Signatures of localised particle acceleration at a global coronal shock wave

Abstract

Extreme ultraviolet (EUV) waves are global waves in the solar corona which can accelerate particles. The efficiency of the acceleration depends on local plasma characteristics e.g. Alfvén speed and the geometry of the magnetic field. This shock-driven particle acceleration can produce radio signatures such as Type II radio bursts and herringbone emission. Here we investigate signatures of particle acceleration by a weak coronal shock on 10 March 2024. In particular, we combine EUV images with radio imaging and spectral observations to determine how and where this weak shock could accelerate energetic particles. A potential field source surface extrapolation was used to examine the pre-eruption ambient magnetic field while the evolution of the global wave was probed using running difference and base difference EUV images. The EUV images enabled the speed and Alfvén Mach number of the EUV wave to be characterised. The combination of radio images and dynamic spectra provide evidence of beams of shock-accelerated electrons localised to a dimming region at the time the EUV wave passes through it. The speeds and energies of these electrons were estimated from the drift rates of their herringbones. The EUV wave initially propagated West, channelled by loop systems, before changing direction northward. From the EUV intensity jump at the wavefront, the Alfvén Mach number was estimated to be approximately 1.005 at the time that the herringbones were produced. The herringbone drift rates revealed accelerated electron energies of 75-122 keV, using Newkirk density models with scaling factors of 1.3-2.6. These observations suggest that the weak lateral shock impacted quasi-perpendicular open field in a dimming region, enabling localised particle acceleration. This indicates that the geometry of the ambient magnetic field relative to the shock strongly governs where particles can be accelerated.

arXiv comment9 pages, 6 figures

References in corpus (21)

• Astropy: A Community Python Package for Astronomy
• The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package
• Binary companions of evolved stars in APOGEE DR14: Search method and catalog of ~5,000 companions
• A Review of Solar Type III Radio Bursts
• CALLISTO - A new concept for solar radio
• 'EUV Waves' are Waves: First Quadrature Observations of an EUV Wave from STEREO
• Large-scale Coronal Propagating Fronts in Solar Eruptions as Observed by the Atmospheric Imaging Assembly on Board the Solar Dynamics Observatory\,--\,An Ensemble Study
• Are "EIT Waves" Fast-Mode MHD Waves?
• What is the Nature of EUV Waves? First STEREO 3D Observations and Comparison with Theoretical Models
• Quasiperiodic acceleration of electrons by a plasmoid-driven shock in the solar atmosphere
• Understanding the Physical Nature of Coronal "EIT Waves"
• Multiple Regions of Shock-accelerated Particles during a Solar Coronal Mass Ejection
• Coronal response to an EUV wave from DEM analysis
• Investigation on the Coronal Magnetic Field Using a Type II Solar Radio Burst
• Evolution of the Alfvén Mach number associated with a coronal mass ejection shock
• An Investigation of the CME of 3 November 2011 and its Associated Widespread Solar Energetic Particle Event
• The Temperature-Dependent Nature of Coronal Dimmings
• Moreton and EUV Waves Associated with an X1.0 Flare and CME Ejection
• Localised acceleration of energetic particles by a weak shock in the solar corona
• Radio evidence for a shock wave reflected by a coronal hole
• Bursty acceleration and 3D trajectories of electrons in a solar flare