PARTICLE ACCELERATION AND MAGNETIC FIELD AMPLIFICATION IN THE JETS OF 4C74.26

Journal Article · Sat Jun 20 00:00:00 EDT 2015 · Astrophysical Journal

DOI:https://doi.org/10.1088/0004-637X/806/2/243· OSTI ID:22522252

Araudo, A. T.; Blundell, K. M. ^[1]; Bell, A. R. ^[2]

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1. University of Oxford, Astrophysics, Keble Road, Oxford OX1 3RH (United Kingdom)
2. University of Oxford, Clarendon Laboratory, Parks Road, Oxford OX1 3PU (United Kingdom)

We model the multi-wavelength emission in the southern hotspot of the radio quasar 4C74.26. The synchrotron radio emission is resolved near the shock with the MERLIN radio-interferometer, and the rapid decay of this emission behind the shock is interpreted as the decay of the amplified downstream magnetic field as expected for small scale turbulence. Electrons are accelerated to only 0.3 TeV, consistent with a diffusion coefficient many orders of magnitude greater than in the Bohm regime. If the same diffusion coefficient applies to the protons, their maximum energy is only ∼100 TeV.

• OSTI ID: 22522252
• Journal Information: Astrophysical Journal, Vol. 806, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
ACCELERATION
AMPLIFICATION
COSMIC PROTONS
DIFFUSION
GALAXIES
INTERFEROMETRY
JETS
MAGNETIC FIELDS
QUASARS
SHOCK WAVES
TEV RANGE
TURBULENCE
WAVELENGTHS