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Peer-reviewedCC BY 4.0The Astrophysical Journal

SN 1006: A Cosmic Laboratory for Investigating Shock Acceleration Physics

  • Emma McGinness1
  • Rebecca Diesing2,3
  • Damiano Caprioli1
  • Fabio Acero4,5
5 affiliations
  1. 1The University of Chicago
  2. 2Institute for Advanced Study
  3. 3Columbia University
  4. 4Université Paris-Saclay
  5. 5FSLAC IRL 2009
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Abstract

SN 1006 is a historical Type Ia supernova remnant that exhibits nonthermal emission ranging from radio to multi-TeV γ -rays. Most of this emission (particularly X-rays and γ -rays) is concentrated in polar caps aligned with the ambient magnetic field, which makes it an ideal laboratory for studying cosmic ray (CR) acceleration at different shock obliquities and the hadronic/leptonic nature of the γ -ray emission. We model SN 1006’s morphology, multiwavelength spectrum, and radial profile using a self-consistent multizone kinetic model of particle acceleration that accounts for CR-driven shock modification, magnetic field amplification, drift in magnetic fluctuations, and temporal dynamics including adiabatic and synchrotron losses. Our model can reproduce both the observed spectral and spatial properties, with the exception of the radio profile, which we argue requires 3D hydrodynamic effects to replicate. We find that quasi-parallel regions (where the shock normal aligns with the ambient magnetic field) exhibit very prominent CR acceleration (20% efficiency), while quasi-perpendicular regions exhibit efficiencies below 1%, consistent with the results of kinetic simulations. We also find that electrons are responsible for the majority of the γ -ray emission from SN 1006 (i.e., it is a leptonic source), with the exception of the northwest region due to an encounter with a dense cloud.

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Cite

BibTeXRIS
BibTeX
@article{mcginness20261006,
  title = {{SN 1006: A Cosmic Laboratory for Investigating Shock Acceleration Physics}},
  author = {Emma McGinness and Rebecca Diesing and Damiano Caprioli and Fabio Acero},
  journal = {The Astrophysical Journal},
  year = {2026},
  month = oct,
  doi = {10.3847/1538-4357/aea3f3},
  url = {https://iopscience.iop.org/article/10.3847/1538-4357/aea3f3},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - SN 1006: A Cosmic Laboratory for Investigating Shock Acceleration Physics
AU  - Emma McGinness
AU  - Rebecca Diesing
AU  - Damiano Caprioli
AU  - Fabio Acero
PY  - 2026
DA  - 2026/10/09
JO  - The Astrophysical Journal
DO  - 10.3847/1538-4357/aea3f3
UR  - https://iopscience.iop.org/article/10.3847/1538-4357/aea3f3
AB  - SN 1006 is a historical Type Ia supernova remnant that exhibits nonthermal emission ranging from radio to multi-TeV γ -rays. Most of this emission (particularly X-rays and γ -rays) is concentrated in polar caps aligned with the ambient magnetic field, which makes it an ideal laboratory for studying cosmic ray (CR) acceleration at different shock obliquities and the hadronic/leptonic nature of the γ -ray emission. We model SN 1006’s morphology, multiwavelength spectrum, and radial profile using a self-consistent multizone kinetic model of particle acceleration that accounts for CR-driven shock modification, magnetic field amplification, drift in magnetic fluctuations, and temporal dynamics including adiabatic and synchrotron losses. Our model can reproduce both the observed spectral and spatial properties, with the exception of the radio profile, which we argue requires 3D hydrodynamic effects to replicate. We find that quasi-parallel regions (where the shock normal aligns with the ambient magnetic field) exhibit very prominent CR acceleration (20% efficiency), while quasi-perpendicular regions exhibit efficiencies below 1%, consistent with the results of kinetic simulations. We also find that electrons are responsible for the majority of the γ -ray emission from SN 1006 (i.e., it is a leptonic source), with the exception of the northwest region due to an encounter with a dense cloud.
SN  - 0004-637X
SN  - 1538-4357
ER  -