Extraordinary, moon-forming planet collision spotted 1850 light-years away

All throughout the Universe, there are normally three ways that moons can form.

Pluto, shown as imaged with Hubble in a composite mosaic, along with its five moons. Charon, its largest, must be imaged with Pluto in an entirely different filter due to their brightnesses. The four smaller moons orbit this binary system with a factor of 1,000 greater exposure time in order to bring them out. Nix and Hydra were discovered in 2005, with Kerberos discovered in 2011 and Styx in 2012. These five moons were likely formed via an early collision, rather than either in situ or as a result of gravitational capture.

1.) A circumplanetary disk can fragment into moons, common around giant worlds.

Wide-field (left) and close-up (right) views of the moon-forming disc surrounding PDS 70c. Two planets have been found in the system, PDS 70c and PDS 70b, the latter not being visible in this image. They have carved a cavity in the circumstellar disc as they gobbled up material from the disc itself, growing in size. In this process, PDS 70c acquired its own circumplanetary disc, which contributes to the growth of the planet and where moons are very likely in the process of forming, similar to the formation of Jupiter’s Galilean moons.

2.) Interloping, low-mass bodies can be gravitationally captured.

Triton’s south polar terrain, as photographed by the Voyager 2 spacecraft and mapped to a spheroid of the appropriate shape and size. About 50 dark plumes mark what are thought to be cryovolcanoes, with those dark trails colloquially called ‘black smokers.’ Triton is a captured Kuiper belt object, having most certainly cleared out almost all of Neptune’s original moons, and represents the largest captured Moon in the known Universe for now.

3.) Or giant collisions can occur, kicking up debris that coalesces into moons.

When two large bodies collide, as they very likely did between proto-Earth and a hypothesized smaller but still massive world known as Theia in the early Solar System, they’ll generally merge to form one more massive body as a result, but the debris kicked up from the collision can coalesce into one or more large moons. This was likely the case not only for Earth, but for Mars and Pluto and their lunar systems as well, forming our modern Earth and Moon just a few tens of millions of years after the Sun ignited.

That third way explains many lunar systems, including Earth’s, Mars’s, and even Pluto’s.

Rather than only the two Martian moons we see today, Phobos and Deimos, a collision followed by a circumplanetary disk may have given rise to three moons of Mars, where only two survive today. The idea is that Mars’s once-innermost moon was destroyed and fell back onto Mars long ago. This hypothetical transient moon of Mars, proposed in a 2016 paper, is now the leading idea in the formation of Mars’s moons, and helps explain the enormous differences in topography between Mars’s northern and southern hemispheres.

When a massive planetary collision occurs, a diffuse, puffed-up structure known as a synestia forms.

A synestia will consist of a mixture of vaporized material from both the larger mass planet/protoplanet and the smaller impactor, which will form one or more large moons inside of it from the coalescence of moonlets. This is a general scenario capable of creating one single, large moon with the physical and chemical properties we observe Earth’s moon to have, multiple moons like those found around Mars or Pluto, or more complex systems around higher-massed worlds.

There can be so much debris that even the parent star’s light can be blocked.

When two objects in space collide, whether asteroids, moons, rocky planets, or even giant planets, a large cloud of light-blocking debris will be produced. When that cloud passes in front of its parent star relative to an external observer, that star will appear to dim and fainten. Many such collisions likely occurred between planetesimals in our early Solar System, giving rise to a fascinating set of planetary and lunar systems.

These events should be common in young stellar systems, emitting long-lasting infrared afterglows.

This image shows, in infrared light (taken with the WISE space telescope), the 1572 remnant of a type Ia supernova: Tycho’s “stella nova.” Ejected stellar material can glow due to heat in the infrared for tens of thousands of years, and the ejecta from supernova can be asymmetric and can have segregated elements within it.

It looks like scientists just witnessed the creation of one: around a star located 1850 light-years away.

This simulated collision shows what would happen when Neptune/Mini-Neptune planets collide, with debris, ejecta, and a synestia resulting in the aftermath. Although much of this material will eventually be stretched out over the orbit of the post-merger planet, much of it will remain in a circumplanetary synestia structure, destined to form moonlets and eventually a new lunar system around the final-state planet.

In December of 2021, a young, unremarkable star — 2MASS J08152329-3859234 — suddenly dimmed spectacularly.

Whereas Betelgeuse, as shown here, dimmed and then re-brightened due to a surface event intrinsic to the star itself, other mechanisms for stellar dimming, including dust, debris, and other light-blocking phenomena, are more common around lower-mass, young stellar systems.

This wasn’t observed by a human, but by an all-sky supernova monitoring service: ASAS-SN.

ASAS-SN is an all-sky supernova (and other transient event) search constructed in partnership with Las Cumbres Observatories and built with off-the-shelf astronomical equipment. It is one of the best ways we have, today, of automatically detecting brightening or faintening events for stars, wherever and whenever they occur.

Looking in archival data, an infrared brightening — with wavelength-dependent magnitudes — occurred ~2.5 years prior.

In the top row, the brightness of the main star located 1850 light-years away is shown. Below, infrared observations of the system dating back to years before the dimming event can be seen, supporting the notion of an energy-releasing collision between two planets in the outer part of this stellar system. When that debris cloud blocks the parent star’s light, the faintening/dimming event occurs.

It’s as though two Neptune/mini-Neptune exoplanets collided, creating a massive debris cloud.

Its infrared afterglow should persist for centuries.

A synestia doesn’t just consist of this puffy ring/torus of debris around a joint planetary core, but also rises to temperatures in excess of 1000 K, causing it to emit substantial amounts of its own infrared radiation, with peaks in different parts of the infrared spectrum dependent on the exact temperature and temperature profile of the system in question. The heat from the early Moon, just 24,000 km away initially, would have played a role in heating the lunar-facing side of the Earth.

Periodically, that cloud blocks its parent star’s light.

The dimming that the star 2MASS J08152329-3859234 experienced can be well-modeled by a cloud of debris resulting from a planet-planet collision passing in front of its parent star located at a significant orbital distance from the star itself. This is consistent with a synestia: a proposed debris cloud that would result from such a planet-planet collision, transiting in front of the star relative to our line-of-sight.

In time, a single giant world with a rich lunar system will emerge.

This artist’s impression shows a synestia: the aftermath of a massive planetary collision that creates a puffy torus-like shape of debris that persists for many thousands of years. As the synestia evolves, a circumplanetary disk with moonlets and eventually full-fledged moons will emerge.

Mostly Mute Monday tells an astronomical story in images, visuals, and no more than 200 words.