In recent years, the Juno mission revealed that Jupiter's core was much more diffuse than astronomers had expected.

One theory is that "within a few million years" of its formation, Jupiter experienced a head-on collision with a planetesimal of about $10M_{⊕}$, adding a lot more mass to its core from the silicate planetesimal, but also causing the core's contents to be broken up and mixed with the inner envelope.

The models used in this theory placed Jupiter at a distance of 5.2 AU from the Sun, which is approximately the same as its semi-major axis in the present day. The planetesimal in question would be at the higher end of the valid mass range for a Super-Earth.

Now, according to the Grand Tack theory, Jupiter originally formed at a distance of $\approx 3.5$ AU and migrated inwards toward the Sun, before gravitational interactions with Saturn caused the two planets to move outward and brought Jupiter to its present-day orbit.

Saturn itself would have formed at a distance of $\approx 4.5$ AU, increasing in mass from $30M_{⊕}$ to $60M_{⊕}$ during the first $10^5$ years of Jupiter's inward migration, before starting its own inward migration. This would have been much faster than Jupiter's, enabling Saturn to "catch up" and the gravitational interactions as described to then occur.

The original formations would all have occurred over a timescale of $\lessapprox 6Myr$, maybe closer to $\approx 3Myr$. (The original paper describing the Grand Tack refers only to "a few Myr"; the figures here are based on "Disc Frequencies and Lifetimes in Young Clusters", which it cites in support of this.) The inward and outward migrations would then have occurred in an 800,000 year time period (see Figure 1 of the Grand Tack paper)

(Incidentally, the cores of Uranus and Neptune are each $\approx 5M_{⊕}$ at the start of this migration, increasing to values $> 10M_{⊕}$ at the end of it.)

Diagram from arXiv 1201.5177)

So far, the two models look quite compatible with each other, with the collision occuring after Jupiter settles into its 5.2 AU orbit. But there is one detail I'm not sure about. Here comes the question:

  • Descriptions of the Grand Tack theory describe Jupiter as scattering early planetesimals as its gravity disturbed their orbits. Some collided with each other, some were propelled into the Sun... Is it more likely that one of these collided with Jupiter itself at the head-on angle needed for the core-warping collision? Which would mean the impact occurred before Jupiter reached its final orbit.

In addition...

  • The "few million years" timescale is quite vague. Does anyone know any additional detail which might suggest the impact occurred prior to the Grand Tack's timeframe?

References (not paywalled):

Haisch Jr, K. E., Lada, E. A., & Lada, C. J. (2001). Disk frequencies and lifetimes in young clusters. The Astrophysical Journal Letters, 553(2), L153.

Walsh, K. J., Morbidelli, A., Raymond, S. N., O'Brien, D. P., & Mandell, A. M. (2011). A low mass for Mars from Jupiter’s early gas-driven migration. Nature, 475(7355), 206-209.

Liu, S. F., Hori, Y., Müller, S., Zheng, X., Helled, R., Lin, D., & Isella, A. (2019). The formation of Jupiter's diluted core by a giant impact. Nature, 572(7769), 355-357.

Guillot, T. (2019). Signs that Jupiter was mixed by a giant impact.

with accompanying articles:

Wall, M. (2017). More Jupiter Weirdness: Giant Planet May Have Huge, 'Fuzzy' Core. (space.com)

Weitering, H. (2018). 'Totally Wrong' on Jupiter: What Scientists Gleaned from NASA's Juno Mission. (space.com)

(2019). A core-warping impact in Jupiter's past? (Astronomy Now)

A paper cited in earlier versions of this question but which turned out to be incompatible with the Grand Tack theory:

Pirani, S., Johansen, A., Bitsch, B., Mustill, A. J., & Turrini, D. (2019). Consequences of planetary migration on the minor bodies of the early solar system. Astronomy & Astrophysics, 623, A169.

with accompanying article:

Jupiter's unknown journey revealed

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    $\begingroup$ Unpaywalled: arxiv.org/abs/2007.08338 $\endgroup$ – Keith McClary Dec 6 '20 at 4:25
  • $\begingroup$ @KeithMcClary Big thanks for that. I'm at work right now but will edit that into the question later. Thanks again! $\endgroup$ – Astrid_Redfern Dec 7 '20 at 11:01
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    $\begingroup$ Something I have concern with though is that your link proposing to take place 2-3 Myr after Jupiter’s formation states that Jupiter formed much further out than present distance and then migrated in. There’s no mention of Jupiter migrating further inwards and then back out at all. I’m not sure if that hypothesis and grand tack are even compatible, unless I am missing some information. $\endgroup$ – ShroomZed Feb 6 at 16:35
  • $\begingroup$ @ShroomZed I've looked at the original paper covered by the article ("Consequences of planetary migration on the minor bodies of the early solar system"). A quote: "many mechanisms has been proposed in order to explain the low mass of the asteroid belt, such as ... the Grand Tack scenario ... We are not going to explore further this issue since we did not simulate the inner part of the solar system ..." I'm investigating further - the papers it cites seem to assume that competing torques cause Type 1 inward migration to cease, and say nothing about outward, but 1/ $\endgroup$ – Astrid_Redfern Apr 3 at 11:38
  • $\begingroup$ this may be based on simplifying assumptions, and it may be possible to add in something similar to the Grand Tack in a reasonable modified model. As I say, I'm reading further, and I'm wondering how hot Jupiters/Chthonian planets fit into this. Apologies for not replying sooner, and thanks for bringing it to my attention. $\endgroup$ – Astrid_Redfern Apr 3 at 11:39

I think this question might trigger more an open-ended discussion, than a definitive answer, but let me try my take on it.


Is it more likely that one of these collided with Jupiter itself at the head-on angle needed for the core-warping collision?

In order to collide, a co-orbital configuration is more favourable than a orbit-crossing encounter at high eccentricity (as seen in Liu et al., extended fig. 2), but their 'high angles' don't quantify high eccentricities properly. This is because in their simulations, all planetesimals are initialized at circular orbits, with initial distances of 5-10 mutual Hill-radii (their k parameter). Why I think they didn't properly compare apples with apples, is because usually an eccentric planet would have more kinetic energy than allowed in their simulations, reducing the collision cross-section.
This would lead to drastically reduced impact rates at high angles, compared to the data they show. Furthermore in the early scattering scenario that you propose, most planetesimals would be of too low mass to trigger the core mixing.

The mass required for the impactors is, I think, the major point why the two scenarios are not compatible. The initial conditions for the impact scenarios are those of 5 densely packed 10 $m_{\rm oplus}$ planets, of which one undergoes runaway gas accretion and becomes Jupiter. Those conditions are explained to arise due to oligarchic growth. For the 5 planets, this means that 50 $m_{\rm \oplus}$ are packed in a region of 5 AU size. This is already 1/3 of a median class 0 disc mass, and it necessitates a 100% high efficiency when translating pebbles to planetesimals to planets.
Seeing those numbers lets me strongly doubt the realism of the initial conditions.

Concerning the other part of your question,

The few million years" timescale is quite vague. Does anyone know any additional detail which might suggest the impact occurred prior to the Grand Tack's timeframe?

The few-million years are coming from a certain amount of cooling and compactification that is required for the impact to successfully mix Jupiter's envelope. Hence, the impact should not have occurred prior to the Grand Tack.

Taken both those things together, the cooling requirement and the mass/compactness of the initial conditions necessary, I don't think both scenarios are compatible.

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    $\begingroup$ @Astrid_Redfern: I would say (1) of your first comment and (1) of the second go hand-in-hand, and then the entropy and mass arguments are two separate points. Sorry If my writing wasn't clearn enough on that. Overly simplified assumptions, do you mean whether one could take more realistic initial conditions for the impact model to make it happen? I am sure that this would be subject of current research. However, while resonant chains of equal mass, which destabilize after gas disc dispersal, do happen in planet formation models, this amount of solid mass is at the upper limit that you ca build $\endgroup$ – AtmosphericPrisonEscape Apr 6 at 22:48
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    $\begingroup$ and to selectively only make one of the equal-mass resonant chain planets into a gas giants is also strange. I think, the more realistic you go, the harder it gets to hit Jupiter in a repeatable way, such that the occurrence for this event is something sensible like 50% and not incredibly unlikely. Reality might be stochastic, but a certain school of us would still like solar system formation models to produce high probabilities for the scenarios we envision. $\endgroup$ – AtmosphericPrisonEscape Apr 6 at 22:52
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    $\begingroup$ Another comment is on the necessity of the Grand Tack scenario itself, which was devised initially as a physically self-consistent way to create a planetesimal ring between 0.7 and 1.0-1.5 AU (as earlier work showed that you need this ring to build small Mercury, small Mars and a low-mass planetesimal belt with excited e and i.) Newer work points in the direction that a Grand Tack might not be necessary, and that a one-directional migration with pebble accretion (such as the paper by Pirani et al., that you've cited) can lead to the desired solar system. $\endgroup$ – AtmosphericPrisonEscape Apr 6 at 22:56
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    $\begingroup$ None of the models works without grave problems (some outlined above), that's why none of them is accepted. Furthermore, combining those two scenarios seems to difficult, as the simulation outcome of the GT precludes the initial conditions necessary for the core-impact scenario. Another explanation for Jupiter's diffuse core is core erosion (Militzer et al. 2011), as silicate rock becomes thermodynamically unstable in H/He gas under high pressure and dissolves into the gas. All those scenarios are individual puzzle pieces, no finished puzzle exists yet. $\endgroup$ – AtmosphericPrisonEscape Apr 9 at 13:52
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    $\begingroup$ @Astrid_Redfern: Sorry, i seem to have mixed up the year. ui.adsabs.harvard.edu/abs/2012ApJ...745...54W/abstract in 2012 for erosion of high-pressure water ice, ui.adsabs.harvard.edu/abs/2012PhRvL.108k1101W/abstract for MgO, ui.adsabs.harvard.edu/abs/2014ApJ...787...79G/abstract for SiO2. Applying those to planetary evolution models, would be another batch of papers though. $\endgroup$ – AtmosphericPrisonEscape Apr 17 at 14:48

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