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Stochastic Electron Acceleration in Shell-Type Supernova Remnants

This study explores the mechanisms behind electron acceleration in shell-type supernova remnants (SNRs), highlighting the challenges faced by leptonic and hadronic models in explaining the observed multi-wavelength spectra, particularly in RX J1713.7-3946. We discuss the viability of stochastic electron acceleration via fast-mode waves and show how this mechanism can provide a suitable electron distribution while addressing known observational constraints such as X-ray variability and energy equipartition. Understanding these processes is crucial for distinguishing between competing models through advanced observational techniques.

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Stochastic Electron Acceleration in Shell-Type Supernova Remnants

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  1. Stochastic Electron Acceleration in Shell-Type Supernova Remnants Siming Liu Los Alamos National Laboratory In Collaboration with Zhonghui Fan, Christopher L. Fryer, Jianmin Wang, and Hui Li

  2. Challenges to the Leptonic Models 1 TeV spectrum too narrow: Background photon? Porter et al. Tanaka et al.

  3. Uchiyama et al. 2007 2 Weak B field: Variability Challenges to the Leptonic Models Tanaka et al.

  4. A New Paradigm for Collisionless Shocks Lee et al. 1994

  5. Speed Profiles in the Downstream vA<<U

  6. Turbulence spectrum

  7. Electron Acceleration by Fast Mode Waves

  8. Spectral Fit to SNR RX J1713.7-3946

  9. Kelvin-Helmholtz Instability? No Thermal X-rays The Nature of the SNR Shock

  10. Nonthermal Electron Energy Thermal Energy Acceleration Efficiency Energy equipartition between B and nonthermal electrons

  11. X-ray Variability Scattering Mean Free path Filament Width Diffusion Time: 0.93 yr Uchiyama et al. 2007

  12. Conclusions Hadronic model faces several challenges in accounting for the broadband spectrum of shell-type supernova remnants Leptonic models need a gradual high energy cutoff Stochastic electron acceleration by fast mode waves in the downstream of collisionless shocks can produce the required electron distribution with reasonable model parameters. Hard X-ray and gamma-ray observations can distinguish these models

  13. Observations HESS

  14. No thermal X-rays Egret upper limit 1 Suppression of Electron Acceleration 4 Hard Spectrum with p<2.0 2 High Energy & 3 Density Requirement Challenges to the Hadronic Models SNR RX J1713.7-3946 Tanaka et al.

  15. 5 B Field Amplification Challenges to the Hadronic Models Tanaka et al.

  16. Challenges to the Hadronic Models 6 Lack of Correlation between TeV and Cloud Distribution: Plaga

  17. Acceleration Time

  18. SNR RX J0852.0-4622 and Cas A (Preliminary)

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