BibTex format
@article{Schwadron:2024:1538-4357/ad527f,
author = {Schwadron, NA and Bale, SD and Bonnell, J and Case, A and Shen, M and Christian, ER and Cohen, CMS and Davis, AJ and Desai, MI and Goetz, K and Giacalone, J and Hill, ME and Kasper, JC and Korreck, K and Larson, D and Livi, R and Lim, T and Leske, RA and Malandraki, O and Malaspina, D and Matthaeus, WH and McComas, DJ and McNutt, RL and Mewaldt, RA and Mitchell, DG and Niehof, JT and Pulupa, M and Pecora, F and Rankin, JS and Smith, C and Stone, EC and Szalay, JR and Vourlidas, A and Wiedenbeck, ME and Whittlesey, P},
doi = {1538-4357/ad527f},
journal = {Astrophysical Journal},
title = {Parker Solar Probe Observations of Energetic Particles in the Flank of a Coronal Mass Ejection Close to the Sun},
url = {http://dx.doi.org/10.3847/1538-4357/ad527f},
volume = {970},
year = {2024}
}
RIS format (EndNote, RefMan)
TY - JOUR
AB - We present an event observed by Parker Solar Probe (PSP) at ∼0.2 au on 2022 March 2 in which imaging and in situ measurements coincide. During this event, PSP passed through structures on the flank of a streamer blowout coronal mass ejection (CME) including an isolated flux tube in front of the CME, a turbulent sheath, and the CME itself. Imaging observations and in situ helicity and principal variance signatures consistently show the presence of flux ropes internal to the CME. In both the sheath and the CME interval, the distributions are more isotropic, the spectra are softer, and the abundance ratios of Fe/O and He/H are lower than those in the isolated flux tube, and yet elevated relative to typical plasma and solar energetic particle abundances. These signatures in the sheath and the CME indicate that both flare populations and those from the plasma are accelerated to form the observed energetic particle enhancements. In contrast, the isolated flux tube shows large streaming, hard spectra, and large Fe/O and He/H ratios, indicating flare sources. Energetic particle fluxes are most enhanced within the CME interval from suprathermal through energetic particle energies (∼keV to >10 MeV), indicating particle acceleration, as well as confinement local to the closed magnetic structure. The flux-rope morphology of the CME helps to enable local modulation and trapping of energetic particles, in particular along helicity channels and other plasma boundaries. Thus, the CME acts to build up energetic particle populations, allowing them to be fed into subsequent higher-energy particle acceleration throughout the inner heliosphere where a compression or shock forms on the CME front.
AU - Schwadron,NA
AU - Bale,SD
AU - Bonnell,J
AU - Case,A
AU - Shen,M
AU - Christian,ER
AU - Cohen,CMS
AU - Davis,AJ
AU - Desai,MI
AU - Goetz,K
AU - Giacalone,J
AU - Hill,ME
AU - Kasper,JC
AU - Korreck,K
AU - Larson,D
AU - Livi,R
AU - Lim,T
AU - Leske,RA
AU - Malandraki,O
AU - Malaspina,D
AU - Matthaeus,WH
AU - McComas,DJ
AU - McNutt,RL
AU - Mewaldt,RA
AU - Mitchell,DG
AU - Niehof,JT
AU - Pulupa,M
AU - Pecora,F
AU - Rankin,JS
AU - Smith,C
AU - Stone,EC
AU - Szalay,JR
AU - Vourlidas,A
AU - Wiedenbeck,ME
AU - Whittlesey,P
DO - 1538-4357/ad527f
PY - 2024///
SN - 0004-637X
TI - Parker Solar Probe Observations of Energetic Particles in the Flank of a Coronal Mass Ejection Close to the Sun
T2 - Astrophysical Journal
UR - http://dx.doi.org/10.3847/1538-4357/ad527f
VL - 970
ER -