This revision is a significant contribution to our current understanding of planetary formation, suggesting that the mechanisms may be more varied than we think, even between planets of the same type, located in the same neighbourhood - rocky planets, such as Mars and Earth.
You see, we're not really 100 percent sure about how planets form. Astronomers have a pretty good general idea, but the finer details … well, they're rather hard to observe in action.
The broad strokes of planetary formation process are bound up in stellar formation itself. Stars form when a clump in a cloud of dust and gas collapses in on itself under its own gravity, and starts spinning. This causes the surrounding dust and gas to start swirling around it, like water swirling around a drain.
As it swirls, all that material forms a flat disc, feeding into the growing star. But not all the disc will get slurped up - what remains is called the protoplanetary disc, and it goes on to form the planets; that's why all the Solar System planets are roughly aligned on a flat plane around the Sun.
When it comes to planetary formation, it's thought that tiny bits of dust and rock in the disc will start to electrostatically cling together. Then, as they grow in size, so too does their gravitational strength. They start to attract other clumps, through chance interactions and collisions, gaining in size until they're a whole dang planet.
For Earth, this process was thought to have taken tens of millions of years. But the iron isotopes in Earth's mantle, according to scientists from the University of Copenhagen in Denmark, suggest otherwise.
In its composition, Earth appears to be unlike other Solar System bodies. Earth, the Moon, Mars, meteorites - all contain naturally occurring isotopes of iron, such as Fe-56 and the lighter Fe-54. But the Moon, Mars and most meteorites all have similar abundances, while Earth has significantly less Fe-54.
The only other rock that has a similar composition to Earth's is a rare type of meteorite called CI chondrites. The interesting thing about these meteorites is that they have a similar composition to the Solar System as a whole.
Imagine if you were to get all the ingredients for a bolognese. Mix them all together in one big pot - that's the protoplanetary disc, and later the Solar System. But if you scattered your ingredients into a bunch of smaller pots, with different proportions of each ingredient - now you have the individual planets and asteroids.
What makes CI chondrites special is that in this analogy, they are like teeny tiny pots containing the initial proportions of ingredients for a full bolognese. So, having one of these space rocks on hand is like having a microcosm of the dust that swirled around in the protoplanetary disc at the dawn of the Solar System, 4.6 billion years ago.
According to current planetary formation models, if things just smooshed together, the iron abundances in Earth's mantle would be representative of a mix of all different kinds of meteorites, with higher abundances of Fe-54.
The fact that our planet's composition is only comparable to CI dust suggests a different formation model. Instead of rocks banging together, the researchers believe that Earth's iron core formed early through a rain of cosmic dust - a faster process than the accretion of larger rocks. During this time, the iron core formed, slurping up the early iron.
Then, as the Solar System cooled, after its first few hundred thousand years, CI dust from farther out was able to migrate inwards, to where Earth was forming. It sprinkled all over Earth, basically overwriting whatever iron was in the mantle.