Spiral patterns in planetesimal circumbinary disks

Abstract

Planet formation scenarios and the observed planetary dynamics in binaries pose a number of theoretical challenges, especially in what concerns circumbinary planetary systems. We explore the dynamical stirring of a planetesimal circumbinary disk in the epoch when the gas component disappears. For this purpose, following theoretical approaches by Heppenheimer (1978) and Moriwaki and Nakagawa (2004), we develop a secular theory for the dynamics of planetesimals in circumbinary disks. If the binary is eccentric and its components have unequal masses, a spiral density wave is generated, engulfing the disk on the secular timescale, which may exceed 10^7 yr, depending on the problem parameters. The spiral pattern is transient; thus, its observed presence may betray system's young age. We explore the pattern both analytically and in numerical experiments. The derived analytical spiral is a modified lituus; it matches the numerical density wave in the gas-free case perfectly. Using the SPH scheme, we explore the effect of residual gas on the wave propagation.

21 pages, 5 figures

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• Three-lane and multi-lane signatures of planets in planetesimal disks
• Circumbinary Disks of the Protostellar Binary Systems in the L1551 Region
• External or internal companion exciting the spiral arms in CQ Tau?
• Tidal decay of circumbinary planetary systems
• Simulations of the dynamics of the debris disks in the systems Kepler-16, Kepler-34, and Kepler-35
• "Horseshoe" Structures in the Debris Disks of Planet-Hosting Binary Stars
• Simulation of images of protoplanetary disks after collision with free-floating planets
• Dynamical environments of relativistic binaries: The phenomenon of resonance shifting