Growing the terrestrial planets from the gradual accumulation of sub-meter sized objects

TL;DR

This paper applies the Viscous Stirred Pebble Accretion model to the terrestrial planet region, successfully reproducing the small mass of Mars and the asteroid belt by considering initial planetesimal sizes and accretion efficiency.

Contribution

It demonstrates that Viscous Stirred Pebble Accretion can explain the formation of terrestrial planets and the asteroid belt, addressing previous challenges in planet formation models.

Findings

VSPA reproduces small Mars and asteroid belt structure.

Accretion efficiency drops beyond 1.5 AU for asteroid-sized planetesimals.

Mars's growth is naturally limited by the model's accretion dynamics.

Abstract

Building the terrestrial planets has been a challenge for planet formation models. In particular, classical theories have been unable to reproduce the small mass of Mars and instead predict that a planet near 1.5 AU should roughly be the same mass as the Earth. Recently, a new model called Viscous Stirred Pebble Accretion (VSPA) has been developed that can explain the formation of the gas giants. This model envisions that the cores of the giant planets formed from 100 to 1000 km bodies that directly accreted a population of pebbles --- sub-meter sized objects that slowly grew in the protoplanetary disk. Here we apply this model to the terrestrial planet region and find that it can reproduce the basic structure of the inner Solar System, including a small Mars and a low-mass asteroid belt. Our models show that for an initial population of planetesimals with sizes similar to those of the main belt asteroids, VSPA becomes inefficient beyond $\sim\!$1.5 AU. As a result, Mars's growth is stunted and nothing large in the asteroid belt can accumulate.