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Interactions between the Planetary Magnetic Field and the Surrounding Gas Flows in the Final Stage of the Giant Planet Formation. I. Two Distinct Evolutionary Scenarios

  • Authors: Pengfei Tang, Xiaogang Wang, Tianchun Zhou, Jiayong Zhong

Pengfei Tang et al 2026 The Astrophysical Journal 1005 .

  • Provider: AAS Journals

Caption: Figure 15.

Time evolution of Uϕ, ﹩{\dot{U}}_{\phi ,{\rm{C}}F}﹩, ﹩{\dot{U}}_{\phi ,{\rm{L}}or}﹩, ﹩{\dot{U}}_{\phi ,{\rm{BD}}}﹩, ﹩{\dot{U}}_{\phi ,{\rm{J}}oule}﹩, and ﹩{\dot{U}}_{\phi ,{\rm{R}}F}﹩ within the twisted upper-half magnetosphere for simulations G101Dn5In4n3 and G101Dn5In4n4m5. The volume integral is taken over the twisted upper-half magnetosphere in the rθ plane, with the toroidal integral omitted due to axisymmetry. Specifically, the volume element is ﹩dV={r}^{2}\sin (\theta )drd\theta ﹩. The red circles mark the ends of the high-latitude accretion of the gas at the CPD inner edge (see the text for details). The top and bottom panels share the same x-axis, while the left and right panels share the same y-axis.

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