LOFAR Observations of a Jet-driven Piston Shock in the Low Solar Corona

Maguire, Ciara A.; Carley, Eoin; Zucca, Pietro; Vilmer, Nicole; Gallagher, Peter T.

doi:10.3847/1538-4357/abda51

Cited by 18 publications

(16 citation statements)

References 51 publications

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“…A similar conclusion for five events observed in the 164−435 MHz range was reached by Maia et al (2000). The coronal shock radio sources may occur in front of an erupting flux rope (Bain et al 2012;Zimovets et al 2012;, above expanding soft X-ray loops (e.g., Klein et al 1999;Dauphin et al 2006), in association with an erupting jet during the progression of a CME (e.g., Zucca et al 2014a;Maguire et al 2021), in front of an EUV bubble in both radial and lateral directions (Kouloumvakos et al 2014) or ahead of a CME that was deflected in the low corona (Pick et al 2016).…”

Section: Introductionsupporting

confidence: 61%

Multiwavelength observations of a metric type-II event

Alissandrakis

Nindos

Patsourakos

et al. 2021

A&A

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We have studied a complex metric radio event that originated in a compact flare, observed with the ARTEMIS-JLS radiospectrograph on February 12, 2010. The event was associated with a surge observed at 195 and 304 Å and with a coronal mass ejection observed by instruments on board STEREO A and B near the eastern and western limbs respectively. On the disk the event was observed at ten frequencies by the Nançay Radioheliograph (NRH), in Hα by the Catania observatory, in soft X-rays by GOES SXI and Hinode XRT, and in hard X-rays by RHESSI. We combined these data, together with MDI longitudinal magnetograms, to get as complete a picture of the event as possible. Our emphasis is on two type-II bursts that occurred near respective maxima in the GOES light curves. The first, associated with the main peak of the event, showed an impressive fundamental-harmonic structure, while the emission of the second consisted of three well-separated bands with superposed pulsations. Using positional information for the type-IIs from the NRH and triangulation from STEREO A and B, we found that the type-IIs were associated neither with the surge nor with the disruption of a nearby streamer, but rather with an extreme ultraviolet (EUV) wave probably initiated by the surge. The fundamental-harmonic structure of the first type-II showed a band split corresponding to a magnetic field strength of 18 G, a frequency ratio of 1.95 and a delay of 0.23−0.65 s of the fundamental with respect to the harmonic; moreover it became stationary shortly after its start and then drifted again. The pulsations superposed on the second type-II were broadband and had started before the burst. In addition, we detected another pulsating source, also before the second type-II, polarized in the opposite sense; the pulsations in the two sources were out of phase and hence hardly detectable in the dynamic spectrum. The pulsations had a measurable reverse frequency drift of about 2 s−1.

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Section: Introductionsupporting

confidence: 61%

Multiwavelength observations of a metric type-II event

Alissandrakis

Nindos

Patsourakos

et al. 2021

A&A

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“…Note that in the case of type II bursts, reports indicate that the centroids of F-and H-components at any given observing frequency are nearly cospatial (Zucca et al 2018). So we can consider the corresponding emission to be generated in the same location, although there could be an apparent shift in the observed position of particularly the F-component due to propagation effects (Maguire et al 2021). Moving further, depolarization as the cause of low dcp in the case of F-component O mode applies mostly to type I bursts only (see, e.g., Melrose 2017).…”

Section: Analysis and Resultsmentioning

confidence: 99%

Circular Polarization Observations of Type II Solar Radio Bursts and the Coronal Magnetic Field

Ramesh

Kathiravan

Chellasamy

2022

ApJ

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It is well known that magnetic field strength (B) in the solar corona can be calculated using the Alfvén Mach number (M A ) and Alfvén speed (v A ) of the magnetohydrodynamic shock waves associated with coronal type II radio bursts. We show that observations of weak circularly polarized emission associated with the harmonic component of the type II bursts provide independent and consistent estimates of B. For the coronal type II burst observed on 2021 October 9, we obtained B ≈1.5 G and ≈1.9 G at a heliocentric distance (r) of ≈1.8 R ⊙, using the above two techniques, respectively.

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“…Recently, Shen et al (2018a) firstly reported that single-pulsed EUV waves can be directly launched by coronal jets in coronal loops. Such an excitation mechanism is similar to the generation of piston shocks in a one-dimensional tube, in which the jet acted as the driver of the wave train that can propagate faster than its driver (Warmuth 2015;Ying et al 2018;Maguire et al 2021). According to the piston shock scenario, our present QFP wave train could be driven by the jet ejection, in which two QFP wave fronts might related to unresolved discrete fine structures consisting of the jet body.…”

Section: Discussionmentioning

confidence: 83%

Homologous Accelerated Electron Beams, Quasi-periodic fast-propagating Wave and CME Observed in one Fan-spine Jet

Duan,

Shen,

Zhou

et al. 2022

Preprint

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Using imaging and radio multi-wavelength observations, we studied the origin of two homologous accelerated electron beams and a quasi-periodic fast-propagating (QFP) wave train associated with a solar jet on 2012 July 14. The jet occurred in a small-scale fan-spine magnetic system embedding in a large-scale pseudostreamer, which associated with a GOES C1.4 flare, a jet-like coronal mass ejection (CME), a type II radio burst, and a type III radio burst. During the initial stage, a QFP wave train and a fast moving on-disk radio source were detected in succession ahead of the jet along the outer spine of the fan-spine system. When the jet reached a height of about 1.3 solar radii, it underwent a bifurcation into two branches. Based on our analysis results, all the observed phenomena in association with the jet can be explained by using a fanspine magnetic system. We propose that both the type III radio burst and the on-disk fast moving radio source were caused by the same physical process, i.e., the energetic electrons accelerated by the magnetic reconnection at the null point, and they were along the open field lines of the pseudostreamer and the closed outer spine of the fanspine structure, respectively. Due to the bifurcation of the jet body, the lower branch along the closed outer spine of the fan-spine structure fell back to the solar surface, while the upper branch along the open field lines of the pseudostreamer caused the jet-like CME in the outer corona.

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LOFAR Observations of a Jet-driven Piston Shock in the Low Solar Corona

Cited by 18 publications

References 51 publications

Multiwavelength observations of a metric type-II event

Multiwavelength observations of a metric type-II event

Circular Polarization Observations of Type II Solar Radio Bursts and the Coronal Magnetic Field

Homologous Accelerated Electron Beams, Quasi-periodic fast-propagating Wave and CME Observed in one Fan-spine Jet

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