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Wave–Particle Interaction in the Upstream of Interplanetary Coronal Mass Ejection Shocks

  • Authors: Shanwlee Sow Mondal, Aveek Sarkar, Sofiane Bourouaine

Shanwlee Sow Mondal et al 2025 The Astrophysical Journal 987 .

  • Provider: AAS Journals

Caption: Figure 1.

A typical shock chosen from Table 1, identified as shock 2. The vertical dashed line denotes the arrival time of the shock. The upper plot displays the particle flux of various energetic particles (from 72 keV to 6.7 MeV) near the shock occurrence. Parameters such as the magnitude of the magnetic field (∣B∣), the three components of the magnetic field (Bx, By, Bz), particle density (np), bulk proton velocity (Vp), bulk α particle velocity (Vα), and the evolution of temperature anisotropy (T/T) are graphically represented around the time of the shock arrival.

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