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- BL Lacertae objects: individual (TXS 0506+056, VER J0509+057) (1)
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- BL Lacertae objects: individual: 1ES 2344+514=VERJ2347+517 (1)
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- BL Lacertae objects: individual: Mrk501 (1)
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- X-rays: individuals: Vela Jr (RX J08520-4622) (1)
- accretion, accretion disks (1)
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- binaries: close (1)
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- data behind figure (1)
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- extraterrestrial intelligence (1)
- galaxies: clusters: general (1)
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- galaxies: general (1)
- galaxies: individual (BL Lacertae, VER J2202+422) (1)
- galaxies: individual (M 87) (1)
- galaxies: individual (M 87, VER J1230+123) (1)
- galaxies: individual (Markarian 501) (1)
- galaxies: individual (RGB J2243+203) (1)
- galaxies: individual: 1ES 1741+196=VER J1744+195 (1)
- galaxies:active (1)
- gamma rays : stars (1)
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- gamma-ray burst: individual (GRB 130427A) (1)
- gamma-ray burst: individual (GRB 150323A) (1)
- gamma-ray burst: individual (MGRO J1908+06, VER J1907+062) (1)
- gamma-rays: galaxies (1)
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- hydrodynamics (1)
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- magnetohydrodynamics (MHD) (1)
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- solar wind (1)
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- stars: individual (LS I+61 degrees 303, VER J0240+612) (1)
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- stars: individual (zeta Oph, BD+43 degrees 3654) (1)
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- supernovae : individual (CTB 87) (1)
- supernovae: individual (G0.9+0.1) (1)
- surveys (1)
- techniques: photometric (1)
- the Weibel instability (1)
Institute
Thermal electrons have gyroradii many orders of magnitude smaller than the finite width of a shock, thus need to be pre-accelerated before they can cross it and be accelerated by diffusive shock acceleration. One region where pre-acceleration may occur is the inner foreshock, which upstream electrons must pass through before any potential downstream crossing. In this paper, we perform a large-scale particle-in-cell simulation that generates a single shock with parameters motivated from supernova remnants. Within the foreshock, reflected electrons excite the oblique whistler instability and produce electromagnetic whistler waves, which comove with the upstream flow and as nonlinear structures eventually reach radii of up to 5 ion-gyroradii. We show that the inner electromagnetic configuration of the whistlers evolves into complex nonlinear structures bound by a strong magnetic field around four times the upstream value. Although these nonlinear structures do not in general interact with cospatial upstream electrons, they resonate with electrons that have been reflected at the shock. We show that they can scatter, or even trap, reflected electrons, confining around 0.8% of the total upstream electron population to the region close to the shock where they can undergo substantial pre-acceleration. This acceleration process is similar to, yet approximately three times more efficient than, stochastic shock drift acceleration.