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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 20.

CPD midplane properties. Radial profiles of the midplane temperature (Tmid; top left), aspect ratio (bottom left), midplane density (top right), and rotational velocity normalized by the local Keplerian velocity (vϕ/vK; bottom right) are shown. Solid lines show the results from the selected simulations at their termination times (see Table 1). Dashed lines correspond to the profiles derived based on the analytic temperature prescription given by Equation (12), with labels T1500, T2000, and T4000 denoting analytic models with maximum temperatures set to ﹩{T}_{{\rm{\max }}}=1500\,{\rm{K}}﹩, 2000 K, and 4000 K, respectively (see Equation (12)). Vertical dotted lines in the right panels mark the outer boundary of the damping layer (r = 0.0032 rH). The blue dotted line in the bottom-right panel shows the rotational velocity of planet-corotating gas normalized by the local Keplerian velocity.

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