<p>It depends what you mean by &quot;form&quot;. The planets all <em>began</em> their formation at more-or-less the same time in the first few hundred thousand years after the protosolar cloud contracted. But they <em>ended</em> their formation process at different times.</p>
<p>Solids and planetesimals begun to condense within a few hundred thousand years and the first planetary-sized bodies (say Moon-sized and above) likely formed within 1-3 million years in most parts of the protosolar system. In the inner Solar System where the density of solids was higher, it is possible that the timescales for the accumulation of these solid protoplanetary bodies would lengthen moving outward to lower density regions. However, <a href="https://www.sciencedirect.com/science/article/pii/S0012821X21004660?casa_token=fcfCDMhEgeEAAAAA:KklXuS8IZRHoeyq4HNxTALoUaC52sI_U1D7Lzjp7lmcRDZvzhainz8ODpYXmFgWvHQWBEMs" rel="nofollow noreferrer">Spitzer &amp; Kleine (2021)</a> show, using various radiometric dating techniques, that ancient meteoritic bodies, whose isotopic composition indicates they formed at different radii in the protoplanetary disk, nevertheless <em>began</em> their formation within a million years or so of each other.</p>
<p>These protoplaneta and planetesimals are not the fully-formed planets we see today. The inner Solar System likely endured 10-100 million years of turmoil and collisions before settling into the 4-planet arrangement we see now. Our own Moon is evidence of one of these titanic collisions.</p>
<p>Current models for the formation of Jupiter suggest it fully-formed in about 5-10 million years because the accretion of its gas envelope onto a rocky/icy core (once it had accumulated) would have been very rapid. I think it is fair to say &quot;Jupiter formed first&quot; in the sense of arriving at close to its final state earliest (a view shared by <a href="https://www.pnas.org/content/114/26/6712" rel="nofollow noreferrer">Kruijer et al. 2017</a> on the basis of meteoritic dating as well as the results of hydrodynamic models). Saturn would have been a little slower because its core would have formed later than Jupiter's and the gas density would be lower further out.</p>
<p>The ice giants may also have been fully formed after about 10-20 million years too, but in the sense that their slower growth may have been truncated by the dispersal of the protoplanetary gas disk at that time. In fact it is unlikely that Uranus and Neptune formed where they are found because the growth rate prior to disk removal would have been too slow.</p>
<p>It is fair to say that a lot of the details of this picture are still being worked out. A massive uncertainty, in my opinion, is how long the protoplanetary disk survived and whether and at what rate it cleared from the inside outwards. This timescale is essentially the timescale for the formation of the giant planets (although Jupiter may have been large enough to essentially accrete all the gas it could <em>prior</em> to disk dispersal). It also sounds the starting gun for the period of chaotic rearrangement and collisions in the inner Solar System, because prior to gas removal the drag would have kept the planetesimals in well-behaved orbits.</p>

CC BY-SA 4.0
2022-01-24T09:44:12.570Z
This begs the question: how do we establish all this? Computer models?
Ng Ph
CC BY-SA 4.0
2022-01-24T11:01:07.603Z
@NgPh That is a massively broad question. The timing of various events, particularly the assembly of planetesimals is established from radionuclide dating. Gas giant growth is worked out in computer simulations and is somewhat uncertain. Evidence of a chaotic growth period is many and varied - e.g. the Moon. Evidence of migration comes from the distribution of various minor bodies in the Solar System, the distribution of water etc.
ProfRob
CC BY-SA 4.0
2022-01-24T13:41:42.240Z
I think the survival of the protoplanetary disc in the solar system case is a better known quantity: If one accepts a planetesimal formation scenario that requires gas to act, then the duration of active planetesimal formation gives the duration of gas survival. And that time is fairly well-known to be ~3 Myrs for the solar case from chondrule data. I would argue that the large uncertainties are in the gas giant formation models, some barely make it in 10 Myrs, some are comfortably done after 0.1 Myrs.
AtmosphericPrisonEscape
CC BY-SA 4.0
2022-01-24T14:06:21.983Z
@AtmosphericPrisonEscape Planetesimal formation occurs WELL before the disk disappears. 3Myr may be  a lower limit. The lifetime of the solar disk is very uncertain and the uncertainty grows with radius. The difference between 0.1 and 10 Myr is a bimodal thing depending on whether one accepts core accretion or thermal instability models. i.e Nobody thinks it is 1 million years for example.
ProfRob
CC BY-SA 4.0
2022-01-24T14:22:58.160Z
I think it is also true that different radionuclides yield different values for the spread in meteorite/chondrule ages and formation times - maybe anything from 2-5+ Myr.
ProfRob
CC BY-SA 4.0
2022-01-24T14:23:06.813Z
Meteoritic dating of chondrules indicates continuous formation of planetesimals during the first $t_{26Al}+3Myrs$, quite possibly at different radii in the disc and with later mixing, yes, but it is wrong to say that PLT form all well before disc dispersal. We furthermore know next to nothing about $dN/dt$ during that time, as meteoritics is still sparse. Lichtenberg (2021, Nature) give a nice overview of the data and their scenario. I was not quoting core-accretion vs. disc instability, but core-accretion numbers. Movshovits 2010 and Mordasini 2012-14 show large variability with dust growth.
AtmosphericPrisonEscape
CC BY-SA 4.0
2022-01-24T14:33:33.777Z
Beyond that, there is discrepancy in 3-D hydrodynamic growth models (shorter than 1-D quasistatic). 
There are furthermore scenarios (i wouldn't call them 'evidence') that if the isotopic separation of asteroids-proxied-by-meteors happened via Jupiter's growth, as some believe (e.g. Desch 2017) then this must have happened <0.1 Myrs.
AtmosphericPrisonEscape
CC BY-SA 4.0
2022-01-24T15:06:53.690Z
@ProfRob, specifically then how did we come to the consensus that *"The planets all began their formation at more-or-less the same time in the first few hundred thousand years after the protosolar cloud contracted."*. This looks extremely precise as a conclusion.
Ng Ph
CC BY-SA 4.0
2022-01-24T15:32:40.070Z
@NgPh one uses radio-nucleid dating and composition on isotopic basis. This allows to characterize ages with an accuracy of down to absolute values of 1M years for events dating back to solar system formation (thus 4.567Gyr ago), and partially even better accuracity for their relative age.
planetmaker
CC BY-SA 4.0
2022-01-24T17:04:20.600Z
@NgPh All the (assumed to be primeval) solids (meteorites, carbonaceous chondrules) in the Solar System have absolute ages that are within 2-3 million years of each other. Within the same solid bodies there is a very limited range of relative ages that indicate they individually formed very fast (much less than a million years). If you have astronomy questions (and these seem to be quite good ones) then ask some formal questions on Astronomy SE.
ProfRob
CC BY-SA 4.0
2022-01-24T18:33:27.127Z
@ProfRob (+planetmaker), I am contemplating this avenue. It's magic to me how you, scientifically, infer (a) the age of rocks w/o a few samples of them, (b) With a few samples, that they are representative of that (rocky) planet, (c) With a representative sample, the precise time they merged together (my baker can make fresh bread with this year's flower as well as last year's). Pardon my shortcomings in Astronomy knowledge... but "The planets **all** began their formation ..." seems quite a scientific certainty which could be backed by a link, perhaps (just to probe further by oneself)?
Ng Ph
CC BY-SA 4.0
2022-01-24T19:02:25.743Z
@NgPh Planets begin as rocks. All the old rocks we can find have a similar age. Yes you can hypothesise that (for some reason) what lies at the centre of Jupiter (for instance) has a radically different age, but why would you? Science doesn't prove anything. We haven't found any proof that different parts of the solar system began forming solids at different times (within the resolution of available measuring techniques). In your example the bread-making process *began* last year. The difference is that the planetesimal timescale for formation takes minutes on a proportionate timeline.
ProfRob
CC BY-SA 4.0
2022-01-24T19:04:56.513Z
@NgPh there is no evidence that "this year's flour" even exists. If you have further questions then ask them as a question.
ProfRob
CC BY-SA 4.0
2022-01-24T20:56:14.623Z
@ProfRob, I will, when I am less afraid of getting mockeries in return for my ignorance. Thanks for adding some references. I have just opened Kruijer's paper, and the first sentence of the abstract is "The age of Jupiter, ..., is still unknown" . Understood that "a first few hundred thousand years" is very short compared to the age of the Solar system. I will peruse the paper to see what I have missed. No more question!
Ng Ph
CC BY-SA 4.0
2022-01-25T06:48:15.130Z
@ProfRob Nice answer :)
Kavin Ishwaran
CC BY-SA 4.0
2022-01-24T08:51:16.730Z
2022-01-25T06:42:06.273Z
2022-01-25T06:42:06.273Z
ProfRob
<p>The old theory about the formation of the planets was that they were torn from the Sun by a chance passing star and condensed into solid bodies.</p>
<p>It was also believed that the planets solidified from lava into solid rock faster the farther they were from the heat of the Sun.  Thus the outermost planet would be the oldest and the innermost planet the youngest.</p>
<p>But that theory of planet formation has been obsolete for about 70 years.</p>
<p>The present theory is that the planets formed out of a disc of gas and dust left over from the formation of the Sun.  Motes of dust that collided at slow enough speeds clumped together to form larger dustballs.  Eventually pebble sized objects were formed, and boulder sized objects, and ever larger objects.  Eventually there were countless thousands and millions of plenetesimals which gradually clumped together to form larger masses.  And some of those masses eventually had high enough escape velocities to capture and hold gas molecules.</p>
<p>And there are many theories about that process and how it operated.  So possibly some theories might claim that some of the present planets began forming and/or completed forming earlier than other planets.  But the formation periods of all of the planets probably had a high degree of overlap.</p>

CC BY-SA 4.0
2022-01-24T17:44:17.220Z
2022-01-24T17:44:17.220Z
M. A. Golding
<p>As a supplement to the other fine answers already posted, I'd like to post an image of the disk surrounding the star HL Tauri, created in 2014 using ALMA, the Atacama Large Millimeter Array in Chile.</p>
<p><a href="https://i.sstatic.net/0nWLW.jpg" rel="noreferrer"><img src="https://i.sstatic.net/0nWLW.jpg" alt="enter image description here" /></a></p>
<p>Credit:
ALMA (ESO/NAOJ/NRAO)</p>
<p>From the <a href="https://www.eso.org/public/usa/news/eso1436/" rel="noreferrer">press release</a>, Stuartt Corder, ALMA Deputy Director said:</p>
<blockquote>
<p>These features are almost certainly the result of young planet-like
bodies that are being formed in the disc. This is surprising since
such young stars are not expected to have large planetary bodies
capable of producing the structures we see in this image.</p>
</blockquote>
<p>While this certainly isn't proof that all the planets in our Solar System developed around the same time, this image certainly lends support to the earlier models of near-simultaneous planet formation from a protoplanetary disk.</p>
<p>As the quality of our telescopes improve, so do the quality of our observations.  When the prevailing model is supported by direct observation, it gains credence from the community. I am greatly looking forward to JWST observations of protoplanetary disks.  Perhaps we will be able to see the material in-fall in to the planets, or the planets themselves.</p>

CC BY-SA 4.0
2022-01-24T20:30:21.433Z
I thought the idea that these rings were caused by planets had been debunked but apparently it is still a live issue. The problem is that the HL Tau disk is really young (< 1 million years) and fully fledged planets appear not to have formed so quickly in our Solar System. Note also that the disk is much bigger than the solar system.
ProfRob
CC BY-SA 4.0
2022-01-25T06:48:58.803Z
Useful Supplement !
Kavin Ishwaran
CC BY-SA 4.0
2022-01-25T13:25:36.120Z
In Nesvorny's [Young Solar system ...](https://arxiv.org/abs/1109.2949), page 2, it can be read *"The solar system, with the widely spaced and nearly circular orbits of the giant planets, bears little resemblance to the bulk of known exoplanets"*. So, while the image could lend support to the near-simultaneous formation model, not only it is not proof that the Solar system follows the same, it's insufficient to prove the predominance of the model (elsewhere). Anyway, it's an interesting piece of the puzzle.
Ng Ph
CC BY-SA 4.0
2022-01-24T19:23:54.363Z
2022-01-24T19:23:54.363Z
Connor Garcia
<p>The planets (probably) formed by the accumulation of <a href="https://en.wikipedia.org/wiki/Planetesimal" rel="noreferrer">planetesimals</a>, and they all formed over roughly the same time span. Inner <a href="https://en.wikipedia.org/wiki/Protoplanet" rel="noreferrer">protoplanets</a> had access to more matter, so they probably were able to accumulate that matter faster. On the other hand, a lot of the matter in the Solar System is volatile, so it's more likely to condense in the colder parts of the protoplanetary disk.</p>
<p>Also, gravity favours a &quot;greedy&quot; formation mechanism. A more massive protoplanet will tend to accumulate matter faster than a smaller protoplanet in the same region, due to its stronger gravity.</p>
<p>Most of the matter in the Solar System outside the Sun is in Jupiter, so it's reasonable to assume that Jupiter was an early winner in the matter gathering contest. There are good reasons to believe that Jupiter actually formed closer to the proto-Sun, migrated even closer, and then migrated outwards when it had accumulated a large fraction of its mass.</p>
<p>From <a href="https://en.wikipedia.org/wiki/Grand_tack_hypothesis" rel="noreferrer">Wikipedia</a>,</p>
<blockquote>
<p>the grand tack hypothesis proposes that Jupiter formed at 3.5 AU, then migrated inward to 1.5 AU, before reversing course due to capturing Saturn in an orbital resonance, eventually halting near its current orbit at 5.2 AU.</p>
</blockquote>
<p>It's hard to know the details of the formation of our planetary system. Fortunately, we now have a lot of data about other planetary systems, including some young systems that are still in the early stages of formation, and that data helps us refine our general theories of planetary system formation, as well as theories about the formation of our system. However, a lot of that data is fairly crude, and it's biased because it's a lot easier to detect large exoplanets close to their star than small distant ones.</p>
<p>We can use computers to test theories of Solar System formation. You set up a mathematical model with a bunch of planetesimals, dust, and gas orbiting the proto-Sun, and then crunch the numbers to see if it evolves into something resembling the real Solar System. If it does, your model <em>might</em> be correct. If it doesn't, you adjust the parameters and try again. This process consumes a lot of computing power, since you need to make accurate gravitational calculations involving hundreds and thousands of objects. So the people doing this research generally run their models many times, looking for solid trends, and to help them weed out effects that are due to errors caused by the modeling calculations.</p>
<p>These studies have found that it's quite likely that a lot of planetesimals were ejected into the outer Solar System, or even out of the Solar System's gravitational well and into interstellar space. And of course a lot got thrown into the Sun.</p>
<p>One current theory of late system formation is known as the <a href="https://en.wikipedia.org/wiki/Nice_model" rel="noreferrer">Nice model</a>, originally published in 2005. However, as that article mentions, more recent research indicates that the Nice model needs some adjustments.</p>
<p>A study from 2011 claims that there's a high probability that our system originally had 5 giants, but one of them got thrown out of the system.</p>
<p><a href="https://arxiv.org/abs/1109.2949" rel="noreferrer">Young Solar System's Fifth Giant Planet?</a>, by David Nesvorny.</p>
<h4>Abstract</h4>
<blockquote>
<p>Recent studies of solar system formation suggest that the solar system's giant planets formed and migrated in the protoplanetary disk to reach resonant orbits with all planets inside 15 AU from the Sun. After the gas disk's dispersal, Uranus and Neptune were likely scattered by gas giants, and approached their current orbits while dispersing the transplanetary disk of planetesimals, whose remains survived to this time in the region known as the Kuiper belt.</p>
<p>Here we performed N-body integrations of the scattering phase between giant planets in an attempt to determine which initial states are plausible. We found that the dynamical simulations starting with a resonant system of four giant planets have a low success rate in matching the present orbits of giant planets, and various other constraints (e.g., survival of the terrestrial planets). The dynamical evolution is typically too violent, if Jupiter and Saturn start in the 3:2 resonance, and leads to final systems with fewer than four planets.</p>
<p>Several initial states stand out in that they show a relatively large likelihood of success in matching the constraints. Some of the statistically best results were obtained when assuming that the solar system initially had five giant planets and one ice giant, with the mass comparable to that of Uranus and Neptune, was ejected to interstellar space by Jupiter. This possibility appears to be conceivable in view of the recent discovery of a large number free-floating planets in interstellar space, which indicates that planet ejection should be common.</p>
</blockquote>

CC BY-SA 4.0
2022-01-25T16:53:34.033Z
Comments are not for extended discussion; this conversation has been [moved to chat](https://chat.stackexchange.com/rooms/133505/discussion-on-answer-by-pm-2ring-which-planet-came-first-in-our-solar-system).
Connor Garcia
CC BY-SA 4.0
2022-01-24T08:11:53.583Z
2022-01-24T15:16:53.947Z
2022-01-24T15:16:53.947Z
PM 2Ring
<p>I always wonder which planet came first in our solar system? Sources suggest that Jupiter might be the first planet in our solar system, but how did our solar system evolve into an 8 planet system?</p>

CC BY-SA 4.0
2022-01-24T08:02:18.893Z
If you have sources, you might want to cite or reference them. All planets form concurrently.
planetmaker
CC BY-SA 4.0
2022-01-25T05:44:11.043Z
You can have a look at this WP article: https://en.wikipedia.org/wiki/Formation_and_evolution_of_the_Solar_System
Nilay Ghosh
<solar-system><solar-system-evolution>
Which planet came first in our Solar system?
Kavin Ishwaran
# Which planet came first in our Solar system?

(Asked by: username_0 on 2022-01-24)

I always wonder which planet came first in our solar system? Sources suggest that Jupiter might be the first planet in our solar system, but how did our solar system evolve into an 8 planet system?

**Tags:** solar-system, solar-system-evolution

> **Comments:**
> **username_1**: If you have sources, you might want to cite or reference them. All planets form concurrently.  
> **username_2**: You can have a look at this WP article: https://en.wikipedia.org/wiki/Formation_and_evolution_of_the_Solar_System  

---

## 4 answers

### Answer by username_8 on 2022-01-24. Score: 36 | Accepted answer

The planets (probably) formed by the accumulation of [planetesimals](https://en.wikipedia.org/wiki/Planetesimal), and they all formed over roughly the same time span. Inner [protoplanets](https://en.wikipedia.org/wiki/Protoplanet) had access to more matter, so they probably were able to accumulate that matter faster. On the other hand, a lot of the matter in the Solar System is volatile, so it's more likely to condense in the colder parts of the protoplanetary disk.

Also, gravity favours a "greedy" formation mechanism. A more massive protoplanet will tend to accumulate matter faster than a smaller protoplanet in the same region, due to its stronger gravity.

Most of the matter in the Solar System outside the Sun is in Jupiter, so it's reasonable to assume that Jupiter was an early winner in the matter gathering contest. There are good reasons to believe that Jupiter actually formed closer to the proto-Sun, migrated even closer, and then migrated outwards when it had accumulated a large fraction of its mass.

From [Wikipedia](https://en.wikipedia.org/wiki/Grand_tack_hypothesis),

> the grand tack hypothesis proposes that Jupiter formed at 3.5 AU, then migrated inward to 1.5 AU, before reversing course due to capturing Saturn in an orbital resonance, eventually halting near its current orbit at 5.2 AU.

It's hard to know the details of the formation of our planetary system. Fortunately, we now have a lot of data about other planetary systems, including some young systems that are still in the early stages of formation, and that data helps us refine our general theories of planetary system formation, as well as theories about the formation of our system. However, a lot of that data is fairly crude, and it's biased because it's a lot easier to detect large exoplanets close to their star than small distant ones.

We can use computers to test theories of Solar System formation. You set up a mathematical model with a bunch of planetesimals, dust, and gas orbiting the proto-Sun, and then crunch the numbers to see if it evolves into something resembling the real Solar System. If it does, your model *might* be correct. If it doesn't, you adjust the parameters and try again. This process consumes a lot of computing power, since you need to make accurate gravitational calculations involving hundreds and thousands of objects. So the people doing this research generally run their models many times, looking for solid trends, and to help them weed out effects that are due to errors caused by the modeling calculations.

These studies have found that it's quite likely that a lot of planetesimals were ejected into the outer Solar System, or even out of the Solar System's gravitational well and into interstellar space. And of course a lot got thrown into the Sun.

One current theory of late system formation is known as the [Nice model](https://en.wikipedia.org/wiki/Nice_model), originally published in 2005. However, as that article mentions, more recent research indicates that the Nice model needs some adjustments.

A study from 2011 claims that there's a high probability that our system originally had 5 giants, but one of them got thrown out of the system.

[Young Solar System's Fifth Giant Planet?](https://arxiv.org/abs/1109.2949), by David Nesvorny.

#### Abstract

> Recent studies of solar system formation suggest that the solar system's giant planets formed and migrated in the protoplanetary disk to reach resonant orbits with all planets inside 15 AU from the Sun. After the gas disk's dispersal, Uranus and Neptune were likely scattered by gas giants, and approached their current orbits while dispersing the transplanetary disk of planetesimals, whose remains survived to this time in the region known as the Kuiper belt.
>
> Here we performed N-body integrations of the scattering phase between giant planets in an attempt to determine which initial states are plausible. We found that the dynamical simulations starting with a resonant system of four giant planets have a low success rate in matching the present orbits of giant planets, and various other constraints (e.g., survival of the terrestrial planets). The dynamical evolution is typically too violent, if Jupiter and Saturn start in the 3:2 resonance, and leads to final systems with fewer than four planets.
>
> Several initial states stand out in that they show a relatively large likelihood of success in matching the constraints. Some of the statistically best results were obtained when assuming that the solar system initially had five giant planets and one ice giant, with the mass comparable to that of Uranus and Neptune, was ejected to interstellar space by Jupiter. This possibility appears to be conceivable in view of the recent discovery of a large number free-floating planets in interstellar space, which indicates that planet ejection should be common.

> **Comments:**
> **username_7**: Comments are not for extended discussion; this conversation has been [moved to chat](https://chat.stackexchange.com/rooms/133505/discussion-on-answer-by-pm-2ring-which-planet-came-first-in-our-solar-system).  

---

### Answer by username_3 on 2022-01-24. Score: 14

It depends what you mean by "form". The planets all *began* their formation at more-or-less the same time in the first few hundred thousand years after the protosolar cloud contracted. But they *ended* their formation process at different times.

Solids and planetesimals begun to condense within a few hundred thousand years and the first planetary-sized bodies (say Moon-sized and above) likely formed within 1-3 million years in most parts of the protosolar system. In the inner Solar System where the density of solids was higher, it is possible that the timescales for the accumulation of these solid protoplanetary bodies would lengthen moving outward to lower density regions. However, [Spitzer & Kleine (2021)](https://www.sciencedirect.com/science/article/pii/S0012821X21004660?casa_token=fcfCDMhEgeEAAAAA:KklXuS8IZRHoeyq4HNxTALoUaC52sI_U1D7Lzjp7lmcRDZvzhainz8ODpYXmFgWvHQWBEMs) show, using various radiometric dating techniques, that ancient meteoritic bodies, whose isotopic composition indicates they formed at different radii in the protoplanetary disk, nevertheless *began* their formation within a million years or so of each other.

These protoplaneta and planetesimals are not the fully-formed planets we see today. The inner Solar System likely endured 10-100 million years of turmoil and collisions before settling into the 4-planet arrangement we see now. Our own Moon is evidence of one of these titanic collisions.

Current models for the formation of Jupiter suggest it fully-formed in about 5-10 million years because the accretion of its gas envelope onto a rocky/icy core (once it had accumulated) would have been very rapid. I think it is fair to say "Jupiter formed first" in the sense of arriving at close to its final state earliest (a view shared by [Kruijer et al. 2017](https://www.pnas.org/content/114/26/6712) on the basis of meteoritic dating as well as the results of hydrodynamic models). Saturn would have been a little slower because its core would have formed later than Jupiter's and the gas density would be lower further out.

The ice giants may also have been fully formed after about 10-20 million years too, but in the sense that their slower growth may have been truncated by the dispersal of the protoplanetary gas disk at that time. In fact it is unlikely that Uranus and Neptune formed where they are found because the growth rate prior to disk removal would have been too slow.

It is fair to say that a lot of the details of this picture are still being worked out. A massive uncertainty, in my opinion, is how long the protoplanetary disk survived and whether and at what rate it cleared from the inside outwards. This timescale is essentially the timescale for the formation of the giant planets (although Jupiter may have been large enough to essentially accrete all the gas it could *prior* to disk dispersal). It also sounds the starting gun for the period of chaotic rearrangement and collisions in the inner Solar System, because prior to gas removal the drag would have kept the planetesimals in well-behaved orbits.

> **Comments:**
> **username_4**: This begs the question: how do we establish all this? Computer models?  
> **username_3**: @NgPh That is a massively broad question. The timing of various events, particularly the assembly of planetesimals is established from radionuclide dating. Gas giant growth is worked out in computer simulations and is somewhat uncertain. Evidence of a chaotic growth period is many and varied - e.g. the Moon. Evidence of migration comes from the distribution of various minor bodies in the Solar System, the distribution of water etc.  
> **username_5**: I think the survival of the protoplanetary disc in the solar system case is a better known quantity: If one accepts a planetesimal formation scenario that requires gas to act, then the duration of active planetesimal formation gives the duration of gas survival. And that time is fairly well-known to be ~3 Myrs for the solar case from chondrule data. I would argue that the large uncertainties are in the gas giant formation models, some barely make it in 10 Myrs, some are comfortably done after 0.1 Myrs.  
> **username_3**: @username_5 Planetesimal formation occurs WELL before the disk disappears. 3Myr may be  a lower limit. The lifetime of the solar disk is very uncertain and the uncertainty grows with radius. The difference between 0.1 and 10 Myr is a bimodal thing depending on whether one accepts core accretion or thermal instability models. i.e Nobody thinks it is 1 million years for example.  
> **username_3**: I think it is also true that different radionuclides yield different values for the spread in meteorite/chondrule ages and formation times - maybe anything from 2-5+ Myr.  
> **username_5**: Meteoritic dating of chondrules indicates continuous formation of planetesimals during the first $t_{26Al}+3Myrs$, quite possibly at different radii in the disc and with later mixing, yes, but it is wrong to say that PLT form all well before disc dispersal. We furthermore know next to nothing about $dN/dt$ during that time, as meteoritics is still sparse. Lichtenberg (2021, Nature) give a nice overview of the data and their scenario. I was not quoting core-accretion vs. disc instability, but core-accretion numbers. Movshovits 2010 and Mordasini 2012-14 show large variability with dust growth.  
> **username_5**: Beyond that, there is discrepancy in 3-D hydrodynamic growth models (shorter than 1-D quasistatic).  There are furthermore scenarios (i wouldn't call them 'evidence') that if the isotopic separation of asteroids-proxied-by-meteors happened via Jupiter's growth, as some believe (e.g. Desch 2017) then this must have happened <0.1 Myrs.  
> **username_4**: @username_3, specifically then how did we come to the consensus that *"The planets all began their formation at more-or-less the same time in the first few hundred thousand years after the protosolar cloud contracted."*. This looks extremely precise as a conclusion.  
> **username_1**: @NgPh one uses radio-nucleid dating and composition on isotopic basis. This allows to characterize ages with an accuracy of down to absolute values of 1M years for events dating back to solar system formation (thus 4.567Gyr ago), and partially even better accuracity for their relative age.  
> **username_3**: @NgPh All the (assumed to be primeval) solids (meteorites, carbonaceous chondrules) in the Solar System have absolute ages that are within 2-3 million years of each other. Within the same solid bodies there is a very limited range of relative ages that indicate they individually formed very fast (much less than a million years). If you have astronomy questions (and these seem to be quite good ones) then ask some formal questions on Astronomy SE.  
> **username_4**: @username_3 (+username_1), I am contemplating this avenue. It's magic to me how you, scientifically, infer (a) the age of rocks w/o a few samples of them, (b) With a few samples, that they are representative of that (rocky) planet, (c) With a representative sample, the precise time they merged together (my baker can make fresh bread with this year's flower as well as last year's). Pardon my shortcomings in Astronomy knowledge... but "The planets **all** began their formation ..." seems quite a scientific certainty which could be backed by a link, perhaps (just to probe further by oneself)?  
> **username_3**: @NgPh Planets begin as rocks. All the old rocks we can find have a similar age. Yes you can hypothesise that (for some reason) what lies at the centre of Jupiter (for instance) has a radically different age, but why would you? Science doesn't prove anything. We haven't found any proof that different parts of the solar system began forming solids at different times (within the resolution of available measuring techniques). In your example the bread-making process *began* last year. The difference is that the planetesimal timescale for formation takes minutes on a proportionate timeline.  
> **username_3**: @NgPh there is no evidence that "this year's flour" even exists. If you have further questions then ask them as a question.  
> **username_4**: @username_3, I will, when I am less afraid of getting mockeries in return for my ignorance. Thanks for adding some references. I have just opened Kruijer's paper, and the first sentence of the abstract is "The age of Jupiter, ..., is still unknown" . Understood that "a first few hundred thousand years" is very short compared to the age of the Solar system. I will peruse the paper to see what I have missed. No more question!  
> **username_0**: @username_3 Nice answer :)  

---

### Answer by username_7 on 2022-01-24. Score: 8

As a supplement to the other fine answers already posted, I'd like to post an image of the disk surrounding the star HL Tauri, created in 2014 using ALMA, the Atacama Large Millimeter Array in Chile.

[![enter image description here](https://i.sstatic.net/0nWLW.jpg)](https://i.sstatic.net/0nWLW.jpg)

Credit:
ALMA (ESO/NAOJ/NRAO)

From the [press release](https://www.eso.org/public/usa/news/eso1436/), Stuartt Corder, ALMA Deputy Director said:

> These features are almost certainly the result of young planet-like
> bodies that are being formed in the disc. This is surprising since
> such young stars are not expected to have large planetary bodies
> capable of producing the structures we see in this image.

While this certainly isn't proof that all the planets in our Solar System developed around the same time, this image certainly lends support to the earlier models of near-simultaneous planet formation from a protoplanetary disk.

As the quality of our telescopes improve, so do the quality of our observations. When the prevailing model is supported by direct observation, it gains credence from the community. I am greatly looking forward to JWST observations of protoplanetary disks. Perhaps we will be able to see the material in-fall in to the planets, or the planets themselves.

> **Comments:**
> **username_3**: I thought the idea that these rings were caused by planets had been debunked but apparently it is still a live issue. The problem is that the HL Tau disk is really young (< 1 million years) and fully fledged planets appear not to have formed so quickly in our Solar System. Note also that the disk is much bigger than the solar system.  
> **username_0**: Useful Supplement !  
> **username_4**: In Nesvorny's [Young Solar system ...](https://arxiv.org/abs/1109.2949), page 2, it can be read *"The solar system, with the widely spaced and nearly circular orbits of the giant planets, bears little resemblance to the bulk of known exoplanets"*. So, while the image could lend support to the near-simultaneous formation model, not only it is not proof that the Solar system follows the same, it's insufficient to prove the predominance of the model (elsewhere). Anyway, it's an interesting piece of the puzzle.  

---

### Answer by username_6 on 2022-01-24. Score: 6

The old theory about the formation of the planets was that they were torn from the Sun by a chance passing star and condensed into solid bodies.

It was also believed that the planets solidified from lava into solid rock faster the farther they were from the heat of the Sun. Thus the outermost planet would be the oldest and the innermost planet the youngest.

But that theory of planet formation has been obsolete for about 70 years.

The present theory is that the planets formed out of a disc of gas and dust left over from the formation of the Sun. Motes of dust that collided at slow enough speeds clumped together to form larger dustballs. Eventually pebble sized objects were formed, and boulder sized objects, and ever larger objects. Eventually there were countless thousands and millions of plenetesimals which gradually clumped together to form larger masses. And some of those masses eventually had high enough escape velocities to capture and hold gas molecules.

And there are many theories about that process and how it operated. So possibly some theories might claim that some of the present planets began forming and/or completed forming earlier than other planets. But the formation periods of all of the planets probably had a high degree of overlap.


---

