What kind of spacecraft can be used to explore and study the subsurface lunar environment? This is what a recent study presented at the 56^th Lunar and Planetary Science Conference (LPSC) hopes to address as an international team of researchers discussed the benefits of a mission concept called LunarLeaper, which will be designed to traverse and analyze the various aspects of the lunar subsurface environment, including moon pits and lava tubes.

Here, Universe Today discusses this incredible research with Dr. Anna Mittelholz, who is a lecturer in the Department of Earth and Planetary Sciences at ETH Zurich and lead author of the study, regarding the motivation behind the study, significant takeaways, next steps in developing LunarLeaper, and the importance of exploring the subsurface lunar environment. Therefore, what was the motivation behind the study?

Dr. Mittelholz tells Universe Today, “The primary motivation behind LunarLeaper was to enable agile and versatile access to challenging lunar terrain—particularly regions that traditional rovers struggle to reach, like steep slopes, rugged ejecta fields, and skylights leading to lava tubes. Paired with this outstanding science questions around subsurface lava tube was motivation enough!”

For the study, the researchers discussed several aspects of the LunarLeaper mission concept, including mission objectives, detailed breakdown of data collection, and how LunarLeaper could lay the foundation for future lunar exploration missions. For mission objectives, LunarLeaper will explore and analyze lunar lava tubes for their robotic and human exploration potential, specifically regarding if they could be used for human habitation. Additionally, LunarLeaper will investigate lunar volcanic and geologic history and how the lunar regolith (dust) played a role in the Moon’s evolutionary history.

Most importantly, the researchers analyzed how LunarLeaper could operate on the Moon, specifically navigating the uneven subsurface terrain of lava caves. While the lunar surface has uneven regions from craters, boulders, volcanic fields, and mountains, the environment of lava caves is even more unpredictable from collapsed channels, loose rocks, or sharp edges. This occurs when lava cools and is frozen in place in awkward locations, creating an environment that is difficult to navigate for humans or robots. Therefore, what are the most significant takeaways from this study?

“One key takeaway is that legged locomotion—or in our case, leaping—on the Moon is not only feasible but potentially game-changing for planetary exploration,” Dr. Mittelholz tells Universe Today. “Our simulations show that a hopping robot can navigate uneven terrain much more effectively than wheeled systems. Additionally, we’ve highlighted our specific mission architectures where this approach could provide unique scientific returns, especially in subsurface exploration.”

Mission concepts often take years to go from an idea to reality, comprised of a myriad of steps to ensure all mission aspects are fully operational and capable of performing in a space-based environment. This includes designs, tests, re-designs, more tests, system integrations to ensure each system can communicate with each other, more tests, countless meetings regarding funding and timetables, even more tests, until it’s finally ready for launch. NASA uses their Technology Readiness Levels (TRL) system to gauge progress on a mission plan and rate this progress, accordingly. Therefore, what are the next steps in developing LunarLeaper?

Dr. Mittelholz tells Universe Today, “We just passed our mission concept review and are now mostly focused on increasing the TRL of key systems, such as the locomotion and autonomous navigation.”

While NASA’s Apollo program proudly conducted the most in-depth surface exploration of the Moon, robotic and human exploration of the Moon’s surface began with missions conducted by NASA and the Soviet Union with the Luna and Ranger missions, respectively. As NASA geared up for Apollo, they conducted the Surveyor missions to better understand landing on the Moon’s surface.

After Apollo 17 in 1972, NASA entered a decades-long lull in lunar surface exploration but has still successfully conducted orbital exploration that has helped scientists gain immense insight into the Moon’s formation and evolution, and specifically its geologic and volcanic history. These orbital missions have identified more than 200 moon pits that could potentially lead to lava caves on the Moon while enabling future missions to explore the subsurface lunar environment. But what is the importance of exploring the subsurface lunar environment?

“From an exploration perspective, subsurface lava tubes are of incredible importance as they provide natural shelter for humans, protecting against harsh lunar conditions such as extreme temperature fluctuations, solar radiation, and micrometeorite impacts,” Dr. Mittelholz tells Universe Today. “These environments could serve as safe havens for long-duration missions, offering a potential foundation for sustainable lunar habitation. From a science perspective, the pits provide direct access to the Moon’s subsurface stratigraphy, potentially exposing pristine geological layers that have remained unaltered for billions of years. Studying these layers could yield critical insights into the Moon’s volcanic history, thermal evolution, and the broader processes that shaped the early solar system.”

How will LunarLeaper help scientists better understand the subsurface lunar environment in the coming years and decades? Only time will tell, and this is why we science!

As always, keep doing science & keep looking up!

Links:

• LPSC Abstract - https://www.hou.usra.edu/meetings/lpsc2025/pdf/1957.pdf
• Dr. Anna Mittelholz Personal Website - https://www.annamittelholz.com/
• LunarLeaper - https://www.lunarleaper.space/

The Solar System consists of our star, the Sun, and everything bound to it by gravity; the planets Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, and Neptune, along with dwarf planets like Pluto, dozens of moons, and millions of asteroids and comets. The planets orbit the Sunin elliptical paths, with the inner four being rocky terrestrial worlds and the outer four being gas and ice giants many times larger than Earth.

Artist impression of our Solar System

(Credit : Cacti Staccing Crane)

Our fascination with hunting down more planets in the Solar System has until now not revealed any strong candidates. With Pluto having been classed as the 9th planet for many years, the hunt was on for Planet X. With the demotion of Pluto in 2006, the idea of Planet Nine was first proposed in 2016 by astronomers Batygin and Brown. Its existence is inferred from unusual orbital clustering of several trans-Neptunian objects, suggesting they're being influenced by a large, unseen planetary body. Despite extensive searches using powerful telescopes, Planet Nine has remained theoretical as direct observation has proven elusive.

In a study led by Terry Long Phan and published in Cambridge University Press, the team searches for Planet Nine candidates by using two far-infrared all-sky surveys, IRAS and AKARI, whose 23-year separation allows detection of Planet Nine’s expected orbital motion (~3′/year). The search uses the AKARI Far-Infrared Monthly Unconfirmed Source List (AKARI-MUSL), which is better suited for identifying faint, moving objects than the standard AKARI Bright Source Catalogue. Researchers estimated Planet Nine’s expected flux and motion based on assumed mass, distance, and temperature, then applied positional and flux criteria to match sources between IRAS and AKARI. They identified 13 candidate pairs with angular separations corresponding to heliocentric distances of 500–700 AU and masses of 7–17 Earth masses.

Infrared Astronomical Satellite in space simulator at JPL

(Credit : NASA)

After a rigorous analysis and selection process, including visual inspection of images, the team identified one strong candidate pair, where the IRAS and AKARI sources showed the expected angular separation (42′–69.6′) and were not detected at the same position in each survey. The AKARI detection probability map confirmed the candidate’s consistency with a slow-moving object, showing two detections on one date and none six months earlier. However, IRAS and AKARI data alone are insufficient to determine a precise orbit so there will need to be follow-up observations with DECam, which can detect faint moving objects within about an hour of exposure, are suggested to confirm the candidate and fully determine its orbit, aiding in understanding the solar system’s evolution and structure.

The search for Planet Nine continues to push the boundaries of astronomical discovery using advanced survey techniques and paring it with careful analysis. While the identification of a promising candidate is an exciting step forward, confirmation will require further observations and continued collaboration across the astronomical community. If Planet Nine is ultimately detected, it would mark a monumental addition to our understanding of the Solar System.

Source :

•  A Search for Planet Nine with IRAS and AKARI Data

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Magnetars are among the rarest - and weirdest - denizens of the galactic zoo. They have powerful magnetic fields and may be the source of fast radio bursts (FRBs). A team of astronomers led by European Space Agency researcher Ashley Chrimes recently used the Hubble Space Telescope (HST) to track one of these monsters called SGR 0501+4516 (SGR0501, for short, and SGR stands for Soft Gamma Repeater). It's whipping through the Milky Way at a rate as high as 65 kilometers per second. The big challenge was to find its birthplace and figure out its origin.

At first, astronomers thought it could be related to a supernova remnant called HB9. After a great deal of study, it turns out SGR0501 is not the product of a massive core-collapse supernova, but Chrimes and her colleagues aren't completely sure of its origin, which makes it even more rare and strange.

“Magnetars are neutron stars — the dead remnants of stars — composed entirely of neutrons. What makes magnetars unique is their extreme magnetic fields,” said Chrimes. "Our definite conclusion is that SGR0501 did not originate in HB9. However, since there is no other clear birth site or smoking gun for a different origin, the alternatives are all plausible and we can’t yet say which is the most likely."

Unraveling the Track of the Traveling Magnetar

There are only about 30 known magnetars in the Milky Way Galaxy. These dense balls of neutrons aren't very big - only about 20 km (12 miles) across. Their tiny sizes belie the incredibly strong magnetic fields that they generate. As the folks at NASA like to say, those fields are strong that if one flew by Earth at the distance of the Moon, all our credit cards would be wiped out. Even worse, if we flew out to visit the magnetar on its way, our ship and astronauts would be torn apart.

Luckily, we only observe them from a distance. Chrimes estimates that it most likely lies about 2,000 parsecs (~6520 light-years) away from us. SGR0501 was originally spotted in 2008 when the Swift Observatory detected brief but bright flashes of gamma rays in its direction. It also looked like it was close to the supernova remnant HB9. Naturally, astronomers assumed the two might be related, since known magnetars are the result of core collapse supernova explosions.

The separation between the magnetar and the center of the supernova remnant on the sky is just 80 arcminutes, or slightly wider than your pinky finger when viewed at the end of your outstretched arm. However, things didn't add up after astronomers studied the magnetar with HST. A decade-long set of Hubble observations resulted in images that helped astronomers figure out the magnetar's path as it travels. By tracking its position, the team charted the object’s apparent motion across the sky. Both the speed and direction of SGR 0501+4516’s movement showed that it could not be associated with the nearby supernova remnant. Tracing the magnetar’s trajectory thousands of years into the past showed that there were no other supernova remnants or massive star clusters that could have produced it.

So, What Formed It?

So, if SGR0501 didn't form in a supernova explosion, what else could form a tiny ball of neutrons with a super-strong magnetic field? That was the challenge the team faced next. It turns out that there are a couple of non-supernova ways to make magnetars. One is by merging two lower-mass neutron stars. That would create the larger, stronger SGR0501.

An artist's conception of the merger of two neutron stars to form a more massive one. Such a collision would also emit radio bursts and other emissions.

Courtesy ESO/University of Warwick/Mark Garlick

The other way is by something called accretion-induced collapse. For that, you need a binary star system with a white dwarf as one of the components. As it pulls in gas and material from its companion, it can get greedy and take too much. That destabilizes the white dwarf and leads to a massive explosion. “Normally, this scenario leads to the ignition of nuclear reactions, and the white dwarf exploding, leaving nothing behind. But it has been theorized that under certain conditions, the white dwarf can instead collapse into a neutron star. We think this might be how SGR 0501 was born,” added co-investigator Andrew Levan of Radboud University in the Netherlands and the University of Warwick in the United Kingdom.

How are Fast Radio Bursts Connected to Magnetars?

The birth of a magnetar is a pretty powerful event that gives off the kind of brief but strong emissions that characterize fast radio bursts. If SGR0501 formed from a marger or accretion-induced collapse, that might explain the phenomenon of FRBs. These are very short (on the order of less than a millisecond) that don't always re-occur (in other words, they're transient flashes in the sky). Many FRBs occur outside our Milky Way, but some are also detected within the Galaxy.

“Magnetar birth rates and formation scenarios are among the most pressing questions in high-energy astrophysics, with implications for many of the universe’s most powerful transient events, such as gamma-ray bursts, super-luminous supernovae, and fast radio bursts,” said Nanda Rea of the Institute of Space Sciences in Barcelona, Spain. Magnetars that form through accretion-induced collapse could provide the kinds of short, powerful bursts of radio waves that characterize FGBs. In particular, that could explain the FRBs seen in ancient stellar populations too old to have massive stars that could explode as supernovae. Since there are other magnetars to study, the team is planning to use HST for further observations of these weirdly magnetic stellar remnants.

For More Information

• NASA’s Hubble Tracks a Roaming Magnetar of Unknown Origin
• The Infrared Counterpart and Proper Motion of Magnetar SGR 0501+4516
• arXiv version

The discovery of exoplanets has transformed astronomy since the early 1990s. Using methods like transit photometry and radial velocity measurements, scientists have identified over 5,000 planets beyond our Solar System, revealing an incredible range of worlds from scorching gas giants to potentially habitable Earth-sized worlds. Space telescopes like Kepler, TESS, and James Webb have increased these discoveries, allowing us to study distant planetary atmospheres.

The James Webb Space Telescope has revolutionised our view of exoplanets

(Credit : NASA)

One particular type of exoplanet, the super-Earths have masses between Earth and Neptune, typically 2-10 times Earth's mass. They are absent from our Solar System but seem to be common elsewhere. Even within this classification, these worlds display remarkable diversity; some rocky with thin atmospheres, others with thick gaseous envelopes. Many orbit in their stars' habitable zones, raising possibilities for liquid water, though their stronger gravity and often tidally locked rotation would create distinctly alien conditions.

A recent study published in Science reveals that super-Earths are common throughout our Galaxy. The international research team, including astronomers from the Center for Astrophysics at Harvard & Smithsonian, discovered a particularly notable super-Earth orbiting its star at a distance greater than Saturn is from our Sun, a region where previously only massive planets had been found.

Illustration of the inferred size of the super-Earth CoRoT-7b (center) in comparison with Earth and Neptune

"We found a 'super Earth'... in a place where only planets thousands or hundreds of times more massive than Earth were found before," explained CfA Fellow Weicheng Zang, the study's lead author. This discovery highlights how dramatically different other planetary systems can be from our own Solar System and contributes to a broader investigation measuring planetary masses relative to their host stars, enhancing our understanding of planetary populations across the Milky Way.

This groundbreaking discovery of a distant super-Earth is part of a comprehensive study that has revealed new insights about planetary populations across the Milky Way by measuring planet masses relative to their host stars. Using microlensing (a technique where light from distant objects is amplified by intervening bodies) researchers could detect planets at large distances from their stars, comparable to the Earth-Saturn orbital range. This represents the largest study of its kind, examining about three times more planets and including worlds approximately eight times smaller than previous microlensing-detected samples.

This study also reveals super-Earths are at least as common as Neptune-sized planets throughout our galaxy, significantly advancing planetary science through advanced observational techniques. As instruments like the James Webb Space Telescope continue characterizing exoplanet atmospheres, astronomers edge closer to understanding planetary formation and the potential for extraterrestrial life. The discovery of such diverse planetary systems challenges our assumptions and suggests a Universe filled with planets of varied sizes and compositions in unexpected orbital arrangements. This expanding cosmic census not only deepens our astronomical knowledge but helps us better understand Earth's place in the Cosmos.

Source : 

• Astronomers Find Far-flung “Super Earths” Are Not Farfetched

Lately, there's been plenty of progress in 3D printing objects from the lunar regolith. We've reported on several projects that have attempted to do so, with varying degrees of success. However, most of them require some additive, such as a polymer or salt water, as a binding agent. Recently, a paper from Julien Garnier and their co-authors at the University of Toulouse attempted to make compression-hardened 3D-printed objects using nothing but the regolith itself.

Getting things into space is expensive, so it should be no surprise that any 3D printing technology that requires shipping large amounts of things from Earth is at a disadvantage. Various projects, like one being run by a company called AI Spacefactory, utilize additives like polymers that must be made on Earth and then shipped to the Moon before being combined with regolith in situ.

Dr. Garnier hoped to get around that requirement by using selective laser melting (SLM) on a specific type of regolith analog. Known as Basalt of Pic d'Ysson (BPY), this volcanic rock is collected from the Pic d'Ysson, an ancient, extinct volcano in France. It started growing in popularity as a lunar regolith simulant in the early 2000s due to its chemical and mineral composition similarity to basaltic rocks found on the Moon itself.

Lunar regolith will also be a massive pain for explorers in the beginning, as Fraser discussed with Dr. Kevin Cannon

BPY has already been the target of several studies in lunar 3D printing. ESA researchers have published a paper detailing a "solar sintering" technique that uses the Sun's power to fuse PBY powder. Project MOONRISE, which we've reported previously, also used BPY as a feedstock in its zero-gravity 3D printing applications.

However, most of those studies have found that the BPY wasn't up to snuff when 3D printed, at least in terms of the compression strength of the resultant material. Despite the Moon's lower gravity, there are still stresses on the structures of buildings and equipment on the Moon. If a material's compressive strength can't handle that weight, even in the lower gravity, then it's not much use as a building material.

Measurements for the compressive strength of 3D printed BPY vary dramatically based on the type of 3D printing technique used. Powder Bed Fusion processes, which are regularly used to print metals on Earth, had a compressive strength of 4.2 MPa, slightly more than a standard masonry brick. However, that was with a porosity of almost 50% - meaning nearly half the structure was full of holes. Combining 3D printed BPY with a geopolymer binder can increase its strength, but at the cost of requiring the geopolymer to be shipped from Earth.

What might we manufacture on the Moon? Fraser discusses that question with Dr. Alex Ignatiev

The researcher DR. Garnier and his co-authors focused on trying to uncover what properties of the BPY could lead to better mechanical properties. They varied characteristics like whether the powder was primarily "crystalline" or "amorphous". Crystalline powder has a very ordered structure, with some properties, such as compressive strength, varying widely depending on the direction the ordered crystal structure points. On the other hand, amorphous powder is much more disordered, with its physical properties being the same in all directions.

Experiments showed a doubling in the compressive strength of powder that was 100% crystalline compared to powder that was 100% amorphous, highlighting the importance of the regolith structure selected to build the building materials of any future lunar base. 

Optimizing that mix between amorphous and crystalline structure remains on the list of things to do for future work, as well as optimizing the size of particles in the feedstock and the parameters used in the SLM process to create the final material. There's still a long way to go before astronauts can print something usable on the surface of the Moon. But as the date for humanity's return draws closer, it's probably only a matter of time before a mission does make use of the resources available on our lunar neighbor - and they might do so by melting it with a laser.

Learn More:

• J Garnier et al - Selective laser melting of partially amorphous regolith analog for ISRU lunar applications
• UT - MOONRISE: Melting lunar regolith with lasers to build structures on the Moon
• UT - NASA Sends a 3D Printer for Lunar Regolith and More to the ISS
• UT - What Could We Build With Lunar Regolith?

There's no better word for this image of the Sun than Spectacular, which means something impressive, dramatic, or remarkable that creates a spectacle or visual impact. It comes from the Latin word spectaculum, which means a show, spectacle, or public exhibition. Ancient Romans would agree with the word choice if you could somehow show the image to them.

This composite image of the Sun was constructed from 200 individual images captured by the ESA's Solar Orbiter. It shows the Sun's corona, its million-degree atmosphere, in UV. The spacecraft captured the photos on March 9th, 2025, when it was about 77 million km from the Sun.

The Solar Orbiter pointed at different regions of the Sun in a 5x5 grid. During each pointing, the spacecraft captured six high-resolution and two wide-angle images with its Extreme Ultraviolet Imager, an instrument designed to study the Sun's chromosphere and Corona.

The grey region shows the 5x5 grid in one position on the Sun's surface.

Image Credit: ESA & NASA/Solar Orbiter/EUI Team, D. Berghmans (ROB) LICENCE CC BY-SA 3.0 IGO

The image shows coronal loops, solar prominences, and filaments. Interested readers can download a high-resolution image, allowing them to zoom in on incredible detail.

It's easy to lose yourself in the incredible details of the image. The looping structures on the Sun's limb are prominences. They're plasma and magnetic field structures that have their roots in the photosphere and extend into the corona. They can last weeks and even months, extending for hundreds of thousands of kilometres. Sometimes, they detach from the Sun and become coronal mass ejections (CMEs).

When CMEs strike Earth, they can trigger geomagnetic storms that, if strong enough, can damage power grids and cause other mayhem. That's one of the primary reasons scientists study the Sun. CMEs and the constant solar wind are collectively called space weather.

Studying the Sun also helps scientists understand stellar physics and stellar evolution. Many of the Sun's processes, like nuclear fusion and plasma dynamics, are present elsewhere in the Universe, making the Sun a natural laboratory for observing those processes.

If you'd like to download the large, high-res image, visit this.

The Moon's surface is covered by impact craters, ranging from microscopic pits to massive basins over 1,000 kilometres across. These craters formed primarily during the Late Heavy Bombardment period about 4 billion years ago, when the inner Solar System experienced an intense period of asteroid and comet impacts. Unlike Earth, where weathering, erosion, and tectonic activity continually reshapes the surface, the Moon lacks an atmosphere and significant geological activity, allowing these impact features to remain preserved for billions of years. This remarkably preserved cratering record serves to capture crucial history of the formation and evolution of our Solar System.

Lunar craters over the South Pole

(Credit : NASA)

During the formation of craters a significant quantity of the ejected lunar material achieves the Moon’s escape velocity and reaches Earth. Studying these rocks helps us to understand how material moves between the two bodies. A team of researchers have turned their attention to this study and their paper has recently been published. The research, led by Jose Daniel Castro-Cisneros utilises better computer models than previous studies to track how Moon debris reaches Earth.

The study uses simulations to examine more starting conditions over longer time periods to better estimate how much lunar material reaches Earth and whether it contributes to near Earth objects. The team also hoped that by studying Moon debris trajectories, they would be able to piece together Earth's impact timeline and how it affected life and geology. They are also especially interested in objects like Kamo'oalewa, believed to be between 36-100 metres in diameter orbiting near Earth that might actually be a piece of the Moon.

Previous studies of lunar ejecta were improved upon by using the REBOUND simulation package to track particles from the Moon for 100,000 years. Unlike earlier work that used separate phases, the team simultaneously model Earth and the Moon using a more realistic ejection velocity distribution. They recorded data every five years and collision events defined as ejecta reaching 100 km above Earth's surface, providing a more comprehensive picture of how material transfers from the Moon to Earth.

Crater Tycho displaying its wonderful system of rays thought to be lunar ejecta.

The model employed, used simplified vertical impacts, though natural oblique impacts would direct more material toward Earth at lower angles, the approach simplified the process. Current environmental conditions were assumed but historically, when the Moon was closer and experiencing heavier bombardment (over 1.1 billion years ago), even more lunar material would have reached Earth. Future research should incorporate oblique impact models and ancient orbital configurations to better understand early Earth-Moon material exchange.

The team were able to conclude that, following lunar impacts, Earth collects about 22.6% of the ejected material over 100,000 years, with half of these collisions occurring within the first 10,000 years. The collision rate follows a power-law distribution over time (a relationship where a change in one quantity results in a proportional relative change in another) independent of the initial size of those quantities. Material launched from the Moon's trailing side has the highest Earth collision probability, while the leading side produces the lowest. When hitting Earth, lunar ejecta travel at 11.0-13.1 km/s and predominantly strike near the equator (with 24% fewer impacts at the poles). These impacts are nearly symmetrically distributed between morning and evening hours, peaking around 6 AM/PM.

This research significantly advances our understanding of lunar-Earth material exchange, showing that nearly a quarter of lunar impact ejecta reaches Earth—half within just 10,000 years. The findings about equatorial impact concentration and the importance of lunar launch location reveal previously unknown patterns in this process. These results enhance our understanding of the Earth-Moon system's shared impact history while supporting the lunar origin hypothesis for objects like Kamo’oalewa.

Source : 

• Lunar impact ejecta flux on the Earth

Near-Earth Objects (NEOs) are rocky bodies orbiting our Solar System that pass relatively close to Earth's orbit. Scientists have identified over 30,000 NEOs ranging from small boulders to massive rocks spanning several kilometres in diameter. These celestial bodies are of particular interest to astronomers not only for their scientific value in understanding the formation of our Solar System but also because they pose potential impact hazards to our planet. Space agencies like NASA continuously monitor these objects through programs such as the Near-Earth Object Surveillance Mission, calculating their trajectories to provide early warnings of possible collisions.

Near Earth Object Comet Hartley-2 captured by NASA's EPOXI mission

(Credit : NASA/JPL-Caltech/UMD)

Despite significant advances in asteroid detection technology in recent decades, important gaps remain. Ground-based survey programs like the Catalina Sky Survey and Pan-STARRS have collectively discovered over 90% of near-Earth asteroids larger than 1 kilometre, significantly reducing the risk from globally devastating impacts. However, detection rates drop dramatically for smaller objects, with less than 40% of potentially hazardous asteroids in the 140-meter range currently cataloged. Detection challenges include limitations of ground-based telescopes (affected by weather, daylight, and atmospheric interference), blind spots near the sun, and the inherently dark, low-albedo nature of many asteroids.

A Catalina Sky Survey Observatory at dusk at Mount Lemmon Observatory in the Santa Catalina Mountains near Tucson, Arizona

(Credit : Daniel Oberhaus)

International and U.S. defence protocols have identified the urgent need for rapid-response spacecraft reconnaissance capabilities, particularly for asteroids around 50 meters in diameter—objects large enough to cause significant regional damage yet small enough to evade detection until they're dangerously close. Even after the completion of advanced survey initiatives like NEO Surveyor and the Rubin Observatory, approximately half of these 50-meter objects will remain undiscovered until they're nearly upon us. This sobering reality means that for many potential impact scenarios, a quickly deployed flyby mission may represent our only chance to gather critical data before impact.

The Rubin Observatory against the Milky Way

(Credit : Rubin Observatory/NSF/AURA/B)

In a recent paper authored by Nancy L. Chabot and team from Johns Hopkins University, they assert that a planetary defence flyby reconnaissance mission must demonstrate capabilities to quickly reach a small ~50-meter NEO, determine its Earth impact probability, and gather essential physical data to inform decision makers. This presents significant technical challenges, including managing flyby speeds up to 25 km/s and high solar phase angles while collecting crucial data from such a small target.

The core principle of planetary defence is that we don't choose which asteroids threaten us—we must be prepared to respond to whatever object presents a danger. Therefore, the team argues that the mission's true purpose isn't simply demonstrating asteroid flyby technology, but developing robust capabilities specifically tailored for the small, short-warning-time objects most likely to require rapid space-based studies, an essential advancement in our planetary defence readiness.

Source : 

• A Mission to Demonstrate Rapid-Response Flyby Reconnaissance for Planetary Defense

This week brings the Hubble Space Telescope's 35th birthday — but instead of getting presents, the Hubble team is giving out presents in the form of four views of the cosmos, ranging from a glimpse of Mars to a glittering picture of a far-out galaxy.

It’s the latest observance of a tradition that goes back decades, in which NASA and the Space Telescope Science Institute release pictures to celebrate the anniversary of Hubble’s launch into Earth orbit aboard the space shuttle Discovery on April 24, 1990.

“Hubble opened a new window to the universe when it launched 35 years ago,” Shawn Domagal-Goldman, acting director of the Astrophysics Division at NASA Headquarters, said today in an image advisory marking the occasion.

“The fact that it is still operating today is a testament to the value of our flagship observatories, and provides critical lessons for the Habitable Worlds Observatory, which we plan to be serviceable in the spirit of Hubble.”

Hubble didn’t get off to a smooth start. After the 24,000-pound observatory was deployed, scientists discovered that its nearly 8-foot-wide mirror had a manufacturing flaw. In 1993, during the first of five servicing missions, astronauts installed hardware that greatly improved the sharpness of Hubble’s images.

Since then, Hubble’s observations have revolutionized astronomy, contributing to discoveries related to exoplanets, black holes, the nature of the early universe, the existence of dark energy and the accelerating expansion of the cosmos. NASA says Hubble has made nearly 1.7 million observations so far, focusing on about 55,000 astronomical targets and resulting in more than 22,000 research papers.

All those discoveries, and all those images, endeared Hubble to the general public. The loss of the shuttle Columbia and its crew in 2003 led NASA to suspend plans for much-needed repairs, but because of the resulting outcry over the telescope’s potential demise, the space agency agreed to a final servicing mission that took place in 2009.

At the time, NASA expected the telescope to provide dazzling views for an additional five or 10 years. Once again, Hubble exceeded expectations, racking up 16 years of operation without on-orbit repairs.

The images released today illustrate the breadth of Hubble’s range:

• Pictures of Mars were captured between last Dec. 28 and 30, near the time when Mars came closest to Earth in its orbit. The images show the planet’s bright orange Tharsis plateau and its dormant volcanoes, the north polar ice cap and wispy water-ice clouds.

• Another Hubble image from last December focuses on a small portion of the Rosette Nebula, a huge star-forming region 5,200 light-years from Earth. Dark clouds of gas, laced with dust, are silhouetted across the image. The Hubble team also released a wider-scale image of the nebula to add cosmic context.

• In January, Hubble snapped a picture of the planetary nebula NGC 2899, seemingly fluttering like a cosmic moth 4,500 light-years from Earth. The colorful clouds of dust and gas have been shaped by the radiation and stellar winds blasting out from the star at the image’s center.

• Hubble produced a new view of the spiral galaxy NGC 5335 in March. The picture reveals a bar-shaped structure that slices across the galaxy and channels gas inward toward the center, fueling the production of new stars. Patchy streamers of star formation swirl around the edges of the galaxy.

Mars near opposition. Image: NASA, ESA, STScI; Image Processing: Joseph DePasquale (STScI)

Planetary nebula NGC 2899.

Image: NASA, ESA,  STScI; Processing: Joseph DePasquale (STScI)

Spiral galaxy NGC 5335.

Image: NASA, ESA, STScI; Image Processing: Alyssa Pagan (STScI)

Clouds in the Rosette Nebula.

Image: NASA, ESA, STScI; Processing: Joseph DePasquale (STScI)

In recent years, Hubble has been experiencing periodic hiccups, and it's only a matter of time before a glitch puts it out of commission permanently. Meanwhile, the spotlight has been shifting to NASA's James Webb Space Telescope, which was launched in 2021 and has seven times as much light-gathering capability as Hubble does.

Unlike Hubble, JWST sees the universe primarily in infrared light. It doesn't have Hubble's capability to make observations in a wide spectrum ranging from infrared to ultraviolet. And because JWST is positioned at a gravitational balance point a million miles from Earth, it can't be serviced in space, as Hubble was.

In contrast, the Habitable Worlds Observatory would study the universe in visible and ultraviolet light, producing images that would be significantly sharper than Hubble's views. A major goal of that future mission would be to identify potentially habitable Earthlike planets orbiting distant stars. The HWO would also be designed with robotic servicing in mind.

NASA's current plans call for launching the Habitable Worlds Observatory by as early as the 2040s, but those plans — and more immediate plans to launch the Nancy Grace Roman Space Telescope next year — have been thrown into doubt by a proposal from the Trump administration to make deep cuts in NASA's science budget.

A recent analysis gives us new views of key deep-sky objects.

It’s a cosmic shame, that we tend to only see flat-looking, 2-dimensional views of deep-sky objects. And while we can’t just zoom out past the Andromeda galaxy for another perspective, or see the Crab Nebula from another vantage point in space, we can use existing data to simulate objects in 3D.

A recent collection released by Marshall Space Flight Center’s Chandra X-ray Center and the Harvard-Smithsonian Center for Astrophysics shows us familiar objects in a new way. These models combine information from space-borne observatories, including the Chandra X-ray observatory. Released from the payload bay of Space Shuttle Columbia on STS-93, Chandra has proven itself over the last two decades as NASA’s flagship X-ray observatory in space.

Chandra, shortly after deployment from shuttle Columbia's payload bay.

Credit: NASA

The 3D renderings were made using a combination of observational data and computer simulations. The technique not only allows armchair observers to see old objects in new ways, but it also gives astronomers a method to study these familiar targets from all sides.

“These 3D models allow people to explore—and print—examples of stars in the early and end stages of their lives,” states a recent Chandra X-ray Center (NASA) press release. “They also provide scientists with new avenues to investigate scientific questions and find insights about the objects they represent.”

NASA is even providing users with the files to 3D print these deep-sky objects, free to download. This gives a tactile dimension to the sky, something the user can hold and feel. This is an important factor when it comes to science outreach… after all, none of us can see the sky at x-ray wavelengths.

Here’s the highlighted object-by-object breakdown:

Cassiopeia A: Located about 11,000 light-years distant, Cassiopeia A or Cas A is a well-studied supernovae remnant. A prodigious x-ray and radio source, Cas A hosted the last known galactic supernovae about 340 years ago, although no definitive observations of the event exist.

Cas A, to include the 'Green Monster' loop.

Credit: INAF-Osservatorio Astronomico di Palermo/Salvatore Orlando.

More recently, the James Webb Space Telescope (JWST) has documented what’s become known as the ‘green monster’, a long oxygen-rich filament extending from Cas A. This may provide more insight into this young and evolving remnant.

A 3D printed rendition of Cas A.

Credit: NASA/CXC/SAO/A. Jubett & N. Wolk/Modeled by Sal Orlando.

BP Tauri: This is a young T Tauri star surrounded by a dust ring, just 10 million years old. T Tauri stars are crucial to our understanding of stellar and solar system formation, as they provide a snapshot of the early stages of the process. These are also very energetic and active stars, with flares that sculpt the surrounding cocoon of dust that the stars are embedded in. BP Tauri and the x-ray flares it produces are of primary interest to Chandra researchers.

The Cygnus Loop: This is a familiar target for deep-sky imagers located in the constellation of Cygnus, the Swan. Another, more ancient supernovae remnant, the Cygnus Loop has since undergone a complex interaction with the interstellar medium, allowing Chandra to probe this domain as the residual blast wave is heated to millions of degrees. The Cygnus Loop is an extended object visually extending over three degrees across, about six times the angular diameter of the Full Moon.

The location of the Cygnus Loop in the sky.

Credit: Stellarium.

G 292.0+1.8: The last selected object is an obscure but crucial one. G 292.0+1.8 is another supernovae remnant, located in the constellation Centaurus the Centaur. Astronomers are interested in this remnant for two main reasons: One, it is usually rich in molecular oxygen. Two, it exhibits a rare, reverse shock wave rebounding back towards the original explosion, giving the remnant an asymmetrical shape.

These 3D models were also highlighted in studies out of the Italian Institute for Astrophysics (INAF) in Palermo Italy by Salvatore Orlando and cited in papers from the Monthly Notices of the Royal Astronomical Society, The Astrophysical Journal and Astronomy & Astrophysics.

Who doesn’t want a 3D rendition of the Cygnus Loop on their desktop? For now, it’s the next best thing to going there in person.

The weather gets a little wild and weird on Jupiter. How wild? Spacecraft instruments have measured strong winds, tracked fierce lightning, and found huge methane plume storms rising from deep beneath the clouds. How weird? Think: mushballs raining down like hailstones. They're made of ammonia and water encased in a water ice shell. According to planetary scientists, these mushballs plunge through the Jovian atmosphere. What's more, they probably form on the other gas and ice giants, too.

According to planetary scientist Chris Moeckel and his former advisor Imke de Pater at UC Berkeley, the proof for these strange Jovian slushies came from 3D visualizations of the Jovian atmosphere. You can't tell they're there just by looking at the clouds, however. You have to find a way to peer into the atmosphere and measure the chemical fingerprints of the gases it contains. In 2020, data from the Juno mission and observations by radio telescopes on Earth uncovered strange "nonuniformities" in ammonia gas distribution around the planet. In other words, it isn't distributed evenly throughout the atmosphere. The Juno data in particular showed that ammonia isn't just poorly distributed - it's actually depleted to atmospheric depths of about 150 kilometers, according to de Pater.

“Juno really shows that ammonia is depleted at all latitudes down to about 150 km (93 miles), which is really odd,” said de Pater, who discovered 10 years ago that ammonia was depleted down to about 50 km (31 miles). “That’s what Chris is trying to explain with his storm systems going much deeper than we expected.”

A flattened map of Jupiter reveals the distribution of ammonia beneath the planet’s cloud tops, extending tens of kilometers below the visible cloud deck. Red regions indicate where ammonia is depleted, while black regions show where it is rising from deeper within the atmosphere. The depleted zones appear in bands flanking the equator (0° latitude on the map) and at the poles (not shown), while the upwelling of ammonia is most prominent just north of the equator. The striking absence of deep activity in the mid-latitudes suggests that most of Jupiter’s atmosphere is relatively shallow, with only a few storms punching deeper into the planet.

Credit Chris Moeckel and Imke de Pater, UC Berkeley

Follow the Ammonia Trail

To explain that missing ammonia, another scientist named Tristan Guillot proposed a wild idea: that strong updrafts during storms on Jupiter can lift ice particles high above the clouds. There, the ice mixes with ammonia vapor, which melts the ice into a slush. Just like on Earth, as the ice balls rise and fall, they grow. Eventually, these softball-sized mushballs fall back into the atmosphere, taking the ammonia with them. This helps explain why ammonia appears to be missing from the upper atmosphere: it’s being dragged down and hidden deep inside the planet, where it leaves faint signatures to be observed with radio telescopes.

To Moeckel and others, that idea seemed like an "out there" explanation. "Imke and I both were like, ‘There’s no way in the world this is true,’” said Moeckel. “So many things have to come together to actually explain this, it seems so exotic. I basically spent three years trying to prove this wrong. And I couldn’t prove it wrong.”

Jovian Conditions Conducive to Mushballs

It turns out that conditions in Jupiter's atmosphere could support the formation of mushballs. That atmosphere is mostly hydrogen and helium, inhabited by clouds in its upper layers. Beneath the clouds and upper atmosphere lies a deeper layer of fluid metallic hydrogen. A rocky inner core lives deep inside the planet. The atmosphere contains smaller amounts of ammonia molecules and water vapor, which rise and freeze into droplets. On Earth, droplets of water fall onto the surface as rain or hail. However, Jupiter has no surface until you get to the core. So, if those droplets do fall, how far down do they go? How big do they get?

An illustration depicting how violent storms on Jupiter — and likely other gas giants — generate mushballs and shallow lightning. The mushballs are created by thunderstorm clouds that form about 65 km (40 miles) beneath the cloud tops and fuel a strong updraft that carries water ice upward to extreme altitudes, occasionally above the visible cloud layer. Once they reach altitudes of about 22 km (14 miles) below the visible cloud layer, ammonia acts like an antifreeze, melting the ice and combining with it to form a slushy ammonia-water liquid that gets coated with water ice — a mushball. The mushballs keep rising until they become too heavy and fall back through the atmosphere, growing until they reach the water condensation layer, where they evaporate. This ends up redistributing ammonia and water from the upper atmosphere (green and blue layer) to layers deep below the clouds, creating areas of depleted ammonia visible in radio observations.

Credit NASA/JPL-Caltech/SwRI/CNRS

This is where the mushballs come in. First, scientists began trying to figure out the strange distribution of ammonia in particular. There were proposals that water and ammonia ice get locked up in hailstones. However, nobody could quite explain how to form them heavy enough to fall hundreds of kilometers through Jupiter's messy atmosphere. That's when Guillot made his proposal for the growth of slushy hailstones.

Making a 3D Model

To understand the weather conditions and the possible formation of those weird mushballs, Moeckel began working on a different approach based on the observational data. “I essentially developed a tomography method that takes the radio observations and turns them into a three-dimensional rendering of that part of the atmosphere that is seen by Juno,” Moeckel said.

Moeckel's 3D picture of Jupiter’s troposphere shows that the majority of the weather systems on Jupiter really are shallow. Most extend down perhaps only 10 to 20 kilometers below the visible clouds. Most of the colorful, swirling patterns in the bands encircling the planet are part of that shallow contingent of clouds.

Some weather, however, emerges much deeper in the troposphere, redistributing ammonia and water and essentially unmixing what was long thought to be a uniform atmosphere. The three types of weather events responsible are hurricane-like vortices, hotspots coupled to ammonia-rich plumes that wrap around the planet in a wave-like structure, and large storms that generate mushballs and lightning.

Tripping with a Mushball

“The mushball journey essentially starts about 50 to 60 kilometers below the cloud deck as water droplets. The water droplets get rapidly lofted all the way to the top of the cloud deck, where they freeze out and then fall over a hundred kilometers into the planet, where they start to evaporate and deposit material down there,” Moeckel said. “And so you have, essentially, this weird system that gets triggered far below the cloud deck, goes all the way to the top of the atmosphere, and then sinks deep into the planet.”

Unique signatures in the Juno radio data for one storm cloud provided an important clue to the mushball formation. “There was a small spot under a cloud that either looked like cooling, that is, melting ice, or an ammonia enhancement, that is, melting and release of ammonia,” Moeckel said. “It was the fact that either explanation was only possible with mushballs that eventually convinced me.”

What About Other Planets?

The 3D model and explanations of mushballs on Jupiter offer a more complete look at the complicated dynamics of the Jovian atmosphere. Interestingly, it's very likely that similar conditions for mushball creation could exist at the other gas and ice giants of the solar system. If so, that would give planetary scientists much more insight into the interiors of those worlds as well as the activities going on in their atmospheres.

In an age of exoplanet research, it's also likely that researchers can use Moeckel's tools to extrapolate what they've seen at Jupiter to similar-type worlds around other stars. Since they can see only the upper atmospheres of distant worlds, the ability to interpret chemical signatures in those atmospheres using radio and other observations is important.

For More Information

• On Jupiter, It's Mushballs All the Way Down
• Tempests in the Troposphere: Mapping the Impact of Giant Storms on Jupiter's Deep Atmosphere
• Jupiter's Tropical Atmosphere: Shallow Weather, Deep Plumes and Vortices

Ever since the Mariner probes and Viking missions travelled to Mars, scientists have known that liquid water once flowed on the surface. This is indicated by specific features that form in the presence of water here on Earth, including flow channels, delta fans, hydrated minerals, and sedimentary rocks. In recent decades, the many missions that have studied Mars' atmosphere, surface, and climate have revealed that Mars was a warmer, wetter place during the Noachian period (ca. 4.1 to 3.7 billion years ago).

This has stimulated questions about whether life could have emerged on Mars and where its once-abundant water (and maybe even life) could be found today. A new study by geologists at the University of Colorado Boulder (CU Boulder) provides a potential glimpse of what Mars may have looked like billions of years ago. Their findings suggest Mars experienced heavy precipitation that likely fed valleys and channels that carved the features we still see there today.

The research was led by Amanda Steckel, a postdoctoral geological scientist at Caltech (formerly at CU Boulder), and a member of the Perseverance science team. She was joined by Gregory E. Tucker, a geoscience professor at CU Boulder and a member of the Cooperative Institute for Research in Environmental Sciences (CIRES); Matthew Rossi and Brian Hynek were also co-authors on the study, a research scientist with CIRES and the Earth Lab and a geosciences professor with the Laboratory for Atmospheric and Space Physics (LASP) at CU Boulde, respectively.

While most scientists agree that Mars once had flowing water on its surface, where it came from remains a mystery. While most maintain that a global ocean once covered the entire Northern Lowlands of Mars, while large bodies spotted the southern hemisphere, many scientists assert that Mars was always cold and dry. In this scenario, water existed mainly as ice caps and glaciers that occupied the Northern Lowlands, which experienced occasional melting for short periods.

This is largely based on the fact that roughly 4 billion years ago, the young Sun was only 75% as bright as it is today. As a result, Mars must have had a significant greenhouse effect to maintain temperatures warm enough to support liquid water. Hence, there is an ongoing debate between proponents of the "warm-and-wet" versus the "cold-and-dry" models. To address this, Steckel and her colleagues ran a computer simulation originally developed for Earth studies by Professor Tucker. As Steckel explained in a CU Boulder press release:

"You could pull up Google Earth images of places like Utah, zoom out, and you’d see the similarities to Mars. It’s very hard to make any kind of conclusive statement. But we see these valleys beginning at a large range of elevations. It’s hard to explain that with just ice."

The researchers used the software to model the evolution of the Martian landscape on synthetic terrain similar to Mars' equatorial region. They added water from precipitation to some of their models and melting ice caps to others, and then simulated how this would shape the landscape over tens to hundreds of thousands of years. The team then compared the two models to data obtained by NASA's Mars Global Surveyor (MGS) and Mars Odyssey spacecraft. The precipitation model was consistent with what we see around Mars' equator today.

These include the vast network of channels in the Martian highlands that open onto the low-lying areas in the Northern Lowlands. The rock deposits and delta fans found in these areas further indicate that vast quantities of water once flowed across the landscape. "You'd need meters deep of flowing water to deposit those kinds of boulders," said Hynek. "Once the erosion from flowing water stopped, Mars almost got frozen in time and probably still looks a lot like Earth did 3.5 billion years ago."

While these results are convincing, there are still unanswered questions about Mars' ancient climate. For example, scientists are still unsure how Mars could maintain temperatures warm enough to support precipitation and flowing water, given how the Sun's output was less than it is today. However, this study still provides scientists with a glimpse at what Mars experienced in the past and could also provide new perspectives into the geological history of Earth.

Further Reading:

• University of Colorado

Planetary scientists have plenty of theories about Mars and its environmental past. Two of the most widely accepted are that there was a carbon dioxide atmosphere and, at one point, liquid water on Mars' surface. However, this theory has a glaring problem: Where should the rocks have formed from the interactions between carbon dioxide and water? According to a new paper by scientists at several NASA facilities using data collected by the rover Curiosity, the answer is right under the rover's metaphorical feet.

According to geology, carbon dioxide and water should react together to form "carbonates," a type of mineral that contains an ion made up of carbon and oxygen. This process is relatively common on Earth and even in some manufacturing processes, but the results have never before been seen on Mars, at least not in any quantity.

That is despite a significant amount of effort spent looking for them. Rovers have looked for them to no avail. Even satellites have done spectroscopy on most of the planet and haven't seen anything that could be a carbonate anywhere near the quantities to prove that Mars had an atmosphere of carbon dioxide and liquid water at one time. That was, until the little rover that could stepped in.

Curiosity has had a hand in plenty of important discoveries on the Red Planet. Here's a video from Fraser 7 years ago that discusses some of them.

Curiosity has dug holes throughout Mars' Gale Crater for almost 13 years. During that time, some significant discoveries were made, but this latest one has dramatically impacted our understanding of the evolution of the Martian climate. At three different drill sites around Mount Sharp, Curiosity found evidence for a mineral called siderite, a carbonate material formed with iron.

Siderite itself wasn't present on the surface, though. It was only found when Curiosity drilled down 3-4cm into the surface of a rock and analyzed the resulting drill powder in its CheMin instrument. After the instruments zapped it with X-rays, the researchers found the presence of the elusive mineral that could explain where Mars' atmosphere went, at least partially. 

The presence of carbonates under layers of other rock could also explain why they have been so hard to find up until now. Orbiting satellites wouldn't be able to see a few centimeters into existing rock, and most rover spectroscopy is done without drilling into a sample, so they wouldn't have been able to detect it either. But finding any does lend credence to the idea that Mars used to be habitable for basic microorganisms, at one point at least.

Here's a look back at Curiosity's first science target - Jake the Rock.

Scientists from several different NASA centers, including the Jet Propulsion Laboratory (Curiosity operation), Ames Research Center (CheMin Instrument operation), and John Space Center (data analysis) contributed to the work. According to Benjamin Tutolo, a professor at the University of Calgary, "the discovery of abundant siderite in Gale Crater represents both a surprising and important breakthrough in our understanding of the geologic and atmospheric evolution of Mars." 

It certainly does, though the estimated amount of siderite and other carbonates based on this newest data isn't enough to explain where all of Mars' atmosphere went. There could be other, more abundant hiding places, or the Red Planet could have lost its atmosphere slowly over time due to the solar wind, since it has lacked a magnetic field for so long. As rovers continue to explore its surface, a steady stream of new findings will continue to intrigue planetary scientists, and hopefully help them refine their theories on how Mars came to be what it is today.

Learn More:

• NASA / JPL - NASA’s Curiosity Rover May Have Solved Mars’ Missing Carbonate Mystery
• Tutolo et al - Carbonates identified by the Curiosity rover indicate a carbon cycle operated on ancient Mars
• UT - Could There Be Bacteria Living on Mars Today?
• UT - It's Not Just Rocks, Scientists Want Samples Mars's Atmosphere

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NASA’s Lucy spacecraft made a successful flyby of the second asteroid on its must-see list over the weekend, and sent back imagery documenting the elongated object’s bizarre double-lobed shape.

It turns out that asteroid Donaldjohanson — which was named after the anthropologist who discovered the fossils of a human ancestor called Lucy — is what’s known as a contact binary, with a couple of ridges in its narrow neck. In today’s image advisory, NASA compares the ridged structure to a pair of nested ice cream cones.

“Asteroid Donaldjohanson has strikingly complicated geology,” said Hal Levison, a planetary scientist at the Southwest Research Institute who serves as the Lucy mission’s principal investigator. “As we study the complex structures in detail, they will reveal important information about the building blocks and collisional processes that formed the planets in our solar system.”

Lucy came as close as 600 miles (960 kilometers) to Donaldjohanson on April 20, snapping images every two seconds or so as it zoomed past. The pictures confirmed the asteroid’s status as a contact binary — that is, a compound object formed by the sticky collision of two smaller celestial bodies. Donaldjohanson is somewhat larger than it was previously thought to be, with a length of about 5 miles (8 kilometers) and a width of 2 miles (3.5 kilometers) at the widest point.

The Easter encounter took place three and a half years after Lucy was launched, and 17 months after the 52-foot-wide probe flew past its first target asteroid, Dinkinesh, and a mini-moon called Selam. Like Donaldjohanson, Selam was found to be a contact binary.

Researchers consider both of Lucy’s encounters in the main asteroid belt, which lies between the orbits of Mars and Jupiter, to be mere warmups for the mission’s main event: a detailed study of so-called Jupiter Trojan asteroids. Such asteroids are trapped harmlessly at resonance points in Jupiter’s orbit due to the giant planet’s gravitational influence. No spacecraft has ever gotten close to a Jupiter Trojan.

Tom Statler, NASA program scientist for the $989 million Lucy mission, said the quality of the early imagery demonstrates the “tremendous capabilities” of Lucy’s instruments. “The potential to really open a new window into the history of our solar system when Lucy gets to the Trojan asteroids is immense,” he said.

Over the next few weeks, researchers will retrieve, process and analyze data from Lucy’s black-and-white imager as well as its color imager, infrared spectrometer and thermal infrared spectrometer. The spacecraft is scheduled to spend most of this year traveling through the main asteroid belt.

Lucy’s first encounter with a Jupiter Trojan asteroid, known as Eurybates, is due to take place in August 2027. Four additional Trojan encounters will follow between 2027 and 2033.

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