Image Details
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.
© 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A.