Rapid Formation of Icy Super-Earths and the Cores of Gas Giant Planets

TL;DR

This paper presents a coagulation model demonstrating rapid formation of super-Earths and gas giant cores through interactions with the gaseous disk, explaining observed planetary mass distributions.

Contribution

The model introduces a new mechanism involving collision fragments and gas interaction, enabling quick planet formation within 1 million years.

Findings

Protoplanets reach Earth mass in about 1 Myr.

Super-Earths form more frequently than gas giants in low mass disks.

The model aligns with the Solar System's planetary mass distribution.

Abstract

We describe a coagulation model that leads to the rapid formation of super-Earths and the cores of gas giant planets. Interaction of collision fragments with the gaseous disk is the crucial element of this model. The gas entrains small collision fragments, which rapidly settle to the disk midplane. Protoplanets accrete the fragments and grow to masses of at least 1 Earth mass in roughly 1 Myr. Our model explains the mass distribution of planets in the Solar System and predicts that super-Earths form more frequently than gas giants in low mass disks.