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

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.

6 pages, Accepted, ApJL

References in corpus (14)

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• What pebbles are made of: Interpretation of the V883 Ori disk
• HD 145263: Spectral Observations of Silica Debris Disk Formation via Extreme Space Weathering?
• Gaia21bty: An EXor lightcurve exhibiting an FUor spectrum
• A Chemical Map of the Outbursting V883 Ori system: Vertical and Radial Structures
• Ejection of Chondrules from Fluffy Matrices
• Gaia20bdk -- a new FUor in Sh 2-301 Star Forming Region
• Cosmic Dust IX