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Acceleration of Electrons and Ions by an “Almost” Astrophysical Shock in the Heliosphere

  • Authors: Immanuel Christopher Jebaraj, Oleksiy Agapitov, Vladimir Krasnoselskikh, Laura Vuorinen, Michael Gedalin, Kyung-Eun Choi, Erika Palmerio, Nicolas Wijsen, Nina Dresing, Christina Cohen, Athanasios Kouloumvakos, Michael Balikhin, Rami Vainio, Emilia Kilpua, Alexandr Afanasiev, Jaye Verniero, John Grant Mitchell, Domenico Trotta, Matthew Hill, Nour Raouafi, Stuart D. Bale

Immanuel Christopher Jebaraj et al 2024 The Astrophysical Journal Letters 968 .

  • Provider: AAS Journals

Caption: Figure 2.

Energetic particles and the evolution of the wave foreshock. Panels (A)–(D) show the time–energy plots for high-energy electron counts detected by EPI-Hi, low-energy electron flux from EPI-Lo, proton flux from EPI-Lo, and the amplitude of transversal (⊥) and parallel (∥) magnetic fluctuations. In panel (E), we present the proton intensity spectra for three selected times (06:40, 07:10, and at the shock, averaged as 07:13–07:15 UT) with an E −1 power law shown for reference, which indicates the changes in energetic particle distribution. Panel (F) shows the Fourier power spectra of B R (estimating B power) and the sum of B T and B N (estimating B power) in the foreshock and the background. Variations in the proton flux and magnetic fluctuations over a 2 minute period surrounding the shock transition are shown in panels (G) and (H).

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