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Most detected planet-bearing binaries are in wide orbits, for which a highinclination, $i_B$, between the binary orbital plane and the plane of theplanetary disk around the primary is likely to be common. In this paper, weinvestigate the intermediate stages - from planetesimals to planetaryembryos/cores - of planet formation in such highly inclined cases. Our focus ison the effects of gas drag on the planetesimals' orbital evolution, inparticular on the evolution of the planetesimals' semimajor axis distributionand their mutual relative velocities. We first demonstrate that a non-evolvingaxisymmetric disk model is a good approximation for studying the effects of gasdrag on a planetesimal in the highly inclined case ($30^\circ <i_B<150^\circ$).We then find that gas drag plays a crucial role, and the results can begenerally divided into two categories, i.e., the Kozai-on regime and theKozai-off regime, depending on the specific value of $i_B$. For both regimes, arobust outcome over a wide range of parameters is that, planetesimalsmigrate/jump inwards and pile up, leading to a severely truncated and denseplanetesimal disk around the primary. In this compact and dense disk, collisionrates are high but relative velocities are low, providing conditions which arefavorable for planetesimal growth, and potentially allow for the subsequentformation of planets.

Planet Formation In Highly Inclined Binary Systems I. Planetesimals Jump Inwards And Pile Up