Open AccessSpatially Separated Electron and Proton Beams in a Simulated Solar Coronal Jet
Author(s) -
Ross Pallister,
P. F. Wyper,
D. I. Pontin,
C. R. DeVore,
Federica Chiti
Publication year - 2021
Publication title -
astrophysical journal/the astrophysical journal
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.376
H-Index - 489
eISSN - 1538-4357
pISSN - 0004-637X
DOI - 10.3847/1538-4357/ac2e6d
Subject(s) - physics , heliosphere , electron , coronal mass ejection , jet (fluid) , astrophysics , particle acceleration , solar flare , photosphere , magnetic reconnection , nanoflares , corona (planetary geology) , computational physics , current sheet , magnetohydrodynamics , solar wind , astronomy , plasma , nuclear physics , mechanics , astrobiology , spectral line , venus
Magnetic reconnection is widely accepted to be a major contributor to nonthermal particle acceleration in the solar atmosphere. In this paper we investigate particle acceleration during the impulsive phase of a coronal jet, which involves bursty reconnection at a magnetic null point. A test-particle approach is employed, using electromagnetic fields from a magnetohydrodynamic simulation of such a jet. Protons and electrons are found to be accelerated nonthermally both downwards toward the domain’s lower boundary and the solar photosphere, and outwards along the axis of the coronal jet and into the heliosphere. A key finding is that a circular ribbon of particle deposition on the photosphere is predicted, with the protons and electrons concentrated in different parts of the ribbon. Furthermore, the outgoing protons and electrons form two spatially separated beams parallel to the axis of the jet, signatures that may be observable in in-situ observations of the heliosphere.