Computer Science
Scientific paper
Apr 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002em%26p...88...89d&link_type=abstract
Earth, Moon, and Planets Volume 88, Number 2, pp. 89-113
Computer Science
2
Accretion, Accretion Disks, Celestial Mechanics, Stellar Dynamics, Solar System, Formation, Circumstellar Matter, Planetary Systems, Triple Systems, Stars, Pre-Main Sequence
Scientific paper
The star formation process usually leads to the formation of protoplanetary disks. Planets are thought to arise from the material of these disks. Amongst the stars in the solar neighbourhood, single systems like our own are a minority. Most stars are found in binaries or in systems of even higher multiplicity. In this paper, we extend the simulations presented in Paper I (de la Fuente Marcos and de la Fuente Marcos, 1998a) to hierarchical triple systems. As in Paper I, we study the stage of planetary formation during which the particulate material is still dispersed as centimetre-to-metre sized primordial aggregates. We investigate the response of the particles, in a protoplanetary disk with radius RD = 100 AU around a solar-like star, to the gravitational field of bound perturbing companions in a moderately wide (300 1600 AU) orbit. As for this problem no analytic description of the orbital evolution of the particles exists, we perform numerical integrations using a Bulirsch Stoer integrator. For this purpose, we have carried out a series of simulations of coplanar hierarchical configurations with three stars using a direct integration code that models gravitational and viscous forces. The massive protoplanetary disk is around one of the components of the triple system. As in Paper I, the evolution in time of the dust sub-disk depends mainly on the nature (prograde or retrograde) of the relative revolution of the stellar companions, and on the temperature and mass of the circumstellar disk. The perturbation of prograde companions induces a trailing spiral structure across the protoplanetary sub-metric dust sub-disk. Metre-sized particles are affected by strong precession. Our results show that the lifetime of particles in a disk in a hierarchical triple system is slightly shorter relative to its valuein Paper I, although the actual value depends on the nature, prograde or retrograde, of the outer companion. The lifetime of particles in a hierarchical triple system including a prograde inner binary and a retrograde outer body is longer than in an equivalent triple with all the companions prograde. Dust disks in hierarchical triple systems with both companions in retrograde motion with respect to the particles in the disk show the shortest lifetimes. Our previous calculations suggest that disk luminosities in binary systems are several orders of magnitude higher than those for single stars. Circumstellar disks in triple systems may be 5 50% more luminous depending on the relative direction of rotation.
de la Fuente Marcos Carlos
de la Fuente Marcos Raúl
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