Fifteen years after astronomers first confirmed the existence of buckminsterfullerene molecules in space, new observations from the James Webb Space Telescope are providing the clearest and most detailed view yet of the environment where these carbon structures form and evolve. The planetary nebula Tc 1, located more than 10,000 light-years away in the constellation Ara, has become one of the most important laboratories for studying complex carbon chemistry in space.

The new observations were led by researchers at Western University, including physicist and astronomer Jan Cami, whose team first identified buckyballs in Tc 1 using NASA’s Spitzer Space Telescope in 2010. That discovery confirmed a prediction made decades earlier by chemists studying carbon molecular structures and demonstrated that these molecules could form naturally in astrophysical environments.

Buckminsterfullerene, commonly referred to as a buckyball, is a molecular structure composed of 60 carbon atoms arranged in a hollow spherical geometry. The structure resembles a geodesic dome or a soccer ball, with a repeating pattern of pentagons and hexagons. The molecule was first synthesized in laboratory conditions in 1985 by Sir Harry Kroto and collaborators, work that later earned the 1996 Nobel Prize in Chemistry.

The significance of detecting these molecules in space extends beyond novelty. Carbon chemistry plays a central role in astrophysics because carbon is one of the primary elements involved in the formation of complex molecules. Understanding how carbon-based structures form and survive in harsh interstellar environments contributes to broader models of stellar evolution, dust formation, and the chemical enrichment of galaxies.

Tc 1 itself is a planetary nebula, a phase in stellar evolution that occurs when a low- to intermediate-mass star exhausts its nuclear fuel and sheds its outer layers. The exposed stellar core emits intense ultraviolet radiation that ionizes the surrounding gas, causing it to glow. Planetary nebulae are dynamic chemical environments where high-energy radiation, shock waves, and cooling gas interact to produce a wide range of molecules and dust grains.

The new JWST observations were conducted using the telescope’s Mid-Infrared Instrument, or MIRI. This instrument is optimized for wavelengths between approximately 5 and 28 microns, a spectral region particularly important for studying molecular vibrations and thermal emission from dust. Many carbon-rich molecules, including fullerenes, emit strongly in the mid-infrared, making MIRI an ideal tool for analyzing their distribution and physical properties.

The resulting image of Tc 1 combines observations from nine infrared filters spanning wavelengths from 5.6 to 25.5 microns. Because these wavelengths lie beyond the range of human vision, the image was processed into visible colors representing different thermal regimes. Shorter infrared wavelengths, associated with hotter gas, appear blue, while longer wavelengths tracing cooler material appear red. The processed image reveals a highly structured nebula containing filaments, shells, and radial features extending outward from the central star.

One of the most notable structures visible in the new image is a feature near the nebula’s center resembling an inverted question mark. While its physical origin is not yet understood, it highlights the complexity of the gas dynamics and chemistry occurring within the nebula. The morphology suggests that multiple interacting processes are shaping the environment, potentially including stellar winds, magnetic fields, and asymmetric mass loss from the dying star.

The scientific value of the JWST observations extends well beyond imaging. MIRI also collected spectroscopic data, allowing researchers to analyze the detailed chemical fingerprints of molecules and dust throughout the nebula. Spectroscopy works by separating incoming light into its component wavelengths, revealing characteristic emission and absorption features associated with specific molecules.

Each molecule interacts with electromagnetic radiation in a unique way because molecular bonds vibrate at characteristic frequencies. In the mid-infrared, these vibrational modes produce emission features that can be used to identify molecular species directly. The spectroscopic data from Tc 1 will allow astronomers to map the spatial distribution of buckyballs and investigate how these molecules interact with their surrounding environment.

One of the major scientific questions concerns why the fullerene emission in Tc 1 is unusually strong compared to other nebulae. Understanding this requires detailed modeling of excitation mechanisms, radiation fields, and local physical conditions. Researchers are investigating whether the brightness is driven primarily by ultraviolet excitation from the central star, interactions with dust grains, or specific chemical pathways unique to this environment.

The engineering capabilities of JWST are central to enabling these observations. Unlike previous infrared observatories, JWST combines a large segmented primary mirror with highly sensitive cryogenically cooled instruments. The telescope operates near the Sun-Earth L2 Lagrange point, where its sunshield continuously blocks heat from the Sun, Earth, and Moon. Maintaining extremely low operating temperatures is essential because infrared detectors are sensitive to thermal radiation generated by the telescope itself.

MIRI, in particular, requires active cooling to temperatures below 7 Kelvin. At these temperatures, detector noise is minimized, allowing the instrument to detect faint infrared signals from distant astrophysical sources. The telescope’s pointing stability and optical precision also contribute to the high spatial resolution visible in the Tc 1 observations.

Compared to the earlier Spitzer observations, JWST provides substantially improved sensitivity and angular resolution. Spitzer confirmed the existence of fullerenes in space, but JWST can now resolve the surrounding nebular structure in much greater detail and obtain higher-quality spectra across a broader wavelength range. This transition reflects the broader evolution of infrared astronomy from detection-focused observations toward detailed physical characterization.

The observations of Tc 1 are likely to remain scientifically important for years. The combination of imaging and spectroscopy provides a dataset capable of supporting multiple studies involving molecular chemistry, dust physics, and nebular dynamics. Researchers are currently preparing several scientific papers based on the observations, focusing on both the fullerene molecules themselves and the broader physical structure of the nebula.

More broadly, the work illustrates how astronomical observations connect chemistry, astrophysics, and instrumentation. Molecules first synthesized in terrestrial laboratories have now been observed in complex stellar environments thousands of light-years away. The same physical laws governing molecular vibrations on Earth operate throughout the galaxy, and increasingly sophisticated observatories are allowing those processes to be measured directly.

The new JWST observations of Tc 1 therefore represent more than a visually striking image. They provide a detailed view into the chemical and dynamical processes occurring around dying stars and expand understanding of how complex carbon molecules form and persist in space.

In December 2025, a comet discovered less than six months earlier passed close enough to Earth for astronomers to train their sharpest instruments on it. What they found was a surprise buried in ice: the water aboard 3I/ATLAS, the third confirmed interstellar comet to visit our solar system, carries a chemical fingerprint radically different from anything in our own planetary neighborhood. The finding, published in Nature Astronomy on April 23, 2026, has forced researchers to reconsider the assumption that our solar system’s water chemistry is representative of the galaxy at large.

The comet, formally designated C/2025 N1 (ATLAS), was first spotted by the Asteroid Terrestrial-impact Last Alert System in Chile on July 1, 2025. It reached perihelion on October 30, 2025, at a distance of 1.4 astronomical units from the Sun, and made its closest approach to Earth on December 19, 2025. Since then, outbound at roughly 210,000 kilometers per hour, it has been the subject of one of the most detailed compositional studies ever conducted on an interstellar object.

The work centered on the deuterium-to-hydrogen ratio in the comet’s water — a ratio that acts as a kind of chemical birth certificate. Deuterium, the heavy isotope of hydrogen with an extra neutron, becomes incorporated into water molecules under specific temperature and radiation conditions. Cold, undisturbed environments produce water with high D/H ratios. Warm, irradiated environments produce lower ratios. The ratio in Earth’s oceans, approximately 1.56 times 10 to the minus 4, has long served as a reference point for comparing planetary systems.

Using the Atacama Large Millimeter/submillimeter Array in Chile, a team led by Luis E. Salazar Manzano and Teresa Paneque-Carreño of Stockholm University observed the comet near perihelion and detected the signature of semi-heavy water, HDO. Normal water, H₂O, fell below detection thresholds. The researchers derived a conservative lower limit for the D/H ratio in the comet’s water of greater than 6.6 times 10 to the minus 3. This is more than 40 times the value found in Earth’s oceans and more than 30 times the typical value measured in Solar System comets.

The implication is stark. Either the protoplanetary disk that gave rise to our solar system was unusual in its water chemistry, or 3I/ATLAS formed in an environment far colder and more chemically pristine than the region where our comets were born. The most likely explanation is that the comet originated in the outer reaches of a planetary system where temperatures never rose above 10 to 20 Kelvin and radiation levels were minimal — conditions consistent with formation in a distant molecular cloud or the outer reaches of another star’s protoplanetary disk, perhaps billions of years ago.

The finding complicates the search for life beyond our solar system in ways that reach beyond cometary science. Water is considered essential for life as we understand it, and astronomers have long used the D/H ratio as a tracer for understanding where and how planets form. If our solar system’s water chemistry turns out to be an outlier rather than a norm, it means the conditions that gave rise to Earth’s oceans may be rarer than expected — and that the building blocks of life are distributed across the galaxy in more diverse configurations than models have historically assumed.

The distinction matters because it shifts the probability landscape for habitability. If most stellar systems form water with high D/H ratios like 3I/ATLAS, then the path from ice to ocean to life involves chemistry that our own system did not follow. If, instead, our system is typical and 3I/ATLAS is an outlier, then the conditions for water retention and planetary habitability may be common. The truth likely falls somewhere in between, but the current data cannot yet say where.

What is clear is that interstellar comets offer something no Solar System object can: a direct sample of material from another planetary system’s formation zone, unmodified by the gravitational and thermal processing that has reshaped everything in our own neighborhood. Each new interstellar visitor that astronomers can study adds another data point to a distribution we are only beginning to map. 3I/ATLAS is the third confirmed interstellar comet. The next one may tell us something different. The story of where water comes from in the galaxy is far from settled.

For most of human history, rivers have been measured locally. Water levels were monitored using gauges installed at specific locations, flow rates were estimated from field observations, and large sections of many river systems remained poorly observed or entirely unmeasured. Even today, vast portions of the world lack continuous hydrological monitoring infrastructure. This limitation has affected flood prediction, water resource management, climate modeling, and ecosystem studies for decades.

The Surface Water and Ocean Topography mission, commonly known as SWOT, is changing that. Developed jointly by NASA Jet Propulsion Laboratory and Centre National d’Études Spatiales, with contributions from the Canadian Space Agency and the United Kingdom Space Agency, the mission provides the first capability to continuously measure rivers and surface water systems globally from space at high spatial resolution.

The scientific importance of this capability is substantial. Rivers are dynamic systems that transport water, sediment, nutrients, and energy across continents. They connect mountain snowpacks, wetlands, forests, agricultural regions, cities, and coastal systems into a single hydrological network. Variations in river flow influence drinking water supplies, food production, hydroelectric generation, biodiversity, and flood risk. Yet despite their importance, comprehensive global measurements have remained incomplete because conventional monitoring depends heavily on ground-based instruments.

SWOT addresses this limitation through radar interferometry, a technique capable of mapping water surface elevations across wide swaths of Earth’s surface. Unlike traditional satellite altimeters, which measure elevation directly beneath the spacecraft along a narrow ground track, SWOT measures two-dimensional surface topography over broad areas. This allows the mission to observe rivers, lakes, reservoirs, wetlands, and coastal waters with much greater spatial coverage.

At the center of the spacecraft is the Ka-band Radar Interferometer, or KaRIn. The instrument operates by transmitting microwave radar pulses toward Earth and receiving the reflected signals using two antennas mounted at opposite ends of a long deployable boom. Because the antennas observe the same surface from slightly different positions, the returned signals contain phase differences related to surface elevation. By combining these measurements interferometrically, scientists can reconstruct detailed topographic maps of water surfaces.

The engineering required to achieve this precision is considerable. Surface elevation changes in rivers are often small, and the instrument must distinguish variations on the order of centimeters from orbit. This requires extremely accurate knowledge of the spacecraft’s position, orientation, and antenna separation. The deployable boom structure must remain mechanically stable despite thermal expansion and orbital stresses. Timing systems and signal processing algorithms must maintain phase coherence between the two radar channels.

SWOT operates in low Earth orbit, repeatedly surveying nearly all of the planet’s surface between approximately 78 degrees north and south latitude. As the satellite revisits river systems over time, it builds a dynamic record of changing water levels and surface extent. This temporal coverage allows researchers to observe seasonal flooding, drought development, sediment transport patterns, and long-term hydrological trends.

One of the mission’s key scientific advances is the ability to measure river slope continuously along large distances. River flow is fundamentally governed by differences in gravitational potential energy, which are reflected in water surface gradients. By mapping these gradients accurately, scientists can estimate discharge rates even in regions where no ground gauges exist. This represents a major improvement in hydrological modeling capability.

The observations are particularly valuable in remote and under-monitored regions. Large river systems such as the Amazon, Congo, and Mekong include areas where conventional measurements are sparse or difficult to maintain. SWOT provides a uniform observational framework that allows direct comparison between river systems worldwide.

The mission also contributes to climate science. Hydrological cycles are strongly influenced by climate variability and long-term warming trends. Changes in precipitation patterns, glacier melt, and evapotranspiration affect river behavior at continental scales. Continuous global measurements improve the ability of climate models to represent freshwater transport and storage, reducing uncertainty in future projections.

Flood forecasting is another major application. River floods develop through complex interactions between rainfall, upstream flow, terrain, and infrastructure. High-resolution measurements of water surface elevation and floodplain extent improve the initialization and validation of hydrodynamic models. This can enhance prediction accuracy and support emergency management efforts.

The engineering challenge extends beyond the spacecraft itself into data processing and distribution. SWOT generates large volumes of radar data that must be converted into scientifically usable products. Signal processing algorithms remove atmospheric effects, radar noise, and surface scattering artifacts. Water detection algorithms distinguish rivers and lakes from surrounding terrain. Calibration systems ensure long-term consistency across observations.

The resulting datasets include measurements of river width, surface elevation, slope, and spatial extent. Combining these measurements with hydrological models allows scientists to estimate discharge and water storage changes over time. The data are distributed to researchers worldwide, enabling applications across hydrology, ecology, climate science, and resource management.

The mission also highlights the increasing role of international collaboration in Earth observation. Large-scale hydrological monitoring requires expertise in radar engineering, orbital systems, geophysics, and computational science. Contributions from multiple space agencies allowed the mission to combine technical capabilities and scientific objectives into a unified observational system.

From a broader perspective, SWOT represents a transition in how freshwater systems are studied. Historically, river science relied heavily on point measurements and regional studies. SWOT introduces a planetary-scale observational framework where rivers can be monitored consistently across continents and over time. This changes not only the quantity of available data, but also the types of scientific questions that can be addressed.

Researchers can now analyze interactions between river systems and climate processes globally rather than locally. They can observe how drought propagates through watersheds, how floodplains evolve seasonally, and how human activities alter natural flow patterns. The continuity and spatial coverage of the measurements provide a level of context that was previously unavailable.

The Mississippi River, the Amazon, and thousands of smaller systems can now be studied within the same measurement framework. This consistency improves comparative analysis and strengthens the ability to identify large-scale hydrological trends.

In practical terms, SWOT provides a new observational capability for managing one of Earth’s most important resources: freshwater. Scientifically, it represents one of the most advanced applications of radar interferometry in Earth observation. By transforming rivers into continuously measured global systems, the mission expands both the scale and precision of hydrological science.

Video credit: NASA Goddard

Deep space missions have always faced a fundamental computing problem. The radiation-hardened processors that can survive the gauntlet of launch vibration, extreme temperature swings, and prolonged exposure to high-energy particles are typically decades behind the chips found in consumer electronics. A spacecraft navigating to Europa or steering a rover across the Martian surface operates with computing power that would have been unremarkable in a desktop computer from the early 2000s. The reason is reliability: space-grade hardware is built to tolerate radiation levels that would corrupt ordinary chips, and that tolerance comes at the cost of performance.

That constraint is now being tested. NASA’s High Performance Spaceflight Computing project, a collaboration between the agency’s Jet Propulsion Laboratory and Microchip Technology, is developing a radiation-hardened system-on-a-chip that promises to deliver up to 500 times the computational capacity of current spaceflight processors. Testing began at JPL in February 2026 and has proceeded with enough success that the team sent an email with the subject line “Hello Universe” — a deliberate nod to the test message that marked early computing milestones — to mark a symbolic milestone at the start of the campaign.

The processor, formally designated the PIC64-HPSC and built by Microchip Technology in Chandler, Arizona, is a multicore system-on-a-chip small enough to fit in the palm of a hand. Despite its compact size, it integrates central processing units, computational offloads, advanced networking units, memory, and input/output interfaces onto a single substrate — the same architecture found in modern smartphones, but engineered to survive conditions no consumer device could endure. The chip is designed to withstand total ionizing doses up to 100 kilorads, survive launch mechanical loads, and operate across temperature extremes that would cause consumer electronics to fail within seconds.

The performance leap comes from a combination of architectural advances and modern fabrication techniques. Current spaceflight processors like the RAD750, which flies on missions including the James Webb Space Telescope, operate at clock speeds measured in hundreds of megahertz. The new chip operates at significantly higher frequencies while maintaining the error correction and fault tolerance that radiation environments demand. The design uses multiple 64-bit RISC-V cores, a choice that balances computational density with the ability to tolerate single-event upsets — where a high-energy particle temporarily disrupts a transistor state — without corrupting mission-critical data.

The practical implications are substantial. A rover with access to this level of computing could run real-time terrain analysis using onboard neural networks, identifying hazards and adjusting course without waiting for commands from Earth. A spacecraft on a long-duration transit could process science data onboard rather than compressing it for transmission, extracting more value from each downlink window. A crewed vehicle could support more sophisticated life support monitoring and autonomous fault response — critical when the distance to Earth means a round-trip signal delay stretches into minutes or tens of minutes.

The test campaign at JPL subjects the chip to simulated space conditions including radiation exposure, thermal cycling, mechanical shock, and electromagnetic interference. High-fidelity landing scenarios from actual NASA missions are being used to evaluate real-world performance under load. Results so far have been consistent with design expectations, and the team has verified that the chip operates at the performance levels projected.

What makes the High Performance Spaceflight Computing project notable beyond raw performance is its commercial structure. NASA selected Microchip as a partner in 2022, and the company funded its own research and development alongside NASA investment. Early access samples have been provided to defense and commercial aerospace partners, suggesting that the technology will flow into multiple programs rather than being confined to NASA missions. The broader aerospace industry, including aviation and automotive manufacturers, has expressed interest in adapted versions for radiation-tolerant Earth-based applications.

The chip is not yet flight certified. The ongoing test campaign will run for several more months, and results will inform the qualification process for specific mission profiles. Once certified, the processor will be incorporated into computing hardware for Earth orbiters, planetary rovers, crewed lunar and Martian hardware, and deep space probes. The intent is for the technology to become a standard building block across NASA’s fleet, enabling a new generation of autonomous spacecraft that can think — and react — without waiting for Earth to tell them what to do.

On May 13, 2026, NASA published new details about the Artemis 3 mission and the changes were striking enough to warrant attention not for what they added, but for what they removed. The mission, originally planned as the first crewed lunar landing since Apollo 17, will now send four astronauts to low Earth orbit aboard the Space Launch System and have them dock with prototype lunar landers. No landing. No lunar surface. The Moon is gone from the mission.

The agency confirmed that Artemis 3 will launch from Kennedy Space Center’s Launch Complex 39B no earlier than late 2027, and that the SLS rocket will fly without its usual upper stage. Instead of the Interim Cryogenic Propulsion Stage, the upper stage that has carried Orion to the Moon on previous flights, NASA will install an inert structural spacer — essentially a hollow cylinder with the same mass, dimensions, and interface geometry as the ICPS. The spacer preserves the rocket’s aerodynamic and structural characteristics without consuming propellant that could be allocated elsewhere.

The reason for the change is straightforward: the lunar landers are not ready. SpaceX’s Starship Human Landing System and Blue Origin’s Blue Moon have both experienced development delays. A crewed lunar landing requires those vehicles to perform rendezvous and docking in lunar orbit, execute a descent to the surface, support a stay of variable duration, and then launch back to rendezvous with Orion. Each step involves systems that have not yet been demonstrated in the configuration needed for crewed operations. NASA, having learned hard lessons from the heat shield anomalies encountered on the Artemis 2 flight in April 2026, decided it would not also accept the risk of an unproven lander.

The restructured Artemis 3 instead serves as what the agency describes as a dress rehearsal — similar in concept to Apollo 9, which tested the lunar module in Earth orbit before the first Moon landing. Four astronauts will launch on the Block 1 SLS configuration, which consists of the core stage and twin solid rocket boosters. Orion will separate from the stack and the crew will spend extended time aboard the spacecraft, testing rendezvous and docking with one or both lander prototypes in the relatively safe environment of low Earth orbit, approximately 463 kilometers above Earth at a 33-degree inclination. The European Service Module that powers Orion will handle orbital raising and maneuvering, with the ICPS being preserved for Artemis 4.

The hollow spacer solution was driven in part by hardware availability. The supply of ICPS stages is limited, having been built for the first three Artemis missions, and transitioning to the Exploration Upper Stage on later Block 1B configurations is still years away. Using the final ICPS on Artemis 4 rather than consuming it on an Earth-orbit test mission makes sense from a launch vehicle economics perspective. The spacer, being fabricated at NASA’s Marshall Space Flight Center in Huntsville, Alabama, maintains the structural interface between the Orion stage adapter and the launch vehicle stage adapter while costing nothing in propellant mass.

Artemis 4 remains targeted as the first crewed lunar landing, currently scheduled for no earlier than 2028, and will use the first ICPS from the original batch. The lander situation will need to be resolved by then. SpaceX is expected to conduct an uncrewed Starship HLS test flight before committing a crewed variant. Blue Origin is targeting an end-of-2026 launch of its Blue Moon Pathfinder MK1, an uncrewed cargo mission to validate the BE-7 engine, precision landing systems, and surface operations. Both companies face continued schedule pressure, and the May 2026 grounding of Blue Origin’s New Glenn rocket following an April 19 second-stage failure adds a further complication for Blue Moon’s path to orbit.

The decision to strip the landing from Artemis 3 drew predictable criticism from observers who saw it as another in a long series of delays. But the engineering logic is sound. Artemis 2’s heat shield erosion, traced to an arc-jet test anomaly and now requiring a redesigned thermal protection system for the Orion capsule, consumed program schedule margin. Adding a lunar landing with unproven vehicles on top of a heat shield redesign would have compounded risk in a domain where the cost of failure is measured in human lives. Moving the landing to Artemis 4 preserves schedule integrity for the test flight while keeping the lunar surface objective alive.

The Artemis program has always been a慢 exercise in managed ambition. The original Constellation program was canceled in 2010. The SLS was ordered to replace shuttle hardware that did not exist. The lunar landing has been pushed back repeatedly as funding, politics, and engineering complexity have collided. Stripping Artemis 3 to an Earth-orbit test is not a sign of weakness. It is a sign that the program has decided, perhaps for the first time, to let engineering reality set the schedule rather than politics.

Aircraft are most vulnerable during takeoff and landing. At these lower speeds, wings must generate significantly more lift than during cruise flight while maintaining stability and control close to the ground. This phase of flight places complex aerodynamic demands on the aircraft, particularly around the wing surfaces, flaps, and slats collectively known as high-lift systems. Understanding how air behaves around these structures is one of the most challenging problems in aerospace engineering.

To address this problem, NASA and its international research partners are using a shared experimental and computational framework known as the High Lift Common Research Model, or CRM-HL. The project provides a standardized wing and aircraft geometry that can be tested across multiple wind tunnels, simulation platforms, and research institutions. By using the same baseline design everywhere, researchers can directly compare results from different facilities and computational methods, improving confidence in the accuracy of aerodynamic predictions.

The effort reflects a broader challenge in modern aerospace engineering. Computational fluid dynamics, or CFD, has become one of the primary tools for aircraft design. Engineers now rely heavily on large-scale simulations to predict airflow behavior around aircraft before physical prototypes are built. However, CFD models are only as reliable as the assumptions, turbulence models, and numerical methods underlying them. Small differences in simulation setup or experimental conditions can produce different results, especially in highly turbulent flow regimes such as those encountered during takeoff and landing.

The High Lift Common Research Model was created to reduce this uncertainty by establishing a common reference geometry for validation studies. The model includes realistic high-lift devices such as deployed flaps and slats, allowing researchers to study airflow structures representative of actual transport aircraft configurations. Because the geometry is shared internationally, multiple organizations can independently analyze the same aerodynamic problem using their own tools and facilities.

The physics involved in high-lift aerodynamics is significantly more complicated than cruise flight. During cruise, airflow around a wing is relatively smooth and attached, meaning the air follows the contour of the wing surface. At low speeds, however, wings must operate at higher angles of attack to generate sufficient lift. This increases the risk of flow separation, where the airflow detaches from the wing surface and becomes highly turbulent.

High-lift devices help manage this problem. Slats on the leading edge of the wing allow air to flow through narrow gaps, energizing the boundary layer and delaying separation. Flaps on the trailing edge increase the wing’s effective curvature and surface area, allowing greater lift generation at lower speeds. These devices create highly three-dimensional flow structures involving vortices, shear layers, and turbulent wakes.

Capturing these phenomena accurately is difficult both experimentally and computationally. Wind tunnel testing remains one of the most important tools for studying complex aerodynamic behavior. Scaled physical models are placed in controlled airflow environments where sensors measure pressure distribution, lift, drag, and flow structure. Advanced visualization techniques such as particle image velocimetry and pressure-sensitive paint can reveal detailed flow patterns across the wing.

The CRM-HL tests include models at various scales, including a 5.2% scale version used for detailed aerodynamic studies. Scaling introduces its own engineering considerations because aerodynamic similarity depends on dimensionless parameters such as Reynolds number and Mach number. Researchers must carefully design test conditions to ensure that scaled models reproduce the relevant physical behavior of full-size aircraft as closely as possible.

Computational simulations complement these physical experiments. CFD software divides the airflow around the aircraft into millions or even billions of small computational cells. The governing equations of fluid motion—the Navier-Stokes equations—are then solved numerically across this grid. These equations describe conservation of mass, momentum, and energy within the fluid.

Directly resolving all turbulent scales in realistic aircraft flows is computationally impractical for most engineering applications. Instead, researchers use turbulence models to approximate the effects of smaller turbulent structures. Different turbulence models can produce different results, particularly in separated flow regions, which is one reason cross-validation against experimental data is essential.

The CRM-HL project allows researchers to compare computational predictions against wind tunnel measurements under controlled conditions. If multiple independent CFD approaches converge toward the same results and match experimental data, confidence in those methods increases. Discrepancies help identify limitations in modeling approaches and guide improvements in numerical techniques.

One of the major benefits of the project is standardization across facilities. Different wind tunnels have different wall effects, flow quality characteristics, and instrumentation systems. Similarly, computational platforms may use different mesh generation strategies, solvers, and turbulence models. By applying all of these methods to the same geometry, researchers can isolate the influence of methodological differences and improve consistency across the aerospace industry.

This collaborative approach is increasingly important as aircraft design becomes more dependent on digital engineering workflows. Modern aerospace programs aim to reduce the number of expensive physical prototypes by relying more heavily on validated simulations during early design phases. Accurate CFD tools can shorten development timelines, reduce costs, and allow engineers to explore a wider range of configurations before committing to manufacturing.

The research also contributes directly to operational improvements. Better understanding of airflow during takeoff and landing can lead to more efficient wing designs, reduced fuel consumption, lower noise levels, and improved safety margins. High-lift systems influence runway performance, stall behavior, and handling characteristics, all of which are critical for commercial aviation.

The simulations produced within the CRM-HL effort provide additional insight into the detailed structure of airflow. Visualizations reveal vortices forming near flap edges, turbulent mixing regions behind deployed surfaces, and pressure gradients across the wing. These features are difficult to measure comprehensively in physical tests alone, making computational analysis a valuable complement.

At a broader level, the project reflects the evolving relationship between experimentation and simulation in aerospace engineering. Wind tunnels remain essential because they provide empirical validation, but computational tools increasingly allow engineers to study phenomena in ways impossible through testing alone. The combination of both approaches creates a more complete understanding of aerodynamic systems.

The High Lift Common Research Model therefore serves not only as a wing design, but as a shared scientific framework. It allows researchers across countries and institutions to evaluate methods against a common reference point, improving the reliability of aerodynamic prediction tools used throughout the aerospace industry.

As aircraft become more efficient and design margins become tighter, this type of coordinated validation effort becomes increasingly important. The airflow around a wing during landing may appear simple from a distance, but in reality it involves some of the most complex fluid dynamics encountered in engineering. Understanding that airflow with precision is essential to the next generation of aircraft design.

Video credit: NASA

For decades, the assumption among planetary scientists was straightforward: small bodies in the outer solar system are too cold, too low in gravity, and too distant from the Sun to hold onto any significant atmosphere. Pluto had been known to have one since the 1980s, but Pluto is large — roughly 2,400 kilometers in diameter, large enough to retain a thin nitrogen atmosphere through a combination of low temperature and sufficient surface gravity. The same was assumed to be true for Eris and Makemake, the other dwarf planets in the Kuiper Belt. But small trans-Neptunian objects, the hundreds of thousands of bodies that orbit beyond Neptune, were expected to lack atmospheres entirely.

On May 4, 2026, a team led by Ko Arimatsu at the National Astronomical Observatory of Japan published a paper in Nature Astronomy reporting the detection of an atmosphere on the trans-Neptunian object (612533) 2002 XV93. The discovery changes that assumption.

2002 XV93 is a plutino — a class of trans-Neptunian objects that orbit in a 3:2 resonance with Neptune, completing two orbits for every three that Neptune makes. It is roughly 500 kilometers in diameter, about one-fifth the size of Pluto, and at the time of the observation it was approximately 5.5 billion kilometers from Earth. The detection method was a stellar occultation: the team observed the asteroid passing in front of a distant star, measuring how the starlight dimmed as 2002 XV93 moved across the line of sight. In an ordinary occultation by an airless body, the starlight drops abruptly and recovers in the same way. In this case, the dimming was gradual, stretching over roughly 1.5 seconds as the star passed through the atmosphere, its light refracted by gas surrounding the small body.

The surface pressure was estimated at 100 to 200 nanobars — roughly 100 times less than Pluto’s atmosphere, and 50 to 100 million times less than Earth’s sea-level pressure. At temperatures of 40 to 50 kelvin, nitrogen and methane ices on the surface could be in a state of slow sublimation, releasing gas into a thin envelope around the body. But the pressure measurement raises an immediate question: at 500 kilometers across, 2002 XV93 should not be able to hold onto an atmosphere for long. Its surface gravity is too weak to retain gas against the thermal escape processes that drain atmospheres into space. An atmosphere at this pressure should dissipate within roughly a thousand years.

Two possible explanations have been proposed. The first is cryovolcanism — ice eruptions on the surface that continuously replenish gas lost to space, maintaining a steady-state atmosphere through ongoing geological activity. The second is a recent impact event that cracked the interior and released volatiles that are currently slowly escaping. JWST observations have found no detectable surface gases, adding a layer of mystery to the finding. The team acknowledges that the atmosphere may be transient, a short-lived phenomenon that will not persist on astronomical timescales.

The scientific significance is not limited to 2002 XV93 itself. The detection demonstrates that small TNOs can retain atmospheres under conditions that models had suggested were prohibitive. If cryovolcanism is the mechanism, it implies that these distant worlds are more geologically active than previously believed. Other dwarf planets and large TNOs may harbor similar transient atmospheres that have simply not been observed yet. The finding redefines the boundary between airless and atmosphere-bearing bodies in the outer solar system.

The discovery also showcases the power of stellar occultation surveys, which can detect atmospheric signatures that would be invisible to direct telescopic observation. Arimatsu’s team used observations from multiple Japanese sites, including telescopes operated by amateur astronomers, to triangulate the geometry and measure the pressure gradient. The approach demonstrates that targeted occultation surveys can characterize the atmospheres of small bodies at distances where direct sensing is impractical.

The condition for a body to retain an atmosphere against thermal escape is determined by the ratio of gravitational binding energy to the thermal energy of gas molecules. For Earth-temperature conditions, hydrogen and helium escape readily because their molecules move at velocities that approach or exceed the body’s escape velocity. At 40 to 50 kelvin, however, the average molecular velocity is much lower, and only light gases like hydrogen and helium are prone to rapid escape. Nitrogen and methane, being heavier molecules, have lower average velocities at the same temperature, making them more readily retained.

The escape velocity from 2002 XV93 is roughly 0.2 kilometers per second — tiny compared to Earth’s 11.2 kilometers per second. At 50 kelvin, the mean thermal velocity of nitrogen molecules is about 0.14 kilometers per second, which is a substantial fraction of the escape velocity. This means that nitrogen molecules at the top of the atmosphere are not strongly bound, and a continuous supply mechanism is required to maintain the observed pressure. The Jean’s escape parameter, which quantifies the fraction of molecules with velocities exceeding escape velocity, is close to unity for this body — a marginal condition that explains why the atmosphere is so thin.

The discovery of an atmosphere on 2002 XV93 adds a new dimension to the taxonomy of trans-Neptunian objects. Where they were once categorized by size, orbital class, and surface color, the possibility of atmospheric activity introduces a geologically active category that was previously unknown beyond the realm of the gas and ice giants. The outer solar system is more complicated, and more interesting, than the textbooks suggested.

In the early hours of March 17, 2026, engineers at the European Space Agency watched as a spacecraft roughly 1.6 billion kilometers away executed the largest trajectory correction of its mission. Hera’s three main engines fired in sequence over several hours, consuming 123 kilograms of hydrazine propellant and delivering a velocity change of 367 meters per second. The maneuver aligned the spacecraft’s solar orbit inclination with that of the Didymos binary asteroid system, confirming that the probe remains precisely on course for its rendezvous in November. Hera will spend the coming months quietly cruising toward a planetary science milestone that researchers have been anticipating since September 2022, when NASA deliberately collided a spacecraft with a small moonlet called Dimorphos.

The DART mission, Double Asteroid Redirection Test, impacted Dimorphos on September 26, 2022, at approximately 6.1 kilometers per second. The collision was not designed to destroy the asteroid but to test whether kinetic energy transferred from a spacecraft could measurably alter the orbit of a body around its parent asteroid. Scientists estimated the impact would shorten Dimorphos’s orbital period around Didymos by roughly 10 percent, a change that ground-based telescopes began measuring within days. The initial finding of approximately 32 minutes shortening was striking enough to declare the test a success, but the full picture required more time and more data to emerge.

In March 2026, NASA announced the conclusion of a multi-year analysis combining radar observations, ground-based telescope measurements, and 22 stellar occultations recorded by volunteer astronomers worldwide. The results confirmed not only that Dimorphos’s orbital period around Didymos shortened by approximately 33 minutes but also that the entire binary system’s orbit around the Sun changed in a measurable way. The Didymos-Dimorphos system’s 770-day solar orbit shortened by approximately 0.15 seconds per revolution, and its orbital speed increased by roughly 11.7 microns per second. The mechanism behind the solar orbit change differs from the immediate transfer of momentum during the impact. Instead, the effect arises from the substantial ejection of rocky debris from Dimorphos following the collision. When the DART spacecraft struck Dimorphos, it displaced millions of kilograms of material that accelerated away from the asteroid in various directions. The conservation of momentum in the system meant that the ejected debris carried away additional orbital energy, effectively acting as a secondary propulsion event. The phenomenon is called momentum enhancement, and the DART results indicate it approximately doubled the net impulse delivered to the asteroid compared to the spacecraft’s own momentum alone.

The 22 stellar occultations that contributed to the measurement illustrate an elegant form of interplanetary science that requires no spacecraft at all. When an asteroid passes in front of a distant star as seen from Earth, the star’s light dims in a characteristic pattern that encodes information about the asteroid’s size, shape, and orbital position. Volunteer astronomers using commercially available equipment recorded these events across multiple continents between October 2022 and March 2025, building a dataset precise enough to detect changes in Dimorphos’s trajectory measured in meters per second. The coordination required to time these observations across dozens of sites reflects the kind of international scientific collaboration that planetary defense has increasingly attracted.

The binary nature of the Didymos-Dimorphos system added complexity to the analysis because the two bodies orbit each other while together orbiting the Sun. Changes in the internal orbital period affect the center of mass of the system, which in turn affects how the system responds to external gravitational influences. Researchers found that the momentum enhancement from debris ejection altered the binary orbit in ways that rippled outward to change the system’s solar orbit. This had never been directly measured before and provides a data point that asteroid deflection models had predicted but never confirmed.

Hera’s mission now is to examine the aftermath of this event at close range. The spacecraft carries two CubeSats named Juventus and Milani that will deploy upon arrival to conduct complementary measurements. Juventus will use a tri-axial magnetometer and a susceptibility probe to characterize Dimorphos’s internal composition and magnetic properties, while Milani will conduct spectroscopic analysis of the asteroid’s surface to map mineralogy and search for organic compounds. The primary spacecraft will map the DART impact crater in high resolution, measure the mass of Dimorphos through subtle gravitational effects on Hera’s trajectory, and characterize the surface morphology that resulted from the collision and subsequent debris cascade.

The approach phase beginning in October 2026 represents the highest-risk period of the mission aside from arrival itself. Hera’s onboard software will use its asteroid framing cameras to autonomously detect and track Didymos and Dimorphos during the three-week approach, a capability that has been tested in simulations but never validated in the actual environment. The navigation challenge is compounded by the binary system’s mutual orbit, which means both bodies are moving relative to each other at velocities that require the spacecraft’s guidance system to track two objects simultaneously. Engineers have uploaded software updates during the cruise phase to prepare for these operations, and mission controllers will monitor the process from ESA’s European Space Operations Centre in Darmstadt.

Understanding why DART produced effects extending to the solar orbit requires examining the three-body dynamics that govern binary asteroid systems. When two objects orbit each other, their motions are governed by their mutual gravitational attraction, which depends on their masses and the distance between them. The impact by DART altered the orbital velocity of Dimorphos, which changed the balance of forces in the binary system. This in turn changed the rate at which the two bodies orbit each other, and the resulting shift in the location of the center of mass altered the system’s overall momentum.

The momentum enhancement factor of approximately 2 observed in the DART results has significant implications for the design of future deflection missions. If a spacecraft impact can deliver twice the expected momentum transfer through debris ejection, then smaller missions could achieve the same deflection effect, reducing launch mass requirements and mission costs. However, the magnitude of the enhancement depends on the surface properties of the target asteroid, which vary considerably. Loose rubble pile asteroids like Dimorphos produce more debris than solid rock bodies, making the enhancement factor difficult to predict for new targets.

The crater formed by DART on Dimorphos will provide direct evidence of the surface response to hypervelocity impact. The crater size and shape encode information about the target’s material properties, including its tensile strength, porosity, and layering. Hera’s high-resolution camera will resolve features down to a few meters, allowing scientists to compare the observed crater with pre-impact predictions and refine impact models for future use.

Roughly 1,000 light-years from Earth, astronomers have identified an enormous protoplanetary disk surrounding a young star system, a structure so large that it extends nearly 400 billion miles across. Nicknamed “Dracula’s Chivito,” the disk is now recognized as the largest protoplanetary disk ever imaged in visible light, offering astronomers a rare opportunity to study the early stages of planetary system formation on an unusually large scale.

The name itself reflects the backgrounds of the researchers involved in the discovery. One astronomer came from Transylvania, historically associated with Dracula, while another came from Uruguay, where the chivito sandwich is considered a national dish. Despite the playful nickname, the scientific significance of the object is substantial. The disk provides a direct observational window into the processes that shape young planetary systems and may help researchers better understand how systems like our own Solar System formed billions of years ago.

The observations were made using the Hubble Space Telescope, whose optical resolution and long operational history continue to make it one of the most important instruments for studying circumstellar environments. Protoplanetary disks are difficult observational targets because they are composed largely of diffuse gas and dust surrounding extremely bright young stars. Imaging them requires both high spatial resolution and careful control of scattered light.

A protoplanetary disk forms during the early stages of star formation. As a molecular cloud collapses under gravity, conservation of angular momentum causes the infalling material to flatten into a rotating disk around the newly forming star. Over time, dust grains within the disk collide and aggregate into progressively larger bodies, eventually forming planetesimals and planets. Gas dynamics, turbulence, magnetic fields, and gravitational interactions all influence this evolution.

Dracula’s Chivito stands out primarily because of its scale. The disk extends approximately 40 times farther than the diameter of our Solar System measured out to the Kuiper Belt. At these distances, the physical conditions differ substantially from those in the inner regions of more typical protoplanetary disks. Material density decreases, orbital periods become extremely long, and interactions with the surrounding interstellar environment may become increasingly important.

The disk was observed nearly edge-on from Earth’s perspective, a geometry that is scientifically useful because it enhances visibility of the dust structure. In edge-on systems, the dense central plane of dust blocks direct starlight, allowing the surrounding scattered light to reveal the disk’s shape and vertical structure. Hubble’s imaging shows a dark central lane surrounded by extended illuminated material, tracing the distribution of dust particles suspended above and below the disk midplane.

The science behind these observations involves the interaction between starlight and microscopic dust grains. Dust particles scatter and absorb light depending on their size, composition, and spatial distribution. By analyzing the brightness and structure of the scattered light, astronomers can estimate properties such as particle size distribution, disk thickness, and density gradients.

One important question concerns the stability of such a large disk. At extreme distances from the central star, the gravitational influence of the star weakens, making the outer regions more susceptible to disruption from nearby stars, interstellar gas clouds, or internal instabilities. Studying these outer regions helps researchers test models of disk evolution and understand the limits of planet formation processes.

The observations may also provide insight into how giant planets form at large orbital distances. Traditional models of core accretion become less efficient farther from the star because material densities are lower and orbital timescales are longer. Alternative formation mechanisms, such as gravitational instability within the disk itself, may play a larger role in these environments. Detailed imaging of large disks like Dracula’s Chivito helps constrain these theoretical models.

From an engineering perspective, capturing this image required both the optical stability of Hubble and advanced image-processing techniques. The telescope operates above Earth’s atmosphere, avoiding atmospheric turbulence that would otherwise blur fine structures. Hubble’s pointing system maintains extremely stable alignment during long exposures, allowing faint scattered light from the disk to be resolved against the much brighter central star.

Image processing is equally important. Observations of circumstellar disks often require subtraction of residual starlight and instrumental artifacts to reveal faint surrounding structures. Calibration procedures remove detector noise, cosmic ray events, and optical distortions. Multiple exposures may be combined to improve signal-to-noise ratio and recover subtle features in the disk.

The scale of the disk also emphasizes the diversity of planetary systems in the galaxy. Early models of planetary formation were strongly influenced by the architecture of the Solar System because it was the only known example. Modern observations have shown that planetary systems exhibit enormous variation in size, orbital structure, and composition. Some contain tightly packed planets orbiting close to their stars, while others possess extended debris structures spanning hundreds of billions of miles.

Dracula’s Chivito contributes to this broader picture by demonstrating that protoplanetary disks themselves can exist at scales much larger than previously observed. Understanding how such systems evolve may help explain the origin of wide-orbit planets and extended debris populations detected around other stars.

The observations also highlight the continued scientific relevance of Hubble more than three decades after launch. Although newer observatories such as the James Webb Space Telescope provide expanded infrared capabilities, Hubble remains highly effective for visible-light imaging of circumstellar structures. The combination of optical and infrared observations allows astronomers to study both scattered starlight and thermal emission from dust, providing complementary information about disk composition and structure.

Future observations may further refine understanding of the system. Spectroscopic analysis could help determine the chemical composition of the disk material, while higher-resolution infrared observations may reveal substructures such as gaps, rings, or asymmetries associated with forming planets. Long-term monitoring could also detect dynamical evolution within the disk over time.

In practical terms, Dracula’s Chivito is a large-scale example of processes believed to have shaped the early Solar System. The disk represents a phase in stellar evolution where gas and dust are actively organizing into more complex structures that may eventually produce planetary systems. By observing such systems directly, astronomers can compare theoretical models with real physical environments.

The discovery provides a detailed observational dataset for studying how stars and planets form together, how disks evolve over time, and how diverse planetary systems can become under different initial conditions.

Video credit: NASA Goddard

SpaceX has set no earlier than May 19, 2026, for the first flight of Starship in its Version 3 configuration, a significant step in the development of the vehicle that NASA has contracted to land astronauts on the Moon and that SpaceX intends to use for missions to Mars. The upcoming flight, designated Flight 12, will lift off from Starbase in South Texas with a window opening around 5:30 to 6:30 p.m. ET, with a backup opportunity on May 20 if weather or technical issues require it.

The Version 3 configuration represents the most capable iteration of the Starship and Super Heavy system yet built. The vehicle stands approximately 150 meters tall with the upper stage stacked on the booster, making it the largest flying object ever constructed. The Super Heavy booster carries 33 Raptor engines — the full complement — compared to the 33-engine configuration that flew in earlier tests, but V3 introduces upgraded engines with higher thrust output and improved longevity. The upper stage, Ship 39, carries the same engine count as its predecessors but benefits from the thermal protection and reusability improvements that the SpaceX team has refined through the program’s rapid iteration cycle.

On May 11 and 12, SpaceX completed a full launch rehearsal that included propellant loading and a 33-engine static fire of Booster 19 with Ship 39 stacked on top. The test was the first time V3 hardware had been subjected to a full-duration static fire with all engines firing simultaneously, and it verified the vehicle’s readiness for flight conditions. The rehearsal included loading cryogenic propellants — liquid oxygen and liquid methane — into both stages, a process that takes hours and involves managing thermal gradients and boil-off rates that are significantly more complex for a vehicle of Starship’s scale than for any prior rocket.

The May 19 target has been in development for several weeks. SpaceX had originally planned an earlier V3 debut but chose to extend the testing and validation phase after discovering a hardware issue during pre-flight inspections. The conservative approach reflects a pattern the company has followed throughout the Starship program: when something does not look right, the team stops, diagnoses, and fixes rather than proceeding and hoping for the best. The strategy has produced a flight rate that is slower than early projections suggested, but it has also produced a vehicle that, by the time it flies, has been tested against the conditions it will actually face.

Flight 12 will be the first Starship flight of 2026 and the twelfth overall test flight in the program’s history. SpaceX has been flying approximately one Starship mission every few months as the vehicle matures, with each flight serving as both a test of new hardware and a demonstration of capabilities that have been validated in previous flights. The Version 3 hardware will attempt to complete the full mission profile: a full-duration burn of both stages, a controlled descent of the booster back toward the launch site where it will be caught by the mechanical arm system, and an upper stage that will perform a controlled splashdown in the Indian Ocean after completing one or more orbits of Earth.

The vehicle’s role in NASA’s Artemis program gives the program a significance that extends beyond SpaceX’s own ambitions. The Human Landing System contract that NASA awarded to Starship requires the vehicle to demonstrate crewed lunar landing capability before astronauts from the Artemis III mission descend to the lunar surface. That demonstration is years away, but the hardware being tested in the V3 flights is the same hardware that will eventually attempt the lunar descent. Each test flight, even if it ends in a loss of vehicle, produces data that refines the engineering and reduces the risk of the crewed mission later.

The May 19 window is specific enough that it suggests the team has high confidence in the timeline, but not so specific that it implies a guarantee. SpaceX has shown, repeatedly, that it will delay a launch rather than fly a vehicle it has reason to doubt. For a rocket program that has redefined what rapid iteration means in aerospace, the patience to wait for the right conditions is not a contradiction — it is the discipline that makes the iteration sustainable.

Super Heavy’s 33-engine first stage is a study in the engineering trade-offs that define modern launch vehicle design. Each Raptor engine produces a specific thrust at sea level, and the total thrust at liftoff is the sum of all 33 engines burning simultaneously. The challenge is not generating that thrust but managing the physical interactions between engines, the structure, and the propellant flow at the scale Super Heavy requires.

The Raptor engine uses a full-flow staged combustion cycle, which means that all of the fuel and oxidizer are gasified before they enter the combustion chamber. This approach produces very high efficiency — specific impulse in the range of 380 seconds at sea level — but it requires turbomachinery that can handle extreme temperatures and pressures without failing. The engineering challenge is not just the performance but the durability: an engine that will be fired multiple times must maintain its tolerances across many cycles of heating and cooling, which is why the V3 engines include upgrades to materials and cooling passages that extend engine life.

At liftoff, the structural loads on Super Heavy are enormous. The vehicle weighs approximately 4,000 metric tons at full propellant, and the acceleration from zero to thousands of meters per second in a few minutes requires structural integrity in the airframe that can withstand both the axial loads along the body and the bending moments produced by the aerodynamic forces acting along the vehicle’s length. The stainless steel construction that SpaceX chose for Starship is not a cost-cutting measure but an engineering decision that trades away the weight efficiency of carbon composites for the fracture toughness and reusability of a material that can survive the thermal and structural extremes of repeated flights without developing the microcracks that compromise composite structures over time.

The catch mechanism — the mechanical arms at the launch tower that are designed to catch the returning booster rather than landing it on legs — remains one of the more ambitious elements of the Starship reusability architecture. The system requires precise trajectory control during descent, a structure on the booster that can interface with the catcher arms, and software that can execute the maneuver reliably at the end of a ballistic arc. The May 19 flight will be the first V3 attempt at this catch, and whether the system works on the first try or requires iteration will define the timeline for the operational reusability that SpaceX has designed the vehicle around.