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Energy and Mass Transport Associated with Impulsive Spicular Flows in Solar Coronal Holes

  • Authors: Lei Ni, Jun Lin, Tanmoy Samanta, Guanchong Cheng, Yifu Wang, Robert Erdélyi

Lei Ni et al 2026 The Astrophysical Journal Letters 1000 .

  • Provider: AAS Journals

Caption: Figure 5.

Distributions of different variables in the zoomed lower atmosphere for the 2.5D run with B0 = 5 G at time 3461.07 s, when a bunch of new spicules just start to appear at the altitude between Y = 0.5 and 2 Mm. The logarithmic temperature (lgT) (A), current density (Jz) (B), magnetic field in the Y-direction (By) (C), the negative divergence of velocity (− ∇ · V) (D), the acceleration along the Y-direction contributed by the pressure gradient (Ap) (E), and the acceleration along the Y-direction contributed by the Lorentz force (AL) (F) are presented. The black thin solid line in panel (B) represents the position where the plasma β = 1.

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