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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 3.

Snapshots of simulations G101Dn5In4 (left) and G101Dn5In4n3 (right) at ﹩t=0.46\,{{\rm{\Omega }}}_{{\rm{KH}}}^{-1}﹩. The density distribution (color scale), poloidal velocity field (black arrows), and magnetic field lines (solid white lines) are shown. The scale of the poloidal velocity is shown at the top right of each panel. The magnetic field lines are depicted by the contours of the poloidal magnetic flux at several specific levels.

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