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Two colliding planets might merge, glance off one another, strip away material, or break into multiple pieces. The result depends on their relative size, impact speed and angle, composition, and spin. A collision can melt or vaporize rock, change a planet’s atmosphere, and scatter debris into space or orbit. Under the right conditions, orbiting debris can come together to form a moon.

The leading explanation for the Moon’s origin is one such giant impact: a large body struck the young Earth, and debris contributed to the Moon. The impact hypothesis is supported by several lines of evidence, but scientists have not settled the exact sequence of events.

Would the planets merge or break apart?

There is no single outcome for a planetary collision. A collision is not necessarily a clean fusion, and it does not always destroy both bodies. Researchers model several possible outcomes, from gradual accretion to catastrophic disruption. Which one occurs depends on how the bodies meet and what they are made of.

Outcome What happens Typical factors
Accretion or merger One body absorbs much of the other’s material, making the surviving body larger. More likely when the impact lets material remain bound to the larger remnant rather than escape.
Graze-and-merge The bodies meet at an angle, separate briefly, then come together and merge. A grazing angle can still lead to a merger, depending on speed, mass, and the bodies’ structure.
Hit-and-run The bodies collide obliquely and then continue on separate paths, with some material exchanged or stripped away. Possible in grazing encounters, especially when the impact does not capture the smaller body.
Erosion or partial accretion The impact removes material from one or both bodies, while a substantial remnant survives. Relative mass, speed, angle, and composition determine how much material is lost or retained.
Catastrophic disruption The collision fragments a body or bodies; some fragments may escape, while others can later gather into larger remnants. High impact energy can promote fragmentation, but the result also depends on geometry and internal structure.

A 2012 study modeled a range of late-stage planet-formation collisions and found a broad mix of outcomes, including partial accretion, graze-and-merge, and hit-and-run. Its proportions describe the conditions modeled in that study, not universal odds for all planetary collisions.

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Elebase USB to USB C Adapter for iPhone 18 Pro Max,USBC Car Charger Adapter
  • Read Before You Buy — No Video Output: These adapters support charging and USB 2.0 data transfer, but cannot transmit video signals. Except for standard USB webcams (which use USB data only), they are not compatible with HDMI/DisplayPort cables, video-capable USB-C hubs, or docking stations with video output.
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What determines the outcome?

  • Relative size and mass: A smaller impactor may erode a larger planet, while similarly sized bodies can merge, rebound, or disrupt each other.
  • Impact angle: A direct strike transfers energy differently from a grazing encounter. An oblique collision may produce a hit-and-run or graze-and-merge.
  • Speed: Greater impact energy can increase melting, vaporization, fragmentation, and atmospheric loss. Speed alone does not determine the result.
  • Composition and internal state: Iron-rich cores, rocky mantles, volatile materials, and prior heating affect what stays bound, escapes, or changes phase.
  • Spin and gravitational setting: Rotation and the system’s gravity influence the remnant’s motion and whether debris can remain in orbit.

What happens to the planets’ material and atmosphere?

A powerful collision sends shock waves through the bodies. Rock at the surfaces can melt or vaporize, and fragments can be launched into space. Material may fall back onto the largest remnant, escape the system, or remain in orbit around a remnant or its star. In this way, impacts can both build planets and reshape or erode them.

Atmosphere can be lost or added

A collision can strip away a planet’s atmosphere, but it can also contribute gases if the impactor carries an atmosphere of its own. A NASA simulation study published in 2020 modeled different body sizes, speeds, compositions, and impact angles for Moon-forming collisions. In those scenarios, the modeled impacts removed about 10% to 60% of Earth’s atmosphere. That range applies to those simulated scenarios, not to planetary collisions generally.

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Could a collision make a moon?

Yes. Material flung into orbit after an impact can remain gravitationally bound to a planet and, under suitable conditions, coalesce into a satellite. In a conventional debris-disk picture, orbiting material gathers over months or years. A high-resolution simulation reported a faster possible route: it placed material directly into orbit and suggested a moon could assemble in hours. That is a simulation result and a hypothesis to test, not an established timeline for how moons form.

Did a planet collision create our Moon?

The leading hypothesis is that a large impactor, commonly called Theia, struck the young Earth and that material from the collision contributed to the Moon. NASA points to the chemical similarity of Earth and Moon rocks, evidence that the Moon once had a magma ocean, and the Moon’s impact record as evidence consistent with an impact origin. The Apollo missions returned 842 pounds (382 kilograms) of lunar samples, which continue to inform studies of the Moon’s formation.

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Anker USB C Hub, 7in1 Multi-Port USB Adapter, 4K@60Hz USBC to HDMI Splitter
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The impact idea is not a complete, settled reconstruction. A successful explanation must account for the Moon’s composition, interior, and present orbit, and scientists continue to test different impact scenarios against samples, spacecraft observations, and models. NASA’s Moon-formation page gives an approximate formation estimate of 60 million years after the Solar System began forming; a NASA Webb article published October 1, 2026, refers to an estimate of around 100 million years after the Sun formed. These are source-specific approximations, not a single precise, agreed date.

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How do astronomers find evidence of collisions elsewhere?

Astronomers often infer a collision from its aftermath rather than watching intact planets collide. Dust, rubble, and the composition of debris around a star can preserve clues about what was struck and how energetic the impact was.

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Rocky debris around HD 172555

NASA’s 2009 account of observations around the young star HD 172555 describes signatures of vaporized rock, melted rock, and rubble, interpreted as evidence of a high-speed collision between rocky bodies. In that interpretation, the bodies’ relative speed was at least 10 kilometers per second (about 22,400 miles per hour). This is an inferred speed, not a directly observed collision.

Extreme debris disks observed by Webb

A NASA Webb report dated October 1, 2026, describes extreme debris disks in young stellar systems. Its interpretation associates silica-rich disks with high-energy impacts involving Mars-sized objects, and silica-poor disks with less energetic collisions involving Moon-sized bodies. The dust composition and brightness help researchers estimate the event’s energy and scale; the observations are not footage of complete planets visibly crashing together.

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Anker USB C Hub, 5-in-1 USBC to HDMI Splitter with 4K Display
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