Plasma Instability Evolution and Particle Heating in the Foot Region of Perpendicular Shocks in Young Supernova Remnants

Law, K. F.F.; Fujioka, S.; Ohira, Y.

Astrophysical Journal, 2025, 982(2), 101

Number of Access:264（2025-08-14 07:29 Counts）

Identifier to cite or link to this item: https://hdl.handle.net/11094/101107

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Title
Plasma Instability Evolution and Particle Heating in the Foot Region of Perpendicular Shocks in Young Supernova Remnants
Creator
ORCID
0000-0002-5484-8870 0000-0002-5484-8870
researchmap permalink
kingfaifarley_law kingfaifarley_law
CreatorName
Law, K. F.F.
NRID
1000040372635 1000040372635
ORCID
0000-0001-8406-1772 0000-0001-8406-1772
researchmap permalink
shinsuke_fujioka shinsuke_fujioka
Scopus Author ID
24474814400 24474814400
CreatorName
Fujioka, S.
CreatorName
Ohira, Y.
Description
Law K.F.F., Fujioka S., Ohira Y.. Plasma Instability Evolution and Particle Heating in the Foot Region of Perpendicular Shocks in Young Supernova Remnants. Astrophysical Journal 982, 101 (2025); https://doi.org/10.3847/1538-4357/adb629.
Abstract
Particle acceleration from collisionless shocks is a key mechanism in the generation of cosmic rays. In particular, shocks in young supernova remnants (SNRs) are considered to be a major source of galactic cosmic rays. This study investigates the early-stage plasma instability evolution and subsequent electron and ion heating in the foot region of high-Mach-number perpendicular shocks in young SNRs, using 2D particle-in-cell simulations. Unlike previous simulations that cover larger regions of the shock structure—including the downstream, shock, and upstream regions—our simulations are local, limited to the shock transition region, and focus on practical parameters with a nonrelativistic shock velocity (v ≈ 0.02c) and the standard mass ratio between protons and electrons. We examined scenarios with and without the presence of return protons, and our results reveal that the Buneman instability, followed by the ion two-stream instability, dominates the early electron-heating process. We observed long-lasting ion heating in the case without return protons and note that the Weibel instability did not emerge within the simulation time frame. These findings enhance the understanding of plasma behavior in young SNR shocks and suggest that local simulations with practical parameters are crucial for exploring electron-heating mechanisms, while also highlighting the conditions under which the Weibel instability may or may not emerge.
Publisher
Institute of Physics
Source Title
Astrophysical Journal
Volume (Issue)
982(2)
Page
101
Date of Issued
2025-04-01
Language
English
Handle URL
https://hdl.handle.net/11094/101107
PISSN
0004637X
eISSN
15384357
Relation.isIdenticalTo
DOI (Publisher Version)
https://doi.org/10.3847/1538-4357/adb629
Access Rights
open access
CopyRight
This article is licensed under a Creative Commons Attribution 4.0 International License.
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Version of Record
Category
学術雑誌論文 Journal Article