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We study the dust motion at the surface layer of protoplanetary disks. Dustgrains in surface layer migrate outward due to angular momentum transport viagas-drag force induced by the stellar radiation pressure. In this study, wecalculate mass flux of the outward motion of compact grains and porous dustaggregates by the radiation pressure. The radiation pressure force for porousdust aggregates is calculated using the T-Matrix Method for the Clusters ofSpheres. First, we confirm that porous dust aggregates are forced by strongradiation pressure even if they grow to be larger aggregates in contrast tohomogeneous and spherical compact grains to which efficiency of radiationpressure becomes lower when their sizes increase. In addition, we find that theoutward mass flux of porous dust aggregates with monomer size of 0.1 $\mu$m islarger than that of compact grains by an order of magnitude at the disk radiusof 1 AU, when their sizes are several microns. This implies that large compactgrains like calcium-aluminum rich inclusions (CAIs) are hardly transported toouter region by stellar radiation pressure, whereas porous dust aggregates likechondritic-porous interplanetary dust particles (CP-IDPs) are efficientlytransported to comet formation region. Crystalline silicates are possiblytransported in porous dust aggregates by stellar radiation pressure from innerhot region to outer cold cometary region in the protosolar nebula.

Outward Motion of Porous Dust Aggregates by Stellar Radiation Pressure in Protoplanetary Disks