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The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation

  • Authors: Shangjia Zhang, Zhaohuan Zhu, Jane Huang, Viviana V. Guzmán, Sean M. Andrews, Tilman Birnstiel, Cornelis P. Dullemond, John M. Carpenter, Andrea Isella, Laura M. Pérez, Myriam Benisty, David J. Wilner, Clément Baruteau, Xue-Ning Bai, and Luca Ricci

2018 The Astrophysical Journal Letters 869 L47.

  • Provider: AAS Journals

Caption: Figure 1.

Two-dimensional gas surface density in log scale for h/r = 0.05, 0.07, and 0.1 from left to right panel blocks. In each block, the models for α = 10−4, 10−3, 10−2 are shown from left to right. The planet mass increases from top to bottom, namely Mp = 11 M, 33 M, 0.3 MJ, 1 MJ and 3 MJ, if M* = M. In each panel, the star is located at the center, and the plotting region is 3 × 3 in units of rp, where rp is the distance between the star and the planet. The planet is located at (x, y) = (1, 0) and orbits counterclockwise around the star. Σmax and Σmin are chosen to highlight the structures in each panel.

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