# Making Terrestrial Planets: High Temperatures, FU Orionis Outbursts, Earth, and Planetary System Architectures

## TL;DR

This paper explores how high-temperature events like FU Orionis outbursts influence the formation of dry silicate planetesimals and the resulting architectures of planetary systems, addressing current gaps in planet formation theory.

## Contribution

It proposes molten grain collisions as a solution to dry silicate planetesimal formation and links accretion events to planetary system configurations.

## Key findings

- Molten grain collisions may produce dry silicate planetesimals.
- FU Orionis outbursts influence planetesimal location and system architecture.
- Systems with FU Orionis events resemble our Solar System.

## Abstract

Current protoplanetary dust coagulation theory does not predict dry silicate planetesimals, in tension with the Earth. While remedies to this predicament have been proposed, they have generally failed numerical studies, or are in tension with the Earth's (low, volatility dependent) volatile and moderately volatile elemental abundances. Expanding on the work of Boley et al. (2014), we examine the implications of molten grain collisions and find that they may provide a solution to the dry silicate planetesimal problem. Further, the source of the heating, be it the hot inner disk or an FU Orionis scale accretion event, would dictate the location of the resulting planetesimals, potentially controlling subsequent planetary system architectures. We hypothesize that systems which did undergo FU Orionis scale accretion events host planetary systems similar to our own, while ones that did not instead host very close in, tightly packed planets such as seen by Kepler.