The Primordial Entropy of Jupiter
Andrew Cumming, Ravit Helled, Julia Venturini

TL;DR
This paper investigates Jupiter's primordial entropy through formation simulations, revealing that non-convective interior regions are common and that formation parameters significantly influence its initial luminosity and entropy gradients.
Contribution
It introduces detailed formation models to quantify Jupiter's initial entropy and luminosity, emphasizing the importance of accretion rates and entropy gradients in early planetary evolution.
Findings
Proto-Jupiter often has non-convective interior regions.
Post-formation luminosity varies by a factor of 2-3 based on model parameters.
Entropy gradients can persist for about 10 million years after formation.
Abstract
The formation history of giant planets determines their primordial structure and consequent evolution. We simulate various formation paths of Jupiter to determine its primordial entropy, and find that a common outcome is for proto-Jupiter to have non-convective regions in its interior. We use planet formation models to calculate how the entropy and post-formation luminosity depend on model properties such as the solid accretion rate and opacity, and show that the gas accretion rate and its time evolution play a key role in determining the entropy profile. The predicted luminosity of Jupiter shortly after formation varies by a factor of -- for different choices of model parameters. We find that entropy gradients inside Jupiter persist for after formation. We suggest that these gradients should be considered together with heavy-element composition gradients when…
Peer Reviews
No public reviews on file for this paper yet. If you reviewed it on a platform where reviews are public (OpenReview, ICLR, NeurIPS, ICML), you can paste yours below so the community can read it here.
Videos
No videos yet. Explain this paper in a talk, walkthrough, or lecture? Add one.
