Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.1309f&link_type=abstract
American Astronomical Society, DPS meeting #38, #13.09; Bulletin of the American Astronomical Society, Vol. 38, p.506
Astronomy and Astrophysics
Astronomy
Scientific paper
In the standard scenario, the formation of planetesimal occurs through coagulation of the dust particles in the protoplanetary disks. However, the meter-sized particles rapidly fall into the central star due to the gas drag force before planetesimal formation. Thus, some outflow mechanisms are required for planetesimal formation. We perform numerical simulations of the radial circulation of the dust particles in weak turbulent protoplanetary disks, taking the stellar radiation pressure induced the dust outflow and a puffed-up inner rim with shadowed region (Dullemond et al. 2001) into account. Our main objective is to confirm that the following dust circulation mechanism will be realized in the protoplanetary disk: at the inner rim, falling dust particles partially evaporate and break up into fine grains, which are stirred up to the irradiated surface layer by magnetorotational instability (MRI) and blown outward by radiation pressure. The blowing particles reenter into the disk interior and settle toward the midplane. Most of the blowing particles reenter into the disk interior within 1AU and settle to the midplane, joining inwardly-migrating dust particles. We find that dust circulation is realized in the shadowed region of the disk. The outflow mass flux at the surface layer becomes a quasi-steady state on a short timescale compared with the disk evolution time through the inflow. Further, the outflow mass flux at the surface layer is comparable to the inflow mass flux at the disk interior in the shadowed region. From our results, we show that the steady surface density distribution of dust is enhanced due to dust circulation in the inner shadowed region. Their enhanced abundance of dust may cause planetesimal formation.
Fujiwara Daisuke
Watanabe Shin
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