435 citations · 5.6k across the 113 of their papers we have counts for
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Opacity of fluffy dust aggregates
Akimasa Kataoka, Satoshi Okuzumi, Hidekazu Tanaka +1
Context. Dust grains coagulate to form dust aggregates in protoplanetary disks. Their porosity can be extremely high in the disks. Although disk emission may come from fluffy dust…
Radial Transport of Large-Scale Magnetic Fields in Accretion Disks. I. Steady Solutions and an Upper Limit on the Vertical Field Strength
Satoshi Okuzumi, Taku Takeuchi, Takayuki Muto
Large-scale magnetic fields are key ingredients of magnetically driven disk accretion. We study how large-scale poloidal fields evolve in accretion disks, with the primary aim of q…
Radial Transport of Large-Scale Magnetic Fields in Accretion Disks. II. Relaxation to Steady States
Taku Takeuchi, Satoshi Okuzumi
We study the time evolution of a large-scale magnetic flux threading an accretion disk. Induction equation of the mean poloidal field is solved under the standard viscous disk mode…
Fluffy dust forms icy planetesimals by static compression
Akimasa Kataoka, Hidekazu Tanaka, Satoshi Okuzumi +1
Context: In planetesimal formation theory, several barriers have been proposed, which are bouncing, fragmentation, and radial drift problems. To understand the structure evolution…
The fate of planetesimals in turbulent disks with dead zones. II. Limits on the viability of runaway accretion
Chris Ormel, Satoshi Okuzumi
A critical phase in the standard model for planet formation is the runaway growth phase. During runaway growth bodies in the 0.1--100 km size range (planetesimals) quickly produce…
The Fate of Planetesimals in Turbulent Disks with Dead Zones. I. The Turbulent Stirring Recipe
Satoshi Okuzumi, Chris W. Ormel
Turbulence in protoplanetary disks affects planet formation in many ways. While small dust particles are mainly affected by the aerodynamical coupling with turbulent gas velocity f…
Static compression of porous dust aggregates
Akimasa Kataoka, Hidekazu Tanaka, Satoshi Okuzumi +1
Context: In protoplanetary disks, dust grains coagulate with each other and grow to form aggregates. As these aggregates grow by coagulation, their filling factor ϕdecreases down t…