Modelling the connection between propagating disturbances and solar spicules

Open Access

Fig. 4.

Time evolution of the velocity perturbation along field line 3 ( ${\hat{v}}_{‖}$ $\hat{v}_{\parallel}$ ) in the simulation with a photospheric wave driver, the temperature along field line 3, and the density perturbation ( $\hat{ρ}$ $\hat{\rho}$ ) along field line 3 calculated using Equation (1). An animated version of this figure is available online.

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