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Eiichiro Kokubo uses numerical dynamics to investigate planet formation. His work with Shigeru Ida identified a regime of oligarchic growth, where neighboring large protoplanets accrete smaller planetesimals while remaining dynamically separated.

The large bodies alter the very population from which they grow: their gravity increases small-body random velocities, changing subsequent collision and capture rates. Following this feedback distinguishes the oligarchic regime from a simple extrapolation in which the largest object keeps outgrowing all its neighbors indefinitely.^[ref]

Oligarchic growth is the stage in which a relatively small number of planetary embryos dominate the dynamics of many smaller planetesimals. It follows runaway planetesimal growth. The embryos remain separated, grow to broadly comparable masses within similar local disk conditions, and regulate their accretion by stirring the population that supplies their material. The primary numerical study describes this embryo–planetesimal structure and typical separations of about ten individual Hill radii.^[ref]

The key feedback is gravitational focusing. In a dispersion-dominated encounter with approach speed $v$ and a small impactor, conservation of energy and conservation of angular momentum give the collision cross-sectionAt fixed internal mass density, $R\propto M^{1/3}$ and $v_{\mathrm{esc}}^2\propto M^{2/3}$. If the background random speed initially is controlled by small planetesimals and varies little with embryo mass, strong focusing gives ${\sigma }_{\mathrm{coll}}\propto M^{4/3}$. For a disk with planetesimal thickness of order $v_z/{\Omega }_K$ and a fixed ratio $v/v_z$, the associated estimate isup to geometric factors. With nearly fixed $v$, this gives $\dot{M}\propto M^{4/3}$ and $\dot{M}/M\propto M^{1/3}$: the largest bodies have the shortest fractional growth times, the essence of runaway growth.

As embryos grow, their gravitational encounters increasingly excite the random eccentricities and inclinations of nearby planetesimals. This is viscous stirring of planetesimals, not molecular fluid viscosity. Higher encounter speeds lower the focusing factor. The largest local embryo heats its feeding population most strongly and thereby suppresses its own relative growth advantage. Gas drag and dissipative collisions oppose stirring; dynamical friction tends to keep the more massive embryos' random motions relatively small while transferring random energy to lighter bodies. The balance between these processes controls the accretion rate.

For an illustrative self-regulated scaling $v\propto M^{1/3}$, the ratio $v_{\mathrm{esc}}/v$ is approximately fixed. The previous growth estimate becomesLarger embryos now grow more slowly in fractional terms, allowing neighboring embryos in comparable environments to approach similar masses. This scaling illustrates the feedback; it is not a universal exact exponent for every planetesimal size distribution, damping law or disk surface-density profile. In particular, a two-body focusing cross-section must be modified in the shear-dominated regime, where encounters are governed by the stellar tidal field.

The relevant gravitational interaction scale is the Hill radius,Close embryo encounters and orbital repulsion keep adjacent embryos separated by several Hill-scale lengths. The mutual Hill radius uses their combined mass; for equal neighboring masses it is $2^{1/3}{R}_H$. Stating which definition is used matters when quoting a spacing coefficient. The spacing is a dynamical scale, not an exact universal integer.

Each feeding zone of a planetary embryo contains a finite solid reservoir. To estimate its isolation mass, let the full annular width be $\Delta a=B{R}_H$, where the dimensionless coefficient $B$ includes the stated choice of width and Hill-radius convention. For local solid surface density ${\Sigma }_s$,Solving givesThus denser solid disks and wider feeding annuli allow larger embryos. If ${\Sigma }_s\propto a^{-p}$, the estimate scales as $M_{\mathrm{iso}}\propto a^{3-3p/2}$ at fixed host mass and $B$. This is a local exhaustion estimate, not an absolute maximum planet mass: radial delivery of solids, pebble accretion, migration and embryo mergers can replenish or enlarge a feeding zone. No solid surface-density normalization is given, so a numerical isolation mass would require an invented disk model.

As the local supply is depleted, growth slows further. After gas damping weakens, embryo orbits may cross and giant collisions can assemble larger terrestrial planets. Farther out, sufficiently massive cores may instead acquire gas before protoplanetary disk dispersal. Oligarchic growth explains why a few comparable embryos share a disk while many smaller planetesimals remain: gravitational stirring weakens focusing and makes accretion self-regulating.

Shigeru Ida studies the assembly of planets from smaller orbiting bodies. With Eiichiro Kokubo, he investigated oligarchic growth, in which a relatively small population of large protoplanets grows by accreting surrounding planetesimals.

The large bodies also stir the random motion of the smaller ones. That dynamical heating changes their capture efficiency, so growth cannot be inferred from mass alone. Their numerical calculations connected growth and orbital spacing, helping explain how a disk of many small bodies can develop a more orderly population of planetary embryos.^[ref]