Properties of the confined magnetosphere at ﹩t=0.6614\,{{\rm{\Omega }}}_{{\rm{KH}}}^{-1}﹩ for simulation G101Dn5In4n4m4. Panels (a)–(d) display the distributions of ρ, ﹩{\tau }_{e,{\rm{CF}}}^{-1}﹩, ﹩{\tau }_{e,{\rm{Lor}}}^{-1}﹩, and ﹩{\tau }_{e,{\rm{CF}}}^{-1}﹩+﹩{\tau }_{e,{\rm{Lor}}}^{-1}﹩, respectively. Panels (e)–(h) show the distributions of B_ϕ, ﹩{\tau }_{e,{\rm{Joule}}}^{-1}﹩, ﹩{\tau }_{e,{\rm{RF}}}^{-1}﹩, and ﹩{\tau }_{e,{\rm{tot}}}^{-1}﹩, respectively. Symmetrical logarithmic color scales are utilized in panels (b)–(d) and (f)–(h), with the range from −10² to 10² shown in linear scale while the other parts in logarithmic scale. In all panels, magnetic field lines are depicted by thin solid lines (white in panel (a), black in panels (b)–(h)). In each panel, these lines trace the poloidal magnetic flux contours at the same set of specific levels. Magenta solid lines delineate the twisted upper-half magnetosphere where B_ϕ/B_pol > 0.05, 4πρv²/B² < 1.0, and θ < π/2. Black dashed lines in panels (b)–(h) indicate the contours of the critical density ﹩{\rho }_{{\rm{crit}}}=100\,{\rho }_{{\rm{\inf }}}﹩, aiding in the identification of the disk profile. Poloidal velocity field is depicted by black arrows in panel (a), with the scale shown at the top right of the panel. Convective and resistive energy fluxes (see definitions in Section 3) within the twisted upper-half magnetosphere are illustrated by lime arrows in panel (b) and cyan arrows in panel (g), respectively, with the scales shown at the top right of the panels. Lorentz force component, J_pol × B/c, and total Lorentz force, J × B/c, within the twisted magnetosphere are presented by blue arrows in panel (c) and violet arrows in panel (e), respectively, with the scale shown at the top right of the panels. The poloidal current field is shown by the salmon streamlines in panel (f). For reference, the escape velocity and the Keplerian timescale at the planetary radius (r_pl = 0.0027 r_H) are v_esc = 27v_KH and ﹩{{\rm{\Omega }}}_{{\rm{K}}}^{-1}=1.4\times 1{0}^{-4}\,{{\rm{\Omega }}}_{{\rm{KH}}}^{-1}﹩, respectively.