Escape of Flare-accelerated Particles in Solar Eruptive Events
arXiv:1909.13578 · doi:10.3847/1538-4357/ab4515
Abstract
Impulsive solar energetic particle events are widely believed to be due to the prompt escape into the interplanetary medium of flare-accelerated particles produced by solar eruptive events. According to the standard model for such events, however, particles accelerated by the flare reconnection should remain trapped in the flux rope comprising the coronal mass ejection. The particles should reach the Earth only much later, along with the bulk ejecta. To resolve this paradox, we have extended our previous axisymmetric model for the escape of flare-accelerated particles to fully three-dimensional (3D) geometries. We report the results of magnetohydrodynamic simulations of a coronal system that consists of a bipolar active region embedded in a background global dipole field structured by solar wind. Our simulations show that multiple magnetic reconnection episodes occur prior to and during the CME eruption and its interplanetary propagation. In addition to the episodes that build up the flux rope, reconnection between the open field and the CME couples the closed corona to the open interplanetary field. Flare-accelerated particles initially trapped in the CME thereby gain access to the open interplanetary field along a trail blazed by magnetic reconnection. A key difference between these 3D results and our previous calculations is that the interchange reconnection allows accelerated particles to escape from deep within the CME flux-rope. We estimate the spatial extent of the particle-escape channels. The relative timings between flare acceleration and release of the energetic particles through CME/open-field coupling are also determined. All our results compare favourably with observations.
References in corpus (36)
- A Model for Solar Coronal Mass Ejections
- Confined and ejective eruptions of kink-unstable flux ropes
- The Two Sources of Solar Energetic Particles
- A Model for the Sources of the Slow Solar Wind
- The standard flare model in three dimensions III. Slip-running reconnection properties
- Generalized Squashing Factors for Covariant Description of Magnetic Connectivity in the Solar Corona
- Hot Spine Loops and the Nature of a Late-Phase Solar Flare
- Sun-to-Earth MHD Simulation of the 14 July 2000 "Bastille Day" Eruption
- Fan-spine topology formation through two-step reconnection driven by twisted flux emergence
- Magnetic Topology of Coronal Hole Linkages
- Critical decay index at the onset of solar eruptions
- A Model for the Escape of Solar-Flare Accelerated Particles
- Numerical Investigation of a Coronal Mass Ejection from an Anemone Active Region: Reconnection and Deflection of the 2005 August 22 Eruption
- Current sheet formation and non-ideal behaviour at three-dimensional magnetic null points
- Evolution of Flare Ribbons, Electric Currents and Quasi-separatrix Layers During an X-class Flare
- The large longitudinal spread of solar energetic particles during the January 17, 2010 solar event
- The Solar Energetic Particle Event on 2013 April 11: An Investigation of its Solar Origin and Longitudinal Spread
- X-ray and UV investigation into the magnetic connectivity of a solar flare
- Magnetic-Island Contraction and Particle Acceleration in Simulated Eruptive Solar Flares
- Perpendicular Diffusion of Solar Energetic Particles: Model Results and Implications for Electrons
- Simulations of Emerging Magnetic Flux. II: The formation of Unstable Coronal Flux Ropes and the Initiation of CMEs
- Coronal magnetic reconnection driven by CME expansion -- the 2011 June 7 event
- A model for stealth coronal mass ejections
- Interchange Slip-Running Reconnection and Sweeping SEP Beams
- Two Episodes of Magnetic Reconnections During a Confined Circular-ribbon Flare
- Acceleration of Relativistic Protons during the 20 January 2005 Flare and CME
- Flux rope, hyperbolic flux tube, and late EUV phases in a non-eruptive circular-ribbon flare
- The Formation of Heliospheric Arcs of Slow Solar Wind
- Magnetohydrodynamic simulation of magnetic null-point reconnections in NOAA AR12192 initiated with an extrapolated non-force-free-field
- Why are flare ribbons associated with the spines of magnetic null points generically elongated?
- A Model for Energy Buildup and Eruption Onset in Coronal Mass Ejections
- Long-lasting injection of solar energetic electrons into the heliosphere
- Hard X-ray emitting energetic electrons and photospheric electric currents
- The relativistic solar particle event of 2005 January 20: origin of delayed particle acceleration
- Magnetic Structures at the Boundary of the Closed Corona: Interpretation of S-web Arcs
- Test particle acceleration in a numerical MHD experiment of an anemone jet
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- From Pseudostreamer Jets to CMEs: Observations of the Breakout Continuum
- Variability of the Reconnection Guide Field in Solar Flares
- A Model for the Coupled Eruption of a Pseudostreamer and Helmet Streamer
- Homologous Accelerated Electron Beams, Quasi-periodic fast-propagating Wave and CME Observed in one Fan-spine Jet
- Multiple injections of energetic electrons associated with the flare/CME event on 9 October 2021
- Linking the Sun to the Heliosphere Using Composition Data and Modelling. A Test Case with a Coronal Jet
- An Observational Study of a "Rosetta-Stone" Solar Eruption
- Improved modelling of SEP event onset within the WSA-Enlil-SEPMOD framework
- Eruption of EUV Hot-Channel near Solar Limb and Associated Moving Type-IV Radio Burst
- Synthetic Remote-sensing and In-situ Observations of Fine-scale Structure in a Pseudostreamer Coronal Mass Ejection through the Solar Corona
- Extended radio emission associated with a breakout eruption from the back side of the Sun
- What determine Solar Flares Producing Interplanetary Type III Radio Bursts?
- Estimating the total energy content in escaping accelerated solar electron beams
- Successive Coronal Mass Ejections Associated with Weak Solar Energetic Particle Events