Fe xii 195.12/186.89 Å), Doppler velocity (Fe xii 193.51 Å), line width (Fe xii 193.51 Å), and temperature diagnostics (Fe viii 185.21 Å, Fe x 184.54 Å, Fe xi 188.22 Å, and Fe xii 193.51 Å). We find a good agreement between the forward modeling parameters and the inverted results at the initial eruption stage of a coronal mass ejection, indicating the robustness of the decomposition method and its immense potential for global monitoring of the solar corona.

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“…We have stored a large amount of observation data of CBSm, and some of the data have been used for scientific research by many institutions and individuals. For example, Hou et al (2023) used solar radio observation data obtained by the system from 02:18 UT to 02:33 UT on 2022 November 12 to investigate coronal jet-driven type II radio bursts. For more observation data, please visit our online data website at http:// 47.104.87.104/MWRS/.…”

Section: Examples Of Solar Radio Burst Eventsmentioning

confidence: 99%

Development of a 90–600 MHz Meter-wave Solar Radio Spectrometer

Chang 常,

Wang 王,

Lu 路

et al. 2024

ApJS

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Radio observation is important for understanding coronal mass ejections (CMEs), coronal shock waves, and high-energy electron acceleration. Here, we developed a new Chashan broadband solar radio spectrometer at a meter wavelength for observing the (super)fine structure of the solar radio burst spectrum. In the signal-receiving unit, we adopt an antenna system consisting of a 12 m large-aperture parabolic reflector and dual-line polarized logarithmic periodic feed source, as well as a high-precision Sun-tracking turntable system, all of which ensure the high-precision acquisition of solar radiation signals. For the digital receiver, we use a high-speed analog-to-digital converter with a sampling rate of 1.25 GSPS to directly sample the signal amplified and filtered by the analog receiver, simplifying the structure of the analog receiver, and design a 16k-point fast Fourier transform algorithm in the field programmable gate array to perform time–frequency transformation on the sampled signals. The default frequency and temporal resolution of the system are 76.294 kHz and 0.839 ms (up to 0.21 ms), respectively. The noise coefficient of the system is less than 1 dB, the dynamic range is more than 60 dB, and the sensitivity is as high as 1 sfu. We have observed a large number of radio bursts, including type I radio storms, hundreds of type III, ∼20 type II, and ∼15 type IV bursts in the past year. These high-quality data are useful in the further study of CMEs and associated particle acceleration and the origins of solar radio bursts.

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A Type II Radio Burst Driven by a Blowout Jet on the Sun

Cited by 14 publications

References 92 publications

Solar Type J Radio Bursts and the Associated Coronal Loop

Solar Type J Radio Bursts and the Associated Coronal Loop

Global Coronal Plasma Diagnostics Based on Multislit Extreme-ultraviolet Spectroscopy

Development of a 90–600 MHz Meter-wave Solar Radio Spectrometer

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