What’s in a gas giant?
No, really. The interiors of Jupiter and Saturn are actually quite difficult to probe. But Saturn’s uniquely glorious and extensive ring system is proving to be an excellent tool for figuring out the densities deep below its thick cloud layers, right down to the core.
That core, according to a new analysis of ‘wobbles’ in Saturn’s innermost main ring, likely isn’t a dense ball of nickel and iron, as many think, but a “fuzzy” region of mostly hydrogen and helium, with a gradual mixing of heavier elements, extending to 60 percent of the planet’s radius and containing around 17 Earth masses of ice and rock.
This finding, published in Nature Astronomy, is similar to recent findings about Jupiter’s interior based on Juno data, and it could change our assumptions about Saturn’s early structure and formation history.
“The fuzzy cores are like a sludge,” said planetary scientist and lead author of the study, Christopher Mankovich from Caltech.
“The hydrogen and helium gas in the planet gradually mix with more and more ice and rock as you move toward the planet’s center. It’s a bit like parts of Earth’s oceans where the saltiness increases as you get to deeper and deeper levels, creating a stable configuration.”
What the core could look like. (Caltech/R. Hurt, IPAC)
How can we learn that from Saturn’s rings? It all has to do with the way rumbles in Saturn’s belly influence the planet’s external gravitational field.
“We used Saturn’s rings like a giant seismograph to measure oscillations inside the planet,” said co-author and Caltech astrophysicist Jim Fuller. “This is the first time we’ve been able to seismically probe the structure of a gas giant planet, and the results were pretty surprising.”
Acoustic waves and oscillations inside cosmic bodies are a brilliant tool for probing their interior structure.
We do it here on Earth, where quakes send similar waves rippling through the planet; how these waves bounce around in there can reveal different densities, allowing us to identify structures we could never hope to see.
On the Sun, and other stars, interior acoustic waves manifest as brightness fluctuations.
Saturn is no place for a seismometer, and it doesn’t undergo brightness fluctuations, but a few years ago, scientists noticed signature patterns in Saturn’s C ring, the innermost of its main rings.
These, they concluded, were unlikely to be produced by Saturn’s moons, as such patterns are in the outer rings; instead, they seem to be generated by oscillations deep in the planetary interior, which influence the gravitational field.
How internal oscillations should affect Saturn’s rings. (Matthew Hedman/University of Idaho)
Thus the field of kronoseismology emerged: the study of Saturn’s interior by analyzing these waves in the C ring.
Now the Caltech team has conducted a new analysis of a previously characterized inner C ring wave, whose frequency was much lower than expected of the established Saturn interior model. This frequency pattern, they found, places a stringent new constraint on Saturn’s interior composition.
“Our models place tight constraints on the mass and size of the heavy-element core of Saturn, even though the dilute nature of this core requires a more nuanced description than in traditional layered models,” they write in their paper.
Based on these constraints, they inferred that the mass of the core is around 55 times the mass of Earth, containing 17 Earth masses’ worth of rock and ice.
The rest would predominantly be hydrogen and helium; the entire thing is diffuse and gradually mixed, rather than strictly delineated stratification, with a denser concentration of heavier elements in the very center.
This poses something of a challenge for planetary formation models. It’s thought that planets form from a bottom-up, pebble accretion model, in which small chunks of rock are electrostatically bound together until the planetary ‘seed’ is large enough to gravitationally attract more and more material – eventually forming a planet.
For gas giants, like Jupiter and Saturn, heavier material was thought to sink towards the center, forming a solid core and letting the lower-density gas rise to the outer regions.
Recent models suggest more gradual distribution of material; or it’s possible that convective mixing results in a more gradual distribution.
Even so, modeling formation pathways for a fuzzy core has proven challenging, and it’s likely that more complex science jiggery-pokery will be required to fully understand how it can happen.
That may be putting the cart a little before the horse, though. The new study is based on one C ring wave. A little more kronoseismology would help validate the interpretation of a fuzzy Saturn core.
The research has been published in Nature Astronomy.
An earlier version of this article was published in May 2021.
