OrbitalHub

On the morning of August 28, 2026, in an engineering building on the campus of the University of Alabama in Tuscaloosa, fourteen teams competed in the finale of NASA’s LunaRecycle Challenge. The contestants included graduate students, hobbyists, a Wyoming aerospace LLC, an Austin 3D-printer company, and a doctoral cohort from MIT that calls itself CERBERUZ. None of them were building rockets or rovers. They were building trash compactors. The wrinkle: the trash had to be turned back into useful parts, on the Moon, in vacuum, in partial gravity, without resupply shipments from Earth.

Their brief was deceptively ordinary. Take a kilogram of dirty foam, plastic bags, Nomex flight jackets, and aluminum food wrappers — the kind of stuff astronauts throw away every day — and turn it into something a habitat can actually use. The competition carried a $3 million purse, a 1,200-team applicant pool, and a NASA program manager who announced the winners live at noon, CDT (NASA Centennial Challenges, August 28 2026).

Astronauts on the International Space Station produce roughly 2.5 kilograms of “non-metabolic” trash per crew member per day — packaging, food pouches, hygiene items, clothing offcuts, broken equipment. On the ISS, most of that ends up loaded onto a Progress cargo freighter and incinerated in the atmosphere. For a Mars mission lasting two and a half years, you can’t do that. For a permanent Artemis Base Camp on the lunar south pole, you can’t do that either, because every kilogram launched from Earth currently costs somewhere in the high five figures by the time it sits on the regolith.

The economics flip if you can keep what you bring. Recycling turns an “input” into a “stockpile.” Foam becomes a habitat tile. A torn glove becomes feedstock for a replacement bracket. The MIT team’s prototype grinds mixed waste into powder, then extrudes it into filament for a 3D printer or pellets for an injection mold. The first-place prize money — $500,000 for the prototype, $275,000 for the digital twin — is small change compared to a single Falcon Heavy launch.

Phase 1 of LunaRecycle launched in September 2024, ran through June 2025, and pulled 1,200 registrations — the largest response to any Centennial Challenge in NASA’s 20-year prize history (Wikipedia, Centennial Challenges). Seventeen teams were named Phase 1 winners from five countries and nine U.S. states. Phase 2 opened to U.S. teams only and required them to build a working prototype, optionally backed by a “digital twin” — a high-fidelity virtual model of the recycling line.

Sixteen teams cleared the Phase 2 milestone round in March 2026. They converged on Tuscaloosa from August 24 through August 28 to test their hardware at McAbee Construction, a local industry partner, with a public industry day and winners’ ceremony in H.M. Comer Hall (University of Alabama Engineering News, March 10 2026).

The first prize went to CERBERUZ, a team of undergraduate, graduate, and doctoral students at MIT. Their system — described in NASA’s award announcement as “Composites for Extraterrestrial Recycling By Engineering the Reuse and Upcycling of Zotek” — accepts mixed logistics waste, grinds it to a uniform powder, and remanufactures it into filament and injection-molded parts. The team’s insight was to stop treating the foam as contamination. Zotek F30, a closed-cell polyvinylidene fluoride foam from the British manufacturer Zotefoams, is what most aerospace interiors are made of — seat cushions, environmental control system ducting, equipment packaging. Once shredded, the foam acts as a reinforcing filler rather than a contaminant, and the resulting composite can be printed or molded into a fresh bracket or handle (NASA Centennial Challenges, August 28 2026).

The other nine teams on the prototype track ran the technology tree in different directions. Terasynth, an Orlando company, took second place with the Lunar Re-Forge System, which converts mixed waste into 3D-printing filament and recovers metals. Penn State’s RECLAIM team used microwave heating to convert plastic and metal waste into cast parts and fuel precursors — unusual because microwave heating penetrates materials volumetrically, not just at the surface. Cislune’s CRAFTER system from Rosemead, California ran pyrolysis, decomposing waste without oxygen to recover carbon, metal feedstock, and construction material. ACME Space LLC in Cheyenne, Wyoming compressed and thermally melted Zotek foam into dense tiles for lightweight structural panels (University of Alabama Engineering News, March 10 2026).

Five additional teams competed at the finale without milestone prizes, including Phoenix Loom (recycling cotton textiles), KLAW Industries (regolith-composite reinforcement), and Space Copy (foam-regolith extrusion).

The MIT team’s choice of PVDF is not incidental. PVDF is a semicrystalline fluoropolymer with a melting point of 177 °C and a density of 1.78 g/cm³ — higher than most commodity plastics, but inert to most solvents, acids, and hydrocarbons (Wikipedia, Polyvinylidene fluoride). In a vacuum-rated environment, the polymer also outgasses less than polyethylene or polyurethane, which matters when every gram of off-gassing condenses on a nearby optical surface. The Zotek F30 variant is a nitrogen-expanded closed-cell foam with densities from 30 to 150 kg/m³, thermally stable to 160 °C, and certified to the OSU heat-release and smoke-density standards required for commercial aircraft interiors (Zotefoams technical data sheet, 2024).

The grinding-and-reinforcement trick relies on a simple rule of composites. A short-fiber or particulate filler, well-dispersed, raises the modulus of a polymer matrix. The foam’s cells collapse into platelet-like fragments under the grinder, and the resulting powder behaves mechanically like a high-aspect-ratio reinforcement when re-melted with a virgin or reclaimed polymer carrier. The team’s digital twin — for which they also took first place — modeled throughput, energy use, and final-part mechanical properties under simulated lunar gravity (1.62 m/s², roughly one-sixth of Earth).

The microwave-based RECLAIM approach uses different physics. Microwaves at 2.45 GHz couple to polar molecules and lossy dielectrics; metal-bearing waste heats volumetrically, while pure plastics heat more weakly. That lets a single chamber process mixed trash without pre-sorting. Pyrolysis sidesteps oxygen entirely: at 400-700 °C under inert gas, polymers break into volatile tars, non-condensable gases, and a solid char. The char fraction typically retains 30-50% of the input carbon mass as a usable feedstock, while the gas fraction can be reformed into methane or hydrogen for fuel cells.

The throughput numbers matter as much as the chemistry. NASA’s challenge brief required finalist systems to demonstrate meaningful mass efficiency — converting a useful fraction of input waste into finished parts without prohibitive energy or astronaut time. The Highest Mass Efficiency award went to Cislune’s CRAFTER; the Most Trash Types Recycled award went to Bob Jones University’s LunaBrix, which combines recycled content with regolith simulant into stackable bricks. The Most Innovative prize went to RECLAIM for the microwave reactor. The People’s Choice went to Terasynth for the autonomous Lunar Re-Forge System (NASA Centennial Challenges, August 28 2026).

LunaRecycle is what NASA’s Centennial Challenges are designed for: a narrow, well-scoped problem with measurable success criteria, open to anyone with the engineering chops. It also happens to be one of the cheapest ways to test a piece of the Artemis program — $3 million, mostly going to small teams with no government contract overhead.

Two things will tell us whether this work matters. First, whether NASA pulls any of the prototypes into a flight experiment on a Commercial Lunar Payload Services lander or a Gateway resupply manifest. Second, whether the same chemistry shows up in the closed-loop life-support trade studies for Mars.

The deeper question is whether a Moon base can be a base at all if it cannot reuse what it already has. The fourteen teams in Tuscaloosa just spent a week making the engineering answer sound like yes.

A small team in Uppsala, Sweden spent five years winnowing a million stars down to nine that glowed strangely warm in the mid-infrared. The signal looked exactly like the signature Freeman Dyson predicted in 1960: starlight absorbed by a swarm of engineered habitats, the waste heat re-radiated at longer wavelengths. When the James Webb Space Telescope finally turned its 6.5-meter mirror on the two most promising candidates this summer, the answer came back in redder light than anyone expected. Both stars were ordinary M dwarfs. The infrared excess came from galaxies nearly a billion light-years behind them. Project Hephaistos had bagged two Hot DOGs and a dusty starburst, not a Kardashev-II civilization.

The search for extraterrestrial intelligence has spent most of its history chasing radio. That made sense in 1960, when Cocconi and Morrison published “Searching for Interstellar Communications” and Frank Drake pointed the Green Bank telescope at Tau Ceti. Radio is cheap, narrow-band, and physics says it can carry information across the galaxy. Optical SETI followed, then gamma-ray and neutrino lookups, then the more recent push for “technosignatures,” a deliberately broad term for any measurable fingerprint of engineered technology.

Dyson signatures sit at the far end of that spectrum. A civilization that wants to harvest a non-trivial fraction of a star’s luminosity has to build something physically large: a swarm of collectors, a shell, a statite array. No known natural astrophysics produces a star that is unusually faint at visible wavelengths while flooding the mid-infrared. The contrast is the whole point.

That contrast also makes Dyson searches almost uniquely easy to spoof. Dust around young stars looks like Dysons. Active galactic nuclei look like Dysons. Gravitationally lensed background galaxies look like Dysons. The trick is not finding candidates. The trick is surviving the long chain of false positives.

Project Hephaistos started as a Stockholm-Uppsala collaboration in 2021, led by Erik Zackrisson. The first step was cross-matching the Gaia DR3 catalog with WISE infrared photometry, then applying color cuts that ought to leave only stars whose mid-infrared output dwarfs their visible output. A first paper in 2024 narrowed roughly one million M dwarfs within 300 parsecs down to seven that survived. A second paper added two more. Nine candidates, designated A through I, each a small red star, each a few billion years old, each suspiciously dim in the optical.

The follow-up paper, Hephaistos III in July 2026 (Korn et al., arXiv:2607.25701), spent months chasing the candidates with ground-based photometry and low-resolution spectroscopy. None of them showed the H-alpha emission or lithium absorption lines expected of a young star with a transitional circumstellar disk. Stellar activity could explain some of the variability, but not the bulk of the infrared excess. The team couldn’t kill the candidates, but they couldn’t confirm them either.

Then Webb settled it.

Hephaistos IV (Zackrisson et al., submitted to MNRAS, arXiv:2607.09460) targeted two of the strongest candidates, D and E, with MIRI imaging and spectroscopy in June 2026. Candidate D, the most exciting, sat at a redshift of roughly z = 0.9, appeared point-source-like in the imaging, and showed a mid-infrared spectrum consistent with a Hot Dust-Obscured Galaxy. Hot DOGs are some of the most luminous galaxies in the universe: their central engines are buried under thick blankets of warm dust that reradiate the optical and ultraviolet output into the infrared, exactly the spectrum a Dyson swarm would produce if you couldn’t resolve it.

Candidate E was a z ~ 0.4 galaxy with extended morphology, bright knots of star formation, and the spectral signature of a dusty starburst. Both galaxies sit within roughly an arcsecond of their foreground M dwarfs on the sky. From WISE’s coarse pixels, the starlight and the galaxy light smeared together. To WISE, that smear looked like a faint optical star with too much infrared emission. To JWST, it looked like an M dwarf with a galaxy photobombing it.

The Hephaistos team’s conclusion is dry: the infrared excess does not originate from Dysonian megastructures or any other radiation mechanisms close to these stars. The next round of search will need much higher spatial resolution than WISE can offer. The 2030s infrared observatories that Andreas Korn and his colleagues point to in their press materials are designed to do exactly that.

The Dyson concept sits inside a framework the Soviet astronomer Nikolai Kardashev proposed in 1964. A Type-I civilization uses all the energy available on its home planet, roughly 10^16 watts for Earth. Type II harvests its star, on the order of 10^26 watts for the Sun. Type III commands an entire galaxy, around 10^36 watts. Dyson’s original 1960 paper in Science asked how a Type-II civilization would dispose of waste heat, and noted that any structure intercepting a meaningful fraction of a star’s luminosity has to reradiate that energy somewhere. The mid-infrared is the natural choice, because a swarm’s equilibrium temperature, set by balancing absorbed starlight against emitted blackbody radiation, falls somewhere around 200 to 400 kelvin for a star like the Sun.

The peak wavelength of that emission is set by Wien’s displacement law, λ_peak (μm) ≈ 2898 / T (K).

A 300 kelvin Dyson swarm peaks near 9.7 micrometers, right inside WISE’s W3 band at 12 micrometers and JWST MIRI’s red end. That’s why the Hephaistos search uses W3-W1 color cuts: stars that should look like blackbodies at 2,800 to 3,800 kelvin but instead dump energy into a 9-micrometer band stand out.

The contamination problem is structural. WISE’s 12-micrometer pixels are 6.5 arcseconds wide. JWST’s shortest MIRI imaging band runs near 5 micrometers with diffraction-limited resolution of about 0.1 arcseconds. The angular resolution ratio is roughly 65 to 1, which means WISE blends sources that JWST can split. A faint background galaxy with a hot dusty nucleus will add flux to every pixel that contains the M-dwarf centroid. If the galaxy is at high redshift and K-corrected into the mid-infrared, its spectrum can look almost like a blackbody with the right temperature. That’s exactly what Hot DOGs do.

For the candidate identification, the math is straightforward. Given an apparent magnitude in the visible m_v and a magnitude in the mid-infrared m_W3, a star with a Dyson shell at temperature T emitting as a modified blackbody shows an infrared excess of Δ(m_W3 − m_v) = (m_v − M_v) − (m_W3 − M_W3) − BC_corr, where M_v and M_W3 are the absolute magnitudes expected for the stellar photosphere alone. Anything more than a few magnitudes of excess on top of the expected Rayleigh-Jeans tail triggers the flag. WISE picked up roughly 9 such objects out of 10^6.

The engineering is also telling. JWST’s MIRI instrument, which did the actual follow-up, is a 50-kelvin cryocooled camera and spectrograph operating from 5 to 28 micrometers. It took roughly 30 years from concept to first light. The contrast with WISE is sharp: WISE was a 40-centimeter survey telescope that mapped the entire sky in six months, while JWST is a 6.5-meter segmented mirror at L2 that can spend hours on a single target. The two designs are complementary, and that complementarity is exactly what broke this case open.

The Dyson search is not getting easier. It is getting slower, more expensive, and more rigorous. Each round of follow-up costs more telescope time than the round before, and the surviving candidates shrink in number faster than new surveys add to the list. The Hephaistos result is part of a pattern: most candidate Dysons turn out to be dusty galaxies, AGN, or stellar variability. A few percent have stayed unexplained, but the unexplained share keeps shrinking.

For the Dyson concept itself, none of this is fatal. A Type-II civilization would not necessarily produce a signature WISE could see, and a Type-III civilization’s footprint is so diffuse that it would look like background noise in any single survey. The Hephaistos team is already planning the next iteration, with higher-resolution mid-infrared facilities in the 2030s and follow-up on the surviving seven candidates that Webb hasn’t yet looked at. The question that motivated Freeman Dyson in 1960, where the waste heat of an advanced civilization ought to show up, still has no answer. We are simply narrowing where it isn’t.

At roughly 650 light-years from Earth, the Helix Nebula is close enough to show structure that most planetary nebulae conceal. Its famous bright ring is the part that grabs the eye: a vast, blue-green disk of ionized gas surrounding a dying star. A new image from the partially built MOTHRA telescope reveals a quieter feature outside that ring. On the eastern side of NGC 7293, the gas forms a line of at least 22 arcs and partial arcs, each one a bow shock in the faint outer halo. (van Dokkum et al., Nature, 12 August 2026)

The image is not a new portrait of a planetary nebula’s familiar face. It shows the boundary where the nebula stops behaving like an orderly expanding shell and begins to dissolve into the surrounding interstellar medium (ISM). The arcs are the traces of dense fragments of material shed during the star’s asymptotic giant branch (AGB) phase. They are moving through gas faster than sound, compressing and heating the material in front of them.

That boundary is important because the final stage of a star is not the end of its influence. A star can spend much of its life returning its outer layers to the galaxy. The elements forged in the star, along with newly formed dust, eventually become part of new clouds, planets, and stars. The Helix gives astronomers a nearby place to watch that return in progress.

Stars lose mass long before they become white dwarfs. During the AGB phase, a modest-sized star develops a dense, slow wind and expels a shell rich in carbon, dust, and other products of nuclear processing. The planetary nebula is the visible aftermath: a fast flow catches up with that older material and lights it up. Later, the material has to join the much thinner, turbulent gas of the galaxy. That last handoff is hard to observe because the fragments become faint and widely spread.

The Helix is a useful natural laboratory for studying it. Gaia measurements place its central white dwarf about 198.6 parsecs away, close enough to resolve features a few hundredths of a parsec across. The new study found that the coherent bow-forming fragments have a characteristic survival time of about 10,000 years. That is a useful number for models of how galaxies circulate gas and metals. Simulations often treat this transfer as subgrid mixing, because no calculation can represent every cloud and filament inside a galaxy. (van Dokkum et al., Nature, 12 August 2026)

The result also shows how a purpose-built instrument can answer a question that ordinary photographs cannot. MOTHRA, the Modular Optical Telephoto Hyperspectral Robotic Array, uses many Canon 400-millimeter telephoto lenses instead of one enormous mirror. Its official design calls for 1,140 lenses on 30 mounts, with an optical system equivalent to a 4.8-meter f/0.08 refractor. The system is optimized for low-surface-brightness light, the kind of diffuse glow that disappears against the sky, foreground stars, and scattered light. (MOTHRA project, 2026)

The story begins with a late-AGB wind. Some of the material from that wind lies in clumps rather than a smooth shell. Over time, those clumps travel outward. The material now producing the eastern arcs appears to have been expelled earlier than the nebula itself: its velocity and distance imply ages of roughly 20,000 to 30,000 years, while the planetary nebula is about 12,000 years old. (van Dokkum et al., Nature, 12 August 2026)

The nebula is also moving through the local ISM. Gaia-derived measurements give a bulk speed of about 45 kilometers per second. A shock forms where that moving nebula meets material flowing into the opposite direction. The researchers estimate that the eastern bow shocks are traveling at 80 to 90 kilometers per second, with the western features moving more slowly, around 35 kilometers per second. The contrast is visible because the eastern fragments encounter the full combination of nebular expansion and ambient gas, while the western side is partly shielded by a turbulent wake.

A 20-minute-equivalent exposure by the completed MOTHRA array would have required 172.5 single-lens-equivalent hours with the five mounts used in 2025. The resulting image is striking for what appears at the focus of the arcs. There is no bright H-alpha, nitrogen, or oxygen emission at most of those locations. The fragments are likely mostly neutral, so the researchers identify them by the shocks they produce. This is the observational distinction that matters: the arcs are not a new population of objects. They are a map of invisible pieces of the old circumstellar envelope.

The fragments change as they move outward. The inner bows are broad, thin, and sharply bounded. Farther out, they become smaller, clumpy, and less distinct. Their radius of curvature falls by two orders of magnitude between about 0.4 and 1.4 parsecs. (van Dokkum et al., Nature, 12 August 2026)

MOTHRA is a lesson in designing for a measurement rather than for spectacle. A single huge lens is difficult to manufacture, mount, and keep aligned. A telephoto array uses commercially available lenses with excellent coatings and combines their light-gathering area. The trade is a wider field of view and a much more complicated calibration problem. Every lens must be timed, focused, and filtered consistently, and the detector image must be corrected for small differences in pointing and throughput. The Dragonfly project describes the system as a robotic array with a field of view larger than six square degrees, aimed at the faint circumgalactic medium and the cosmic web. (Dragonfly Telephoto Array, 2026)

The filters make the target visible. H-alpha is the hydrogen line at 656.3 nanometers, a useful tracer of ionized gas. MOTHRA uses a 0.93-nanometer H-alpha filter, whose width corresponds to a velocity spread of roughly 425 kilometers per second: Δv ≈ Δλ/λ * c. It also observes [N II] and [O III] emission and uses continuum filters with a narrow notch at the line wavelength. Subtracting the continuum removes much of the light that would otherwise drown the moving gas.

A bow shock is a supersonic interface. A useful first-order measure is the Mach number, M = v_shock/c_s. If the ionized gas has a sound speed near 10 kilometers per second, an 80-to-90-kilometer-per-second shock has M around 8 or 9. The flow compresses the gas, raises its temperature, and changes the strengths of its emission lines. The measured [N II]/H-alpha and [O II]/H-alpha ratios let the team distinguish a fast shock from a faint, slower feature.

The spatial trend provides the time measurement. A fit to the bow curvature can be summarized as R_c ∝ e^(-r / 0.27 pc). At the estimated expansion speed of about 40 kilometers per second, that corresponds to an e-folding disruption time of roughly 7,000 years. The result is a direct clue to the life of an AGB-shell fragment after it meets the ISM. The dense head shrinks through ablation and entrainment, while the surrounding gas carries its dust and elements into the larger galactic reservoir.

MOTHRA turns the outskirts of a familiar nebula into a test of stellar recycling. The 22 arcs are small individually, but their distribution lets researchers measure a process that is usually too faint to trace: the gradual loss of coherence by material shed from an evolved star. The Helix is not simply a glowing shell left behind by a white dwarf. It is a transition zone, where an old stellar envelope becomes part of the interstellar medium.

The completed array will search for similar fragment-driven shocks around other planetary nebulae. Astronomers can test whether the roughly 10,000-year disruption timescale is universal and look for molecular counterparts to the neutral clumps. Each new bow shock will add a coordinate to a still poorly measured stage of the galaxy’s life cycle. The next-generation instruments here are not making the universe look brighter for its own sake. They are revealing the slow, physical handover of matter between generations of stars.

In mid-August, on a concrete ramp at an undisclosed airport in Oklahoma, a freshly painted Boeing 737-700 sat in red, white, and blue. The NASA meatball was on the tail, the registration N837NA on the rear fuselage, and the words reduced gravity research aircraft across the cabin. NASA released the frames on 13 August 2026 (NASA, August 2026).

Behind the new paint is a stranger story. This airframe was delivered to a private operator in 2013 as N712JM, a Boeing 737-73W. By 2020, plane spotters noticed it sitting at Colorado Springs in a green protective coating, bristling with sensors and wiring runs no commercial jet had any business carrying. Aviation journalists at The War Zone traced the registered mailing address on its airworthiness documents to the same building that houses the U.S. Air Force’s Rapid Capabilities Office, the secretive acquisition outfit that fields programs like the B-21 Raider. The Air Force confirmed to The War Zone that N712JM flew for a classified program that has since ended, and NASA acknowledged in contracting documents that the agency itself did not have the need-to-know (The Aviationist, 17 August 2026; The War Zone, 2024).

NASA Armstrong Flight Research Center took ownership in June 2026. The new “NASA 837” carries the registration that once belonged to the agency’s NF-15B test jet, retired in 2009 after 36 years of flight-control research. The 737 inherits the number; the secrets stay behind.

Landing on the Moon is not like floating in orbit. The Moon pulls at roughly 1.62 m/s², about one-sixth of Earth’s 9.81 m/s², and a pressurized suit under that load behaves in ways pure weightlessness cannot reproduce. A suit that weighs as much as the person inside it changes the biomechanics of walking, picking up rocks, climbing ladders, and getting up after a fall. Ground labs cannot simulate those effects without removing gravity.

NASA’s answer for decades has been parabolic flight. A maneuvering aircraft traces the arc of a free-falling object, so for a brief window everything inside the cabin, including the aircraft, falls together. The standard maneuver gives about 20 seconds of microgravity per parabola, with 15 to 30 parabolas stacked into one flight (NASA, “Parabolic Flight,” 2026). Roughly two-thirds of first-time passengers get sick, which is how the aircraft picked up its unofficial name.

Microgravity is the wrong flavor of reduced gravity for Artemis. To produce Moon-like 1/6 g, the pilot cannot just unload the controls and coast. The trajectory must be flown with the airplane carrying more lift and slightly more thrust than it would in a true free fall, so its downward acceleration in the inertial frame is about 8.2 m/s², the difference between Earth’s 9.81 and the Moon’s 1.62. Mars at 0.38 g needs a smaller lift offset. Each profile is a separate skill and a separate test campaign for whatever the experimenters strap to the cabin floor.

NASA has been without a dedicated government parabolic jet since the agency wound down the Reduced Gravity Research Program in July 2014, after its McDonnell Douglas C-9B Skytrain II (N932NA, ex-KLM) developed unsolvable airworthiness issues. The agency now charters flights from Zero Gravity Corporation’s Boeing 727-200, G-FORCE ONE, and from Novespace’s Airbus A310 Zero-G in Bordeaux-Mérignac. Both can simulate lunar and Martian gravity, but neither belongs to NASA, and neither is configured for the suit qualification Artemis is asking for (Wikipedia, “Reduced-gravity aircraft,” 2026).

On 1 June 2026, NASA awarded Denmar Technical Services of Nevada an $8.4 million firm-fixed-price contract to modify the 737-700 for lunar-gravity parabolic operations. The contract runs through 1 February 2027, after which the aircraft will be owned by NASA Armstrong but flown out of NASA Johnson in Houston, with Armstrong retaining oversight (NASA, 1 June 2026).

The aircraft’s primary job is astronaut lunar suit qualification. Each Artemis crew will run parabolas inside the pressurized suit, working through the tasks they expect on the surface: kneeling to deploy a sample scoop, picking up a rock, recovering from a stumble, climbing into a lander hatch. NASA has historically used neutral buoyancy, the large pools where suited astronauts practice procedures underwater, for most of this training, and the agency’s new Langley partial-gravity simulator will handle suspension-based work. The 737 adds a third leg: short bursts of true free-fall at lunar gravity, in an aircraft moving fast enough to give the suits a realistic test of inertia.

The 737 will also serve as a flying testbed for autonomy, sensors, and digital flight-control research under Armstrong’s traditional portfolio (NASA, 13 August 2026).

A parabolic trajectory is, in the inertial frame, what Newton predicted for any object under gravity alone: a constant downward acceleration of g, with the horizontal component unchanging. The aircraft pulls up at about 45°, trading airspeed for altitude. The pilot throttles back to idle and pushes the nose over. From that point, the plane falls along the same arc a dropped stone would, and so does everything loose inside it. From the cabin’s frame of reference, gravity simply vanishes. The reduced-g phase ends when the descent angle reaches roughly 30° below horizontal, where the pilot must pull out.

The 20-second budget is set by how steeply the plane can dive without exceeding airframe limits or the FAA’s airspeed envelope. A 737 enters the maneuver around 7,600 m at roughly 450 km/h. The velocity vector rotates from 45° up through horizontal to 30° below, a swing of 75°, with no vertical speed at the top and acceleration equal to g along the way. That arc, plus the climb-out and recovery, gives 20 to 25 seconds. Each parabola is bookended by a 1.8 g pull-up and a 1.8 g pull-out, so a passenger’s g-load in one cycle runs 1.8 g → ~0 g → 1.8 g (NASA, “Parabolic Flight,” 2026).

To produce lunar gravity rather than zero, the trajectory follows a shallower arc in which the cabin accelerates downward more slowly than a true free-falling object would. The pilot adds enough lift and a small, steady nose-down command so the airplane traces an arc that would correspond to falling toward a body with a stronger pull than the Moon. The residual force on cabin occupants is the difference between Earth’s gravity and the airplane’s actual downward acceleration: 9.81 − 8.19 ≈ 1.62 m/s², or about 0.165 g. Mars is easier at 3.71 m/s².

The aircraft modifications are mostly about padding and instrumentation, not propulsion. A 737 already has the wing loading, thrust margin, and fuel capacity to absorb a parabolic stack. The hard engineering is in protecting the cabin from the 1.8 g bookends (suited astronauts get crushed into their seats for the first and last 30 seconds of every parabola) and in mounting cameras, accelerometers, and umbilicals so test subjects can be observed without falling on top of each other in 0.165 g.

The new 737 is one piece of a much larger validation program. The Artemis suit, the Human Landing System, the Gateway space station, and the rovers all eventually need real partial-gravity testing before they fly. Neutral buoyancy will keep handling long, procedure-driven rehearsals. The Langley gantry will handle suspension work. The 737 supplies what neither can: short, repeated, true free-fall at the right fraction of Earth gravity, even if only twenty seconds at a time.

It is also, quietly, the agency’s first government-owned research aircraft with a classified past NASA still cannot fully explain. The engineers at Armstrong and Johnson get the airplane and the schedule. The historians will keep digging.

In late August 2026, inside a clean tent at the Ensemble de Lancement Vega in Kourou, French Guiana, technicians finished filling a small Italian-built satellite with 30 kilograms of hydrazine. The spacecraft had crossed the Atlantic once already, aboard the MN Colibri, departing Cannes on 9 July and arriving at Pariacabo harbour on 12 July (Wikipedia, “FLEX (satellite),” August 2026). On 15 September 2026 it leaves the ground on a Vega-C, alongside the Copernicus Sentinel-3C satellite (ESA FLEX facts and figures, 2026). The mission has a 3.5-year design life, an 814-kilometre sun-synchronous orbit, and a 400-kilogram dry mass. Its job is not imaging clouds or measuring sea level. It will stare down at forests and croplands and try to measure a faint red glow that plants produce when they photosynthesise, a signal too dim to see with the eye and almost too dim to see from low Earth orbit.

Roughly 120 gigatonnes of carbon per year move between the atmosphere and terrestrial vegetation through photosynthesis, more than ten times the mass of all the carbon humanity emits from fossil fuels (Le Quéré et al., Earth System Science Data, 2024). Almost every climate projection depends on getting that number right, and the spread across current carbon-cycle models is on the order of ±20 GtC/yr. Sun-induced chlorophyll fluorescence, the 1–2% of absorbed light that leaves re-emit at wavelengths around 685 nm and 740 nm, is a direct optical window onto photosynthetic efficiency, because every absorbed photon ends up in one of three places: photochemistry, heat, or fluorescence (Wikipedia, “Chlorophyll fluorescence,” 2026). In a healthy leaf, roughly 82% of absorbed photons drive carbon fixation; the rest is split between heat and this faint red glow.

Until now, fluorescence has been measured with bench-top instruments or aircraft campaigns like HyPlant flown out of Forschungszentrum Jülich (eoportal, FLEX, 2017). There is no global, repeatable, satellite-derived fluorescence product for the terrestrial biosphere. ESA selected FLEX as the eighth Earth Explorer in November 2015, and the satellite has spent a decade working up to one question: can you read the productivity of a soybean field, a larch forest, and a millet plot, all from 800 kilometres up, using only sunlight the leaf itself emitted back?

The hardware story of FLEX starts in November 2016, when ESA awarded the main instrument contract to Leonardo. In January 2019, Thales Alenia Space in Cannes became prime contractor for both spacecraft and instrument integration. The bus is an evolution of the Myriade family that flew COROT and PARASOL, but the avionics come from the Sentinel-3 line. In orbit the satellite measures 1.5 m × 4.9 m × 1.6 m, mass is 400 kg, end-of-life power is 950 W from a deployable solar array backed by a 57.6 Ah Li-ion battery (ESA FLEX facts and figures). The single instrument, the FLuorescence Imaging Spectrometer (FLORIS), covers 500–780 nm with variable spectral sampling: 0.1 nm in the two telluric oxygen absorption bands (O2-A at 759–769 nm and O2-B at 686–697 nm), 0.5–0.65 nm across the red edge, and 2.0 nm in the photochemical reflectance index band (500–600 nm). Spatial resolution is 300 m on a 150 km swath (eoportal, FLEX).

The clever trick is the tandem formation with Sentinel-3. FLEX orbits 40–100 km ahead of a Sentinel-3 platform, so that OLCI and SLSTR look at the same footprint within 6–15 seconds of FLORIS (eoportal, FLEX). Sentinel-3’s broad-band radiance is used to estimate the reflected sunlight contribution inside the O2-A and O2-B absorption lines, which can otherwise swamp the fluorescence signal at the 1–3 mW m⁻² nm⁻¹ sr⁻¹ level the mission is trying to recover. Two spacecraft, two spectrometers, one number.

Late summer 2026 was the home stretch. By April 2026, the integrated satellite had passed functional and environmental testing at Cannes (ESA, “FLEX shows off,” April 2026). It shipped on the MN Colibri to Pariacabo in early July 2026, was uncrated on 21 July, and was fuelled in late August. The launch is scheduled for 15 September 2026 at 22:21 local time from the ELV pad at the Guiana Space Centre on flight VV30 of the Vega-C, alongside Sentinel-3C (ESA press release N° 35–2026, 20 July 2026).

Vega-C is a four-stage European workhorse: a P120C solid first stage (4,323 kN, 279 s Isp, 141.6 t of HTPB propellant), a Zefiro 40 solid second stage (1,304 kN, 293.5 s Isp), a Zefiro 9 solid third stage (317 kN, 295.9 s Isp), and a storable AVUM+ upper stage (RD-843 engine, UDMH/N₂O₄, 2.42 kN, up to five restarts) (Wikipedia, “Vega C,” 2026). FLEX at 400 kg plus Sentinel-3C at roughly 1,250 kg fits inside the rocket’s 2,300 kg sun-synchronous capability.

The fluorescence signal is small because most absorbed light goes to chemistry and heat. Under steady-state illumination, leaf-level energy partitioning is

Y_PSI + Y_NPQ + Y_F = 1

where Y_PSI is the quantum yield of photochemistry through Photosystem II, Y_NPQ is non-photochemical quenching (heat dissipation via the xanthophyll cycle and PsbS protein), and Y_F is the fluorescence yield. FLEX measures Y_F directly; the carbon flux GPP (gross primary production) is then typically inferred as

GPP ≈ APAR × Y_PSI

with APAR (absorbed photosynthetically active radiation) reconstructed from FLORIS’s PRI and red-edge bands plus Sentinel-3’s OLCI/SLSTR radiances.

The reason the O2-A band (759–769 nm) matters is that molecular oxygen in the atmosphere absorbs sunlight there. Inside that absorption feature, any photons reaching the satellite must have been re-emitted at the surface, by the leaf. The depth of the absorption line in a downward-looking spectrum tells you how much extra radiance fluorescence is adding, after correcting for surface reflectance and atmospheric scattering. The Fraunhofer IOF in Jena built the double-slit assembly that defines FLORIS’s spectral resolution in those bands down to 0.1 nm. The narrower the slit, the cleaner the line-depth measurement, but the weaker the signal-to-noise ratio (Wikipedia, “FLEX (satellite),” 2026).

The 27-day repeat cycle at 814 km and 98.64° inclination matches Sentinel-3A’s ground track, so every 27 days the tandem pair sees the same vegetation at the same local time of day and solar geometry. That is essential for separating fluorescence from bidirectional reflectance effects. The 814 km altitude was chosen to give a 27-day repeat with 14+ orbits per day, and to keep the 300 m pixel footprint compatible with Sentinel-3 OLCI.

The third axis of the engineering is calibration stability. FLORIS is an imaging spectrometer, so pixel-to-pixel and band-to-band gain drift will alias straight into apparent fluorescence trends. On-board calibration uses solar diffuser references plus periodic lunar looks. The Sentinel-3 OLCI instrument flies the same calibration philosophy, which is one reason ESA reused its avionics and reference samples on FLEX.

Once commissioned, FLEX is expected to deliver monthly global maps of sun-induced chlorophyll fluorescence at 300 m × 300 m, the first such dataset produced routinely from orbit (ESA FLEX facts and figures). For plant physiologists, the result will be a four-dimensional look at photosynthetic efficiency, with direct implications for drought monitoring, agricultural yield forecasting, and the calibration of dynamic global vegetation models. For the carbon-cycle community, the value is a top-down constraint on GPP that does not depend on meteorological reanalysis.

If FLEX works, it will retire a long-standing assumption baked into climate models, that the greenness of a canopy, measured by NDVI or similar indices, is a proxy for what the canopy is actually doing. Two fields can look equally green and yet be photosynthesising at very different rates, depending on water stress, nutrient status, and temperature. FLEX will measure the difference. The world has never watched photosynthesis happen from space in real time. In three weeks, it will start to.

For twenty years, every byte of data sent home from the surface of Mars has ridden a UHF radio piggyback on a science orbiter that happened to be passing overhead. On 2 September 2026 NASA ended that arrangement. The agency announced that Blue Origin will design, build, launch, and operate a dedicated Mars Telecommunications Orbiter under a firm-fixed-price contract worth up to $700 million, with delivery by the end of 2028 and full operations at the red planet in 2030 (NASA news release, 2 Sep 2026). For the first time since the cancelled 2005 Mars Telecommunications Orbiter, NASA is buying communications capacity at Mars the way it buys launch services from SpaceX: a fixed commercial price for a working spacecraft, with the operator running the show.

The award is small in dollar terms compared to flagship planetary missions and large in strategic terms. It formalizes the commercial-services model that has reshaped cislunar space and applies it 1.4 astronomical units farther out. It puts the first dedicated deep-space relay at a planet, not at the Moon. And it gives Blue Origin — eight years after New Shepard reached the Kármán line — a planetary-scale role that no other company has held.

Every rover since Sojourner has paid a tax for its bandwidth. The UHF Electra relay on Mars Reconnaissance Orbiter tops out near one megabit per second, and that link is shared with instruments the orbiter was actually launched to run (Edwards et al., 2003). The Deep Space Network’s direct X-band uplink is even thinner — a single HiRISE frame takes 1.5 hours at MRO’s 5.2 Mb/s peak (JPL, “Deep Space Communications,” 2017). Perseverance’s plume telemetry, Ingenuity’s flight logs, the trace-gas measurements from ExoMars TGO — all of it competes for slots in orbits selected to do science, not to be comms towers.

A purpose-built relay changes the calculus. Operators can schedule lander passes against an orbit designed for continuous visibility, freed from the geometry of a science primary mission. Layer a deep-space optical terminal on top — analogous to the Deep Space Optical Communications package Psyche has been flight-qualifying since 2023 — and the link budget explodes. DSOC pushed 267 Mb/s from 31 million kilometers in late 2023 and held a link to 467 million kilometers in July 2024 (JPL, 11 Dec 2023; NASA, 25 Apr 2024).

The second-order effect is what NASA gets to stop doing. SCaN has been forced for two decades to add relay payloads to every Mars science orbiter as a tax for participating. Stripping that out frees mass, power, and cost on the next generation of orbiters — a meaningful simplification when the Mars Sample Return architecture is still being rebuilt and human Mars exploration sits on NASA’s stated timeline.

NASA’s request for proposals went out in May 2026, drawn up under procurement authority inserted by the 2025 One Big Beautiful Bill Act, which explicitly allocated $700 million for the orbiter. The Act’s wording tied the procurement to companies that had previously received Mars Sample Return study money and pitched a telecom element as part of those studies — eight firms in total: Aerojet Rocketdyne, Blue Origin, Lockheed Martin, Northrop Grumman, Quantum Space, Rocket Lab, SpaceX, and Whittinghill Aerospace. The competitive field narrowed quickly. The award names Blue Origin as prime, with no public teaming structure disclosed.

Blue Origin owns the full stack: bus, telecom payload, launch on its own New Glenn 7×2, trans-Mars injection, Mars orbit insertion, and operations. The published draft specification lists an areocentric orbit with a 180 km periareon and 4,500 km apoareon — a high-elliptical geometry that gives long dwell times over a fixed surface region while still clearing the atmosphere at the low end. New Glenn 7×2 has a trans-lunar capacity near 7 metric tons (NASA ELV Performance). The company has flown the vehicle successfully twice and failed once — the pad explosion that took LC-36A offline — so it will need to commission LC-36B or shift to Vandenberg to honor the 2028 commitment.

Behind the announcement is the same calculation that produced Commercial Lunar Payload Services and Human Landing System: in a budget environment where every Mars architecture decision is being fought between sample-return, human-exploration, and science advocates, the cheapest move is to buy the bits and let the science missions keep their mass margins.

The relay orbit is the design lever that makes everything else work. A 180 × 4,500 km areocentric orbit gives roughly 8 to 10 hours of continuous visibility over a fixed surface target per orbital period near 7.5 hours. Compared with the 250 km circular sunsynchronous science orbit flown by MRO, the relay geometry trades observation time for surface dwell time. The radio link uses UHF proximity at 390 to 450 MHz with the CCSDS Proximity-1 protocol stack — identical to what flies on MRO, MAVEN, ExoMars TGO, Curiosity, InSight, and Perseverance. Every Mars asset currently on the surface can fall back to the new relay with no hardware changes (Edwards, 2003).

The free-space loss for the UHF proximity leg is bounded by:

L_fs = (4 * pi * d * f / c)^2

At 400 MHz and a slant range of about 1,000 km, path loss lands near 158 dB — the reason surface antennas are low-gain whips and the orbiter carries the high-gain nadir-pointed Electra package. The Earth-return leg at X-band (8.4 GHz) and Ka-band (32 GHz) from Mars runs at roughly 261 dB and 281 dB of free-space loss. Closing a 1 Mb/s link to a 70 m DSN aperture at X-band requires an EIRP around 38 dBi — achievable with a 1.5 m steerable dish.

The optical path changes the math. At 1.55 μm and 1.4 AU, beam divergence dominates over L_fs. The angular beamwidth of a diffraction-limited 22 cm aperture is:

theta = 1.22 * lambda / D ≈ 8.6 microradians

At Mars-Earth range, that gives a beam footprint on Earth near 1,200 km — the same order as the DSOC ground footprint demonstrated in flight, which is why DSOC paired a 22 cm spacecraft telescope with a 5 m Hale-class ground receiver (JPL DSOC poster, 2014). A relay with both a UHF proximity payload for handoff and an optical Earth-return payload for bulk data could push daily return into the terabit range, an order of magnitude over today’s network.

The contract also stress-tests the fixed-price model at interplanetary distances. NASA’s answer was to make the procurement compatible with commercial commsat buses — Blue Origin is expected to leverage a scaled Blue Ring platform — and to define the service in throughput and availability terms, not hardware specifications. The bet is that a commercial GEO production line can be retooled for an areocentric relay without a bespoke NASA-only factory.

The Mars Telecommunications Orbiter was proposed in 2004, cancelled in 2005, rediscovered in 2018 as NeMO, stalled in 2025, and finally contracted 21 years later. If Blue Origin hits the December 2028 delivery date, its 2030 arrival will coincide with a Mars surface far busier than the one Perseverance and Curiosity see today. Mars Sample Return needs continuous relay coverage during lander choreography. Human Mars missions need guaranteed high-bandwidth links that do not depend on a science orbiter being overhead.

The deeper story is that the relay architecture of the inner solar system is being privatized the way launch has been. The agency that built the Deep Space Network is handing its first dedicated relay at Mars to a commercial prime. The hardware questions are interesting; the procurement question is the one that will define the next twenty years.