FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W4378977160> ?p ?o ?g. }

• W4378977160 endingPage "A98" @default.
• W4378977160 startingPage "A98" @default.
• W4378977160 abstract "Context. The Sun produces the most powerful explosions in the Solar System, solar flares, which can also be accompanied by large eruptions of magnetised plasma, coronal mass ejections (CMEs). These processes can accelerate electron beams up to relativistic energies through magnetic reconnection processes during solar flares and CME-driven shocks. Energetic electron beams can in turn generate radio bursts through the plasma emission mechanism. CME shocks, in particular, are usually associated with type II solar radio bursts. Aims. However, on a few occasions, type II bursts have been reported to occur either in the absence of CMEs or shown to be more likely related with the flaring process. It is currently an open question as to how a shock generating type II bursts forms without the occurrence of a CME eruption. Here, we aim to determine the physical mechanism responsible for a type II burst that occurs in the absence of a CME. Methods. By using radio imaging from the Nançay Radioheliograph, combined with observations from the Solar Dynamics Observatory and the Solar Terrestrial Relations Observatory spacecraft, we investigate the origin of a type II radio burst that appears to have no temporal association with a white-light CME. Results. We identify a typical type II radio burst with band-split structure that is associated with a C-class solar flare. The type II burst source is located above the flaring active region and ahead of disturbed coronal loops observed in extreme-ultraviolet (EUV) images. The type II burst is also preceded by type III radio bursts, some of which are in fact J bursts, indicating that accelerated electron beams do not all escape along open field lines. The type II sources show single-frequency movement towards the flaring active region. The type II burst is located ahead of a faint EUV front propagating through the corona. Conclusions. Since there is no CME detection, a shock wave is most likely generated by the flaring process or the bulk plasma motions associated with a failed eruption. The EUV front observed is likely a freely propagating wave that expands into surrounding regions. The EUV front propagates at an initial speed of approximately 450 km s −1 and it is likely to steepen into a shock wave in a region of low Alfvén speed as determined from magneto-hydrodynamic modelling of the corona." @default.
• W4378977160 created "2023-06-02" @default.
• W4378977160 creator A5001466488 @default.
• W4378977160 creator A5020163516 @default.
• W4378977160 creator A5028659349 @default.
• W4378977160 creator A5081622185 @default.
• W4378977160 creator A5092063843 @default.
• W4378977160 date "2023-07-01" @default.
• W4378977160 modified "2023-09-25" @default.
• W4378977160 title "A type II solar radio burst without a coronal mass ejection" @default.
• W4378977160 cites W1503370816 @default.
• W4378977160 cites W1964454386 @default.
• W4378977160 cites W1971994758 @default.
• W4378977160 cites W1978015487 @default.
• W4378977160 cites W1993893656 @default.
• W4378977160 cites W2001135664 @default.
• W4378977160 cites W2005621102 @default.
• W4378977160 cites W2016024818 @default.
• W4378977160 cites W2018405851 @default.
• W4378977160 cites W2025870303 @default.
• W4378977160 cites W2033183532 @default.
• W4378977160 cites W2048335231 @default.
• W4378977160 cites W2053092803 @default.
• W4378977160 cites W2057594951 @default.
• W4378977160 cites W2058113402 @default.
• W4378977160 cites W2064317263 @default.
• W4378977160 cites W2082443845 @default.
• W4378977160 cites W2094483427 @default.
• W4378977160 cites W2098788010 @default.
• W4378977160 cites W210529956 @default.
• W4378977160 cites W2111078819 @default.
• W4378977160 cites W2136295218 @default.
• W4378977160 cites W2140555829 @default.
• W4378977160 cites W2142234851 @default.
• W4378977160 cites W2157220458 @default.
• W4378977160 cites W2160257574 @default.
• W4378977160 cites W2162702920 @default.
• W4378977160 cites W2163210011 @default.
• W4378977160 cites W2242891466 @default.
• W4378977160 cites W2312283570 @default.
• W4378977160 cites W2481913473 @default.
• W4378977160 cites W2488422185 @default.
• W4378977160 cites W27182397 @default.
• W4378977160 cites W2736161771 @default.
• W4378977160 cites W2795402328 @default.
• W4378977160 cites W2884139102 @default.
• W4378977160 cites W2950044430 @default.
• W4378977160 cites W2968587435 @default.
• W4378977160 cites W3031243967 @default.
• W4378977160 cites W3039256424 @default.
• W4378977160 cites W3098393230 @default.
• W4378977160 cites W3102038923 @default.
• W4378977160 cites W3102601759 @default.
• W4378977160 cites W3103972835 @default.
• W4378977160 cites W3104419059 @default.
• W4378977160 cites W3105735183 @default.
• W4378977160 cites W3123091284 @default.
• W4378977160 cites W3134173243 @default.
• W4378977160 cites W3139123450 @default.
• W4378977160 cites W3206722155 @default.
• W4378977160 cites W3208652740 @default.
• W4378977160 cites W4238135743 @default.
• W4378977160 cites W4247625980 @default.
• W4378977160 cites W4308886936 @default.
• W4378977160 cites W4316038213 @default.
• W4378977160 cites W4379650375 @default.
• W4378977160 cites W6047081 @default.
• W4378977160 doi "https://doi.org/10.1051/0004-6361/202245515" @default.
• W4378977160 hasPublicationYear "2023" @default.
• W4378977160 type Work @default.
• W4378977160 citedByCount "1" @default.
• W4378977160 countsByYear W43789771602023 @default.
• W4378977160 crossrefType "journal-article" @default.
• W4378977160 hasAuthorship W4378977160A5001466488 @default.
• W4378977160 hasAuthorship W4378977160A5020163516 @default.
• W4378977160 hasAuthorship W4378977160A5028659349 @default.
• W4378977160 hasAuthorship W4378977160A5081622185 @default.
• W4378977160 hasAuthorship W4378977160A5092063843 @default.
• W4378977160 hasBestOaLocation W43789771601 @default.
• W4378977160 hasConcept C108411613 @default.
• W4378977160 hasConcept C121332964 @default.
• W4378977160 hasConcept C1276947 @default.
• W4378977160 hasConcept C151730666 @default.
• W4378977160 hasConcept C172600038 @default.
• W4378977160 hasConcept C185001636 @default.
• W4378977160 hasConcept C2779343474 @default.
• W4378977160 hasConcept C2779588948 @default.
• W4378977160 hasConcept C2992142144 @default.
• W4378977160 hasConcept C44870925 @default.
• W4378977160 hasConcept C62520636 @default.
• W4378977160 hasConcept C72886185 @default.
• W4378977160 hasConcept C82706917 @default.
• W4378977160 hasConcept C86803240 @default.
• W4378977160 hasConceptScore W4378977160C108411613 @default.
• W4378977160 hasConceptScore W4378977160C121332964 @default.
• W4378977160 hasConceptScore W4378977160C1276947 @default.
• W4378977160 hasConceptScore W4378977160C151730666 @default.
• W4378977160 hasConceptScore W4378977160C172600038 @default.

• next