• Corpus ID: 244908823

Standard Self-Confinement and Extrinsic Turbulence Models for Cosmic Ray Transport are Fundamentally Incompatible with Observations

@inproceedings{Hopkins2021StandardSA,
  title={Standard Self-Confinement and Extrinsic Turbulence Models for Cosmic Ray Transport are Fundamentally Incompatible with Observations},
  author={Philip F. Hopkins and Jonathan Squire and Iryna S. Butsky and Suoqing Ji},
  year={2021}
}
Models for cosmic ray (CR) propagation and dynamics fundamentally depend on the rate of CR scattering from magnetic fluctuations. In the ISM, for CRs with energies from ∼MeV-TeV, these fluctuations are usually attributed either to “extrinsic turbulence” (ET) – a cascade of turbulent fluctuations from larger scales – or “self-confinement” (SC) – self-generated fluctuations from CR streaming. Using simple analytic arguments and detailed numerical simulations of CR transport in galaxy formation… 

Figures and Tables from this paper

References

SHOWING 1-10 OF 10 REFERENCES

Transport Processes in Space Physics and Astrophysics

Statistical Background.- The Boltzmann transport equation.- Charged particle transport in a collisional magnetized plasma.- Charged particle transport in a collisionless magnetized plasma.- The

Physical Processes In The Interstellar Medium

Progress in Particle and Nuclear

  • Azh,
  • 1963

Zeitschrift fur Physik B Condensed Matter

  • 1976

The Nonlinear Diffusion Equation: Asymptotic Solutions and Statistical Problems

Since the 'Introduction' to the main text gives an account of the way in which the problems treated in the following pages originated, this 'Preface' may be limited to an acknowledgement of the

2020) that the spectrum should be closer to eturb(k) ∝ k−1 (giving δs = 0)

  • And the classic Kolmogorov
  • 1941

It is also not clear that isotropy is a good assumption on small scales even for fast modes

  • Kuznetsov & Krasnoselskikh
  • 2008

Below the Alfvén scale `A, where |δv2(λ∼ `A)|〉 ∼ vA, ideal the fluctuations are sub-Alfvénic, by definition

  • Squire & Hopkins
  • 2009

2021b, arXiv e-prints, p

  • 2021

Makwana & Yan 2020) that the spectrum should be closer to eturb(k) ∝ k −1 (giving δs = 0)

  • And the classic Kolmogorov
  • 1941