The Nonlinear Amplification of Magnetic Fields by Cosmic Rays at Supernova Remnant Shocks

Brian Reville; Peter Duffy; Stephen O'Sullivan

doi:10.21427/dgzw-f436

The Nonlinear Amplification of Magnetic Fields by Cosmic Rays at Supernova Remnant Shocks

Brian Reville, Peter Duffy, Stephen O'Sullivan

School of Computer Science

Research output: Contribution to conference › Paper › peer-review

Abstract

A central problem in the theory of cosmic ray acceleration at supernova shock fronts is the generation of turbulent magnetic ﬁelds needed to scatter particles across a shock front. In this paper we build on previous studies [1], [2] into the effect of streaming cosmic rays produced by the outer shocks of supernova remnants on the stochastic component of the magnetic ﬁeld. A three dimensional, MHD code has been constructed which demonstrates the nonlinear growth of the turbulent ﬁeld.

Original language	English
DOIs	https://doi.org/10.21427/dgzw-f436
Publication status	Published - 2006
Event	33rd EPS Conference on Plasma Phys. - Rome, Italy Duration: 19 Jun 2006 → 23 Jun 2006

Conference

Conference	33rd EPS Conference on Plasma Phys.
Country/Territory	Italy
City	Rome
Period	19/06/06 → 23/06/06

Keywords

cosmic ray acceleration
supernova shock fronts
turbulent magnetic fields
streaming cosmic rays
stochastic component
MHD code
nonlinear growth

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10.21427/dgzw-f436Licence: CC BY-NC

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title = "The Nonlinear Amplification of Magnetic Fields by Cosmic Rays at Supernova Remnant Shocks",

abstract = "A central problem in the theory of cosmic ray acceleration at supernova shock fronts is the generation of turbulent magnetic ﬁelds needed to scatter particles across a shock front. In this paper we build on previous studies [1], [2] into the effect of streaming cosmic rays produced by the outer shocks of supernova remnants on the stochastic component of the magnetic ﬁeld. A three dimensional, MHD code has been constructed which demonstrates the nonlinear growth of the turbulent ﬁeld.",

keywords = "cosmic ray acceleration, supernova shock fronts, turbulent magnetic fields, streaming cosmic rays, stochastic component, MHD code, nonlinear growth",

author = "Brian Reville and Peter Duffy and Stephen O'Sullivan",

year = "2006",

doi = "10.21427/dgzw-f436",

language = "English",

note = "33rd EPS Conference on Plasma Phys. ; Conference date: 19-06-2006 Through 23-06-2006",

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TY - CONF

T1 - The Nonlinear Amplification of Magnetic Fields by Cosmic Rays at Supernova Remnant Shocks

AU - Reville, Brian

AU - Duffy, Peter

AU - O'Sullivan, Stephen

PY - 2006

Y1 - 2006

N2 - A central problem in the theory of cosmic ray acceleration at supernova shock fronts is the generation of turbulent magnetic ﬁelds needed to scatter particles across a shock front. In this paper we build on previous studies [1], [2] into the effect of streaming cosmic rays produced by the outer shocks of supernova remnants on the stochastic component of the magnetic ﬁeld. A three dimensional, MHD code has been constructed which demonstrates the nonlinear growth of the turbulent ﬁeld.

AB - A central problem in the theory of cosmic ray acceleration at supernova shock fronts is the generation of turbulent magnetic ﬁelds needed to scatter particles across a shock front. In this paper we build on previous studies [1], [2] into the effect of streaming cosmic rays produced by the outer shocks of supernova remnants on the stochastic component of the magnetic ﬁeld. A three dimensional, MHD code has been constructed which demonstrates the nonlinear growth of the turbulent ﬁeld.

KW - cosmic ray acceleration

KW - supernova shock fronts

KW - turbulent magnetic fields

KW - streaming cosmic rays

KW - stochastic component

KW - MHD code

KW - nonlinear growth

U2 - 10.21427/dgzw-f436

DO - 10.21427/dgzw-f436

M3 - Paper

T2 - 33rd EPS Conference on Plasma Phys.

Y2 - 19 June 2006 through 23 June 2006

ER -

The Nonlinear Amplification of Magnetic Fields by Cosmic Rays at Supernova Remnant Shocks

Abstract

Conference

Keywords

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