Particle acceleration at shocks propagating in inhomogeneous magnetic fields

Details Particle acceleration at shocks propagating in inhomogeneous magnetic fields Particle acceleration at shocks propagating in inhomogeneous magnetic fields

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006a%26a...455..685s&link_type=abstract

Astronomy and Astrophysics, Volume 455, Issue 2, August IV 2006, pp.685-695

Astronomy and Astrophysics

Astrophysics

8

Acceleration Of Particles, Ism: Cosmic Rays, Shock Waves, Sun: Particle Emission

Scientific paper

We consider particle acceleration at the scatter-free limit in quasi-planar shock waves propagating in inhomogeneous magnetic fields. It is shown that both non-constant magnetic field intensity and field-line curvature may lead to efficient acceleration of particles at shocks propagating through the structure. Shocks propagating towards increasing magnetic field intensity trap energetic particles, and as the field increases at the shock front the particles, by conserving their magnetic moment μ_B=E_⊥/B, increase their perpendicular energy by the ratio of maximum field magnitude to the field magnitude at the point of injection, E⊥,max = E⊥, inj B_max/B_inj. This may result in energy gains by factor of 100 in the solar corona. In addition, shocks propagating in curved magnetic fields may trap particles and accelerate them to high energies on field lines on which the shock-normal angle gradually increases toward 90°. Suitable field-line geometries should be common in many astrophysical objects, such as stellar coronae and quasi-perpendicular parts of supernova shocks.

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