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A fundamental, unsolved problem in Solar System formation is explaining themelting and crystallization of chondrules found in chondritic meteorites.Theoretical models of chondrule melting in nebular shocks has been shown to beconsistent with many aspects of thermal histories inferred for chondrules fromlaboratory experiments; but, the mechanism driving these shocks is unknown.Planetesimals and planetary embryos on eccentric orbits can produce bow shocksas they move supersonically through the disk gas, and are one possible sourceof chondrule-melting shocks. We investigate chondrule formation in bow shocksaround planetoids through 3D radiation hydrodynamics simulations. A newradiation transport algorithm that combines elements of flux-limited diffusionand Monte Carlo methods is used to capture the complexity of radiativetransport around bow shocks. An equation of state that includes the rotational,vibrational, and dissociation modes of H$_2$ is also used. Solids are followeddirectly in the simulations and their thermal histories are recorded. Adiabaticexpansion creates rapid cooling of the gas, and tail shocks behind the embryocan cause secondary heating events. Radiative transport is efficient, and bowshocks around planetoids can have luminosities $\sim$few$\times10^{-8}$L$_{\odot}$. While barred and radial chondrule textures could be produced inthe radiative shocks explored here, porphyritic chondrules may only be possiblein the adiabatic limit. We present a series of predicted cooling curves thatmerit investigation in laboratory experiments to determine whether the solidsproduced by bow shocks are represented in the meteoritic record by chondrulesor other solids.

High-Temperature Processing of Solids Through Solar Nebular Bow Shocks: 3D Radiation Hydrodynamics Simulations with Particles