Image Details
Caption: Fig. 1.
Effect of planet mass on spiral structure driven by an external planet. Simulations C, F, and I listed in Table 1 are shown. They have planet mass ratios ﹩q=( 3,5,10) \times 10^{-3}﹩ (left to right), disk aspect ratios ﹩h/ r=0.04﹩, and planet eccentricities ﹩e=0.25﹩. The Roche radius of the planet is shown as a white circle. The gas density is shown when the planet is at perihelion. The planet’s semimajor axis is at 1.2 times ﹩R_{\mathrm{max}\,}﹩, the disk outer edge. These simulations are shown at time ﹩t\sim 6P_{\mathrm{outer}\,}﹩ after the beginning of the simulation, where ﹩P_{\mathrm{outer}\,}﹩ is the rotation period at the disk outer edge.
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