Spatially Resolved Moving Radio Burst Associated with an EUV Wave

Lu, Lei; Feng, Li; Gan, Weiqun

doi:10.3847/2041-8213/ac6ced

Cited by 4 publications

(4 citation statements)

References 45 publications

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“…Based on their findings, they proposed that the band-splitting signals are moderately polarized with left-handed polarized emission stronger than the right-hand one. It is commonly believed that coronal shocks result from the coronal mass ejection (CME) propagation or expansion (e.g., Cliver et al 2004;Vršnak & Cliver 2008;Liu et al 2009;Chen 2011;Li et al 2012;Shen & Liu 2012;Cho et al 2013;Feng et al 2013;Chen et al 2014;Ying et al 2018;Ma & Chen 2020;Lu et al 2022;Zhang et al 2022b).…”

Section: Introductionmentioning

confidence: 99%

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

Hou

Madjarska

et al. 2023

ApJ

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Type II radio bursts are often associated with coronal shocks that are typically driven by coronal mass ejections (CMEs) from the Sun. Here we conduct a case study of a type II radio burst that is associated with a C4.5-class flare and a blowout jet, but without the presence of a CME. The blowout jet is observed near the solar disk center in the extreme-ultraviolet (EUV) passbands with different characteristic temperatures. Its evolution involves an initial phase and an ejection phase with a velocity of 560 ± 87 km s−1. Ahead of the jet front, an EUV wave propagates at a projected velocity of ∼403 ± 84 km s−1 in the initial stage. The velocity of the type II radio burst is estimated to be ∼641 km s−1, which corresponds to the shock velocity against the coronal density gradient. The EUV wave and the type II radio burst are closely related to the ejection of the blowout jet, suggesting that both are likely the manifestation of a coronal shock driven by the ejection of the blowout jet. The type II radio burst likely starts lower than those associated with CMEs. The combination of the velocities of the radio burst and the EUV wave yields a modified shock velocity at ∼757 km s−1. The Alfvén Mach number is in the range of 1.09–1.18, implying that the shock velocity is 10%–20% larger than the local Alfvén velocity.

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Section: Introductionmentioning

confidence: 99%

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

Hou

Madjarska

et al. 2023

ApJ

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“…The speeds of EUV waves range from a few hundreds to ≥2000 km s −1 (Shen & Liu 2012;Liu et al 2018). Furthermore, fast CMEs are capable of driving shock waves propagating in the corona and interplanetary space, which are related to type II radio bursts (e.g., Chen et al 2002;Rouillard et al 2012;Zucca et al 2018;Morosan et al 2019;Downs et al 2021;Lu et al 2022;Ying et al 2022).…”

Section: Introductionmentioning

confidence: 99%

First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops

Zhang

et al. 2022

ApJL

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In this Letter, we perform a detailed analysis of the M5.5 class eruptive flare occurring in active region 12,929 on 2022 January 20. The eruption of a hot channel generates a fast coronal mass ejection (CME) and a dome-shaped extreme-ultraviolet (EUV) wave at speeds of 740–860 km s−1. The CME is associated with a type II radio burst, implying that the EUV wave is a fast-mode shock wave. During the impulsive phase, the flare shows quasi-periodic pulsations (QPPs) in EUV, hard X-ray, and radio wavelengths. The periods of QPPs range from 18 to 113 s, indicating that flare energy is released and nonthermal electrons are accelerated intermittently with multiple timescales. The interaction between the EUV wave and low-lying adjacent coronal loops (ACLs) results in contraction, expansion, and transverse vertical oscillation of ACLs. The speed of contraction in 171, 193, and 211 Å is higher than that in 304 Å. The periods of oscillation are 253 s and 275 s in 304 Å and 171 Å, respectively. A new scenario is proposed to explain the interaction. The equation that interprets the contraction and oscillation of the overlying coronal loops above a flare core can also interpret the expansion and oscillation of ACLs, suggesting that the two phenomena are the same in essence.

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“…In the lower solar atmosphere at optical and UV/EUV wavelengths, the Lyα emission was dominant in the measured radiative losses (Milligan et al 2014), but it was still a minor part of the total radiated flare energy (Kretzschmar et al 2013). Solar flares are often accompanied by radio bursts, such as Type II, III or IV bursts, and microwave bursts (e.g., Mahender et al 2020;Lu et al 2022;Su et al 2022;Yan et al 2023). However, the flare energy in radio emissions is much smaller than that radiated in wavebands of X-rays, UV/EUV and WL, mainly because the radio wave is the longest wavelength in the electromagnetic spectrum, i.e., including microwave, decimeter-wave and even metric-wave (see Pasachoff 1978).…”

Section: Introductionmentioning

confidence: 99%

Global Energetics of Solar Powerful Events on 2017 September 6

Warmuth

Wang

et al. 2023

Res. Astron. Astrophys.

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Solar flares and coronal mass ejections (CMEs) are thought to be the most pow-erful events on the Sun. They can release energy as high as ∼10^32erg in tens of minutes,and could produce solar energetic particles (SEPs) in the interplanetary space. We exploreglobal energy budgets of solar major eruptions on 6 September 2017, including the en-ergy partition of a powerful solar flare, the energy budget of the accompanied CME andSEPs. In the wavelength range shortward of ∼222 nm, a major contribution of the flareradiated energy is in the soft X-ray (SXR) 0.1−7 nm domain. The flare energy radiatedat wavelengths of Lyα and middle ultraviolet is larger than that radiated in the extremeultraviolet wavelength, but it is much less than that radiated in the SXR waveband. Thetotal flare radiated energy could be comparable to the thermal and nonthermal energies.The energies carried by the major flare and its accompanied CME are roughly equal, andthey are both powered by the magnetic free energy in the AR NOAA 12673. Moreover,the CME is efficient in accelerating SEPs, and that the prompt component (whether itcomes from the solar flare or the CME) contributes only a negligible fraction.

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Spatially Resolved Moving Radio Burst Associated with an EUV Wave

Cited by 4 publications

References 45 publications

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

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

First Detection of Transverse Vertical Oscillation during the Expansion of Coronal Loops

Global Energetics of Solar Powerful Events on 2017 September 6

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