Blog

How did Earth, alone among the Solar System’s rocky planets, become the home for life? How, among all this frigid lifelessness, did our planet become warm, hospitable, and life-sustaining? The answer to these questions is complex and multi-faceted, and part of the answer comes from cosmochemistry, an interdisciplinary field that examines how chemical elements are distributed.

The Solar System is a busy place where everything is in motion. It was even more chaotic 4.5 billion years ago, with planets still forming and planetesimals and planetary embryos whizzing around and crashing into one another. Somehow, in all that chaos, Earth received more than its share of carbonaceous chondrites and the amino acids and other life-enabling chemicals that came with them.

Cosmochemistry studies have shown that between 5% and 10% of Earth’s mass came from carbonaceous chondrites that crashed into the young planet. Studies also show that a large chunk of that came from the Theia impactor that created the Moon. To test these ideas more rigorously, a trio of researchers used dynamical simulations of the Solar System’s formation to see if they could replicate it.

The research is titled “Dynamical origin of Theia, the last giant impactor on Earth.” The lead author is Duarte Branco from the Institute of Astrophysics and Space Sciences at the Lisbon Astronomical Observatory in Portugal. The research will be published in the journal Icarus.

One of the critical distinctions in cosmochemistry is the difference between carbonaceous chondrites (CCs) and non-carbonaceous meteorites (NCs). It divides the Solar System’s meteor population into two groups and suggests that the Solar System contains two distinct reservoirs of material. CCs formed further from the Sun, likely beyond Jupiter, and carry more volatiles like water and organic compounds with them. NCs include things like iron meteorites, and contain fewer volatiles.

In order to test the idea that Theia delivered CCs and volatiles to Earth, the researchers ran detailed simulations of the Solar System. These were N-body simulations of the later stages of the growth of terrestrial planets.

The simulations began in the late stages of planetary growth after the Solar System’s gaseous disk was dispersed. The available solid mass was divided into planetesimals and planetary embryos. The simulation included CCs that were scattered inward as Jupiter and Saturn were still growing and accreting matter. Because of the size distinction between planetesimal and planetary embryos, embryos have a higher possibility of interacting with the terrestrial planets and delivering CC material.

The researchers ran three types of simulations. The first they call small only and includes only small CC objects, or planetesimals. The second they call large only and includes only large CC objects, planetary embryos. The third includes both CC planetesimals and embryos and is called the mixed scenario.

For a subset of 10 simulations from each of those scenarios, they included the effect of the giant planet dynamical instability. This is known as the “Nice model” in astronomy and describes how the giant planets shifted their orbits from where they initially formed.

The goal was to determine how CCs and NCs were distributed in the Solar System and to understand how Earth ended up with more CCs than the other rocky planets, especially Mars. The researchers also wanted to understand if the Theia impact could be responsible for delivering a large amount of Earth’s CC material.

One clear result is that the role of giant planet instability, especially Jupiter’s shift to a different orbit, had a pronounced effect on Earth’s accretion of CC material.

This figure shows snapshots from the mixed simulation scenario without giant planet dynamical instability. In early times, CC objects and NC bodies mix together where the terrestrial planets are forming. Some CCs remained orbiting between planets or were still too far to collide. By the simulation’s end, four terrestrial planets existed, including good analogues for Earth and Mars. Image Credit: Branco et al. 2025. Icarus

When the researchers added giant planet dynamical instability, things looked even more interesting. “The giant planet instability dramatically changed the evolution of the system causing a strong pulse of eccentricity excitement, which lead to a wave of collisions and ejections,” the authors write. However, the final state of the system didn’t change much.

This figure shows eccentricity and position snapshots over the time of the simulation, including giant planet dynamical instability. The final snapshot is the real Solar System. Image Credit: Branco et al. 2025. Icarus

A critical part of the simulations concerns the Theia impactor. Previous research suggests that Theia may have been a carbonaceous object. If that’s true, much of Earth’s life-giving habitability may have resulted from that collision.

“In the mixed scenario with no giant planet instability, Earth’s final impactor included a CC component in more than half of all simulations. In 38.5% of simulations, the final impactor was a pure CC embryo, and in another 13.5%, the impactor was an NC embryo that had previously accreted a CC embryo,” the researchers write.

Overall, the simulations paint a picture of the early Solar System where two distinct rings of planetesimals. An inner ring consisting of rocky planetesimals and an outer ring of carbonaceous chondrites. Later, as the ice giants migrated inward, they propelled CC material into the inner Solar System. Some of these were trapped in the asteroid belt, while more massive ones were preferentially scattered into the orbits of the rocky planets. “The late-stage accretion of the terrestrial planets
involved a series of giant impacts between NC embryos and planetesimals, with occasional impacts of CC objects,” the authors explain.

This scenario explains several things about the Solar System. It explains the masses and orbits of the terrestrial planets, and the orbital distribution of asteroids. It also matches the CC mass fraction of Earth and Mars, where Mars lacks the same concentrations of CC material as Earth. If the small only simulation were correct, where CC material was only in the form of planetesimals, the CC mass fraction of Mars and Earth would be roughly the same.

This figure compares the timing of the last giant impacts in 10 mixed simulations that were run both with and without the giant planet instability. The black line represents the point where both values are equal. Each point has two halves with the left half representing the impactor type in the simulation without the giant planet instability and the right half representing the simulation with the giant planet instability. Dry NC impactors are black, CC embryos are blue and CC+NC mixed embryos are green. Image Credit: Branco et al. 2025. Icarus

The researchers set out to show that, in line with other research, Theia could’ve been Earth’s final large impactor and that it contained ample CC material. They appear to have succeeded.

In the simulations, Earth’s final giant impact was with Theia, and that object had higher concentrations of CC material which helped make Earth habitable. That result is in line with scientific thinking. The work shows that the last impact was after between 5 to 150 million years after gas dispersal. A large fraction of those were within 20 to 70 million years. There are uncertainties in the timing of the Theia impact and these results work within those.

The simulations also support other conclusions showing that CC embryos and planetesimals could’ve been accreted throughout Earth’s growth, but were concentrated in later phases of growth.

“Within the context of this scenario, the last giant impactor on Earth contained a CC component in roughly half of all of the mixed simulations,” the authors write. “In the majority of these (38% of simulations), Theia was a pristine CC embryo, and in the remainder of cases Theia was an NC embryo that had previously accreted a CC embryo.”

The research also shows that Jupiter played an important role in the Solar System’s architecture. It not only truncates the asteroid belt, but played an important role in determining the final composition of the terrestrial planets by scattering CC material from the outer Solar System into the path of the rocky planets, especially Earth.

A million things had to be just right for Earth to become the life-sustaining world it is today. How likely it is that there are other worlds out there like it is unknown. It may take more than being in a habitable zone for an exoplanet to support life. There may be a bewildering number of variables that have to go right, including outer giant planets that migrate and deliver carbon to rocky worlds in habitable zones.

Astronomers have turned the Atacama Large Millimeter/submillimeter Array (ALMA) into a time machine to peer back in cosmic time to 1 billion years after the Big Bang.

This has revealed previously hidden structures within the universe’s first galaxies, which could help us understand how the modern cosmos, including our galaxy, the Milky Way, took shape.

BUFFALO, N.Y. — Look inside a brain cell with Huntington’s disease or ALS and you are likely to find RNA clumped together.

These solid-like clusters, thought to be irreversible, can act as sponges that soak up surrounding proteins key for brain health, contributing to neurological disorders.

How these harmful RNA clusters form in the first place has remained an open question.

Now, University at Buffalo researchers have not only uncovered that tiny droplets of protein and nucleic acids in cells contribute to the formation of RNA clusters but also demonstrated a way to prevent and disassemble the clusters.

Their findings, described in a study published Thursday (July 2) in Nature Chemistry , uses an engineered strand of RNA known as an antisense oligonucleotide that can bind to RNA clusters and disperse them.

“It’s fascinating to watch these clusters form over time inside dense, droplet-like mixtures of protein and RNA under the microscope. Just as striking, the clusters dissolve when antisense oligonucleotides pull the RNA aggregates apart,” says the study’s corresponding author, Priya Banerjee, PhD, associate professor in the Department of Physics, within the UB College of Arts and Sciences. “What’s exciting about this discovery is that we not only figured out how these clusters form but also found a way to break them apart.”

The work was supported by the U.S. National Institutes of Health and the St. Jude Children’s Research Hospital.

How RNA clusters form

The study sheds new light on how RNA clusters form within biomolecular condensates.

Cells make these liquid-like droplets from RNA, DNA and proteins — or a combination of all three. Banerjee’s team has researched them extensively, investigating their role in both cellular function and disease, as well as their fundamental material properties that present new opportunities for synthetic biology applications.

The condensates are essentially used as hosts by repeat RNAs, disease-linked RNA molecules with abnormally long strands of repeated sequences. At an early timepoint, the repeat RNAs remain fully mixed inside these condensates, but as the condensates age, the RNA molecules start clumping together, creating an RNA-rich solid core surrounded by an RNA-depleted fluid shell.

“Repeat RNAs are inherently sticky, but interestingly, they don’t stick to each other just by themselves because they fold into stable 3D structures. They need the right environment to unfold and clump together, and the condensates provide that,” says the study’s first author, Tharun Selvam Mahendran, a PhD student in Banerjee’s lab.

“Crucially, we also found that the solid-like repeat RNA clusters persist even after the host condensate dissolves,” Mahendran adds. “This persistence is partly why the clusters are thought to be irreversible.”

Preventing — and reversing — clusters

The team was first able to demonstrate that repeat RNA clustering can be prevented by using an RNA-binding protein known as G3Bp1 that is present in cells.

“The RNA clusters come about from the RNA strands sticking together, but if you introduce another sticky element into the condensate, like G3BP1, then the interactions between the RNAs are frustrated and clusters stop forming,” Banerjee says. “It’s like introducing a chemical inhibitor into a crystal-growing solution, the ordered structure can no longer form properly. You can think of the G3BP1 as an observant molecular chaperone that binds to the sticky RNA molecules and makes sure that RNAs don’t stick to each other.”

In order to reverse the clusters, the team employed an antisense oligonucleotide (ASO). Because ASO is a short RNA with a sequence complementary to the repeat RNA, it was able to not only bind to the aggregation-prone RNAs but also disassemble the RNA clusters.

The team found that ASO’s disassembly abilities were highly tied to its specific sequence. Scramble the sequence in any way, and the ASO would fail to prevent clustering, let alone disassemble the clusters.

“This suggests our ASO can be tailored to only target specific repeat RNAs, which is a good sign for its viability as a potential therapeutic application,” Banerjee says.

Banerjee is also exploring RNA’s role in the origin of life, thanks to a seed grant from the Hypothesis Fund. He is studying whether biomolecular condensates may have protected RNA’s functions as biomolecular catalysts in the harsh prebiotic world.

“It really just shows how RNAs may have evolved to take these different forms of matter, some of which are extremely useful for biological functions and perhaps even life itself — and others that can bring about disease,” Banerjee says.