The effect of late giant collisions on the atmospheres of protoplanets and the formation of cold sub-Saturns

TL;DR

This paper explores how late giant collisions between protoplanets can strip planetary envelopes, leading to the formation of cold sub-Saturns and explaining their observed population without requiring runaway gas accretion.

Contribution

It demonstrates that giant collisions can prevent protoplanets from becoming gas giants, providing a new formation pathway for cold sub-Saturns consistent with observations.

Findings

Giant collisions can remove envelopes via super-Eddington winds.

Post-collision cores can resume accretion but often do not reach runaway growth.

Cold sub-Saturns can form without transforming into gas giants.

Abstract

We investigate the origins of cold sub-Saturns (CSS), an exoplanetary population inferred from microlensing surveys. If confirmed, these planets would rebut a theorised gap in planets' mass distribution between those of Neptune and Jupiter caused by the rapid runaway accretion of super-critical cores. In an attempt to resolve this theoretical-observational disparity, we examine the outcomes of giant collisions between sub-critical protoplanets. Due to the secular interaction among protoplanets, these events may occur in rapidly depleting discs. We show that impactors ~ 5% the mass of near-runaway envelopes around massive cores can efficiently remove these envelopes entirely via a thermally-driven super-Eddington wind emanating from the core itself, in contrast with the stellar Parker winds usually considered. After a brief cooling phase, the merged cores resume accretion. But, the evolution timescale of transitional discs is too brief for the cores to acquire sufficiently massive envelopes to undergo runaway accretion despite their large combined masses. Consequently, these events lead to the emergence of CSS without their transformation into gas giants. We show that these results are robust for a wide range of disc densities, grain opacities and silicate abundance in the envelope. Our fiducial case reproduces CSS with heavy (>= 30 M_Earth) cores and less massive (a few M_Earth) sub-critical envelopes. We also investigate the other limiting cases, where continuous mergers of comparable-mass cores yield CSS with wider ranges of core-to-envelope mass ratios and envelope opacities. Our results indicate that it is possible for CSS and Uranus and Neptune to emerge within the framework of well studied processes and they may be more common than previously postulated.