2011A&A...527A..10Z


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST01:19:32

2011A&A...527A..10Z - Astronomy and Astrophysics, volume 527A, 10-10 (2011/3-1)

The first stages of planet formation in binary systems: how far can dust coagulation proceed?

ZSOM A., SANDOR Z. and DULLEMOND C.P.

Abstract (from CDS):

On the basis of current theoretical models, giant planets can form via gravitational instability or core accretion. The terrestrial planets are ``failed cores'' in the core accretion paradigm that do not evolve into gas giants. Planets residing in binary systems place strong constraints on planet formation theory as any model must work in binary systems too, in spite of the strong perturbations from the secondary star. We examine the first phase of the core accretion model, namely the dust growth/fragmentation in binary systems. In our model, a gas and dust disk exists around the primary star and is perturbed by the secondary. We study the effects of a secondary with/without eccentricity on the dust population to determine the sizes the aggregates can reach and how that compares to the dust population in disks around single stars. We solve the equation of motion of dust aggregates including gas drag and gravitational forces from both stars, as well as the hydrodynamical equations for the gas disk. We determine the velocity of these particles relative to the gas (or relative to micron-sized, well-coupled dust particles) and construct a collision model with growth and erosion. Particles below the critical fragmentation velocity increase in mass by sweeping up the small dust population; particles above this critical speed are eroded by collisions with the small dust population. We use this model to determine the sizes that aggregates can reach in the disk, in addition to the equilibrium mass and stopping time distributions between growth and erosion. We find that the secondary star has two effects on the dust population: 1. the disk is truncated because of the presence of the secondary star, and the maximum mass of the particles is lower in lower gas densities. This effect is predominant in the outer disk; 2. the perturbation of the secondary increases the eccentricity of the gas disk, which in turn increases the relative velocity between the dust and the gas. Hence the maximum particle sizes are further decreased. The second effect of the secondary influences the entire disk. Coagulation is efficiently reduced even at the very inner parts of the disk. The average mass of the particles is lower by four orders of magnitude (as a consequence, the stopping time is shorter by one order of magnitude) in disks around binary systems than for dust in disks around single stars.

Abstract Copyright:

Journal keyword(s): binaries: general - planets and satellites: formation - protoplanetary disks - methods: numerical

Simbad objects: 4

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Number of rows : 4

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * alf Hyi PM* 01 58 46.1946699 -61 34 11.494778 3.33 3.13 2.84 2.55 2.39 F0IV 202 0
2 HD 41004 ** 05 59 49.6473573887 -48 14 22.805780232   9.49 8.65     K1IV 151 1
3 HD 196885 PM* 20 39 51.8753142885 +11 14 58.702911143   6.92 6.385 6.32   F8V 157 1
4 * gam Cep SB* 23 39 20.9015326708 +77 37 56.505477975 5.190 4.250   2.6   K1III-IVCN1 547 1

    Equat.    Gal    SGal    Ecl

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2020.07.10-01:19:32

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