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Driving Spiral Arms in the Circumstellar Disks of HD 100546 and HD 141569A

  • Authors: Alice C. Quillen, Peggy Varnière, Ivan Minchev, and Adam Frank

Quillen et al. 2005 The Astronomical Journal 129 2481.

  • Provider: AAS Journals

Caption: Fig. 6.

Role of disk thickness for external bound stellar‐mass companions. These simulations have mass ratios ﹩q=0.2﹩ and perturber eccentricities ﹩e=0.4﹩. The disk aspect ratios are ﹩h/ r=0.04﹩ for the top panels (simulation N) and ﹩h/ r=0.1﹩ for the bottom panels (simulation P). Left to right, each panel shows simulations just before periapse (left), at periapse, after periapse, and nearly at apoapse (right). The disk edge profile is smoother when the disk is thicker and the spiral structure is more open.

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