The upward energy fluxes and mass fluxes from the chromosphere to the corona. Panels (A)–(C) show the evolutions of upward energy fluxes carried by Alfvén (F_A) waves, fast-mode waves (F_fast) and slow-mode waves (F_slow), and the upward kinetic energy flux (F_kin) at Y = 1, 5, and 13 Mm, respectively, in the 2.5D run with initial magnetic field B₀ = 5 G. The averaged values within a cycle of spicule formation at different altitudes for this case are presented in panel (D). Panels (E)–(G) are the same but with an initial magnetic field of B₀ = 20 G, and the averaged values within a cycle of spicule formation at different altitudes for this case are presented in panel (H). The mass fluxes varying with time at Y = 1 Mm, Y = 5 Mm and Y = 13 Mm in the two cases are presented in panels (I)–(K), and the averaged values at different altitudes within a cycle of spicule formation for the two cases are presented in panel (L).