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By NASA
6 min read
Preparations for Next Moonwalk Simulations Underway (and Underwater)
An astronaut glove designed for International Space Station spacewalks is prepped for testing in a chamber called CITADEL at NASA JPL. Conducted at temperatures as frigid as those Artemis III astronauts will see on the lunar South Pole, the testing supports next-generation spacesuit development.NASA/JPL-Caltech Engineers with NASA Johnson and the NASA Engineering and Safety Center ready an astronaut glove for insertion into the main CITADEL chamber at JPL. The team tested the glove in vacuum at minus 352 degrees Fahrenheit (minus 213 degrees Celsius).NASA/JPL-Caltech A JPL facility built to support potential robotic spacecraft missions to frozen ocean worlds helps engineers develop safety tests for next-generation spacesuits.
When NASA astronauts return to the Moon under the Artemis campaign and eventually venture farther into the solar system, they will encounter conditions harsher than any humans have experienced before. Ensuring next-generation spacesuits protect astronauts requires new varieties of tests, and a one-of-a-kind chamber called CITADEL (Cryogenic Ice Testing, Acquisition Development, and Excavation Laboratory) at NASA’s Jet Propulsion Laboratory in Southern California is helping.
Built to prepare potential robotic explorers for the frosty, low-pressure conditions on ocean worlds like Jupiter’s frozen moon Europa, CITADEL also can evaluate how spacesuit gloves and boots hold up in extraordinary cold. Spearheaded by the NASA Engineering and Safety Center, a glove testing campaign in CITADEL ran from October 2023 to March 2024. Boot testing, initiated by the Extravehicular Activity and Human Surface Mobility Program at NASA’s Johnson Space Center in Houston, took place from October 2024 to January 2025.
An astronaut boot — part of a NASA lunar spacesuit prototype, the xEMU — is readied for testing in JPL’s CITADEL. A thick aluminum plate stands in for the cold surface of the lunar South Pole, where Artemis III astronauts will confront conditions more extreme than any humans have yet experienced.NASA/JPL-Caltech In coming months, the team will adapt CITADEL to test spacesuit elbow joints to evaluate suit fabrics for longevity on the Moon. They’ll incorporate abrasion testing and introduce a simulant for lunar regolith, the loose material that makes up the Moon’s surface, into the chamber for the first time.
“We’ve built space robots at JPL that have gone across the solar system and beyond,” said Danny Green, a mechanical engineer who led the boot testing for JPL. “It’s pretty special to also use our facilities in support of returning astronauts to the Moon.”
Astronauts on the Artemis III mission will explore the Moon’s South Pole, a region of much greater extremes than the equatorial landing sites visited by Apollo-era missions. They’ll spend up to two hours at a time inside craters that may contain ice deposits potentially important to sustaining long-term human presence on the Moon. Called permanently shadowed regions, these intriguing features rank among the coldest locations in the solar system, reaching as low as minus 414 degrees Fahrenheit (minus 248 degrees Celsius). The CITADEL chamber gets close to those temperatures.
Engineers from JPL and NASA Johnson set up a test of the xEMU boot inside CITADEL. Built to prepare potential robotic explorers for conditions on ocean worlds like Jupiter’s moon Europa, the chamber offers unique capabilities that have made it useful for testing spacesuit parts.NASA/JPL-Caltech “We want to understand what the risk is to astronauts going into permanently shadowed regions, and gloves and boots are key because they make prolonged contact with cold surfaces and tools,” said Zach Fester, an engineer with the Advanced Suit Team at NASA Johnson and the technical lead for the boot testing.
Keeping Cool
Housed in the same building as JPL’s historic 10-Foot Space Simulator, the CITADEL chamber uses compressed helium to get as low as minus 370 F (minus 223 C) — lower than most cryogenic facilities, which largely rely on liquid nitrogen. At 4 feet (1.2 meters) tall and 5 feet (1.5 meters) in diameter, the chamber is big enough for a person to climb inside.
An engineer collects simulated lunar samples while wearing the Axiom Extravehicular Mobility Unit spacesuit during testing at NASA Johnson in late 2023. Recent testing of existing NASA spacesuit designs in JPL’s CITADEL chamber will ultimately support de-velopment of next-generation suits being built by Axiom Space.Axiom Space More important, it features four load locks, drawer-like chambers through which test materials are inserted into the main chamber while maintaining a chilled vacuum state. The chamber can take several days to reach test conditions, and opening it to insert new test materials starts the process all over again. The load locks allowed engineers to make quick adjustments during boot and glove tests.
Cryocoolers chill the chamber, and aluminum blocks inside can simulate tools astronauts might grab or the cold lunar surface on which they’d walk. The chamber also features a robotic arm to interact with test materials, plus multiple visible-light and infrared cameras to record operations.
Testing Extremities
The gloves tested in the chamber are the sixth version of a glove NASA began using in the 1980s, part of a spacesuit design called the Extravehicular Mobility Unit. Optimized for spacewalks at the International Space Station, the suit is so intricate it’s essentially a personal spacecraft. Testing in CITADEL at minus 352 F (minus 213 C) showed the legacy glove would not meet thermal requirements in the more challenging environment of the lunar South Pole. Results haven’t yet been fully analyzed from boot testing, which used a lunar surface suit prototype called the Exploration Extravehicular Mobility Unit. NASA’s reference design of an advanced suit architecture, this spacesuit features enhanced fit, mobility, and safety.
In addition to spotting vulnerabilities with existing suits, the CITADEL experiments will help NASA prepare criteria for standardized, repeatable, and inexpensive test methods for the next-generation lunar suit being built by Axiom Space — the Axiom Extravehicular Mobility Unit, which NASA astronauts will wear during the Artemis III mission.
“This test is looking to identify what the limits are: How long can that glove or boot be in that lunar environment?” said Shane McFarland, technology development lead for the Advanced Suit Team at NASA Johnson. “We want to quantify what our capability gap is for the current hardware so we can give that information to the Artemis suit vendor, and we also want to develop this unique test capability to assess future hardware designs.”
In the past, astronauts themselves have been part of thermal testing. For gloves, an astronaut inserted a gloved hand into a chilled “glove box,” grabbed a frigid object, and held it until their skin temperature dropped as low as 50 F (10 C). McFarland stressed that such human-in-the-loop testing remains essential to ensuring future spacesuit safety but doesn’t produce the consistent data the team is looking for with the CITADEL testing.
To obtain objective feedback, the CITADEL testing team used a custom-built manikin hand and foot. A system of fluid loops mimicked the flow of warm blood through the appendages, while dozens of temperature and heat flux sensors provided data from inside gloves and boots.
“By using CITADEL and modern manikin technology, we can test design iterations faster and at much lower cost than traditional human-in-the-loop testing,” said Morgan Abney, NASA technical fellow for Environmental Control and Life Support, who conceived the glove testing effort. “Now we can really push the envelope on next-generation suit designs and have confidence we understand the risks. We’re one step closer to landing astronauts back on the Moon.”
Through Artemis, NASA will send astronauts to explore the Moon for scientific discovery, economic benefits, and build the foundation for the first crewed missions to Mars.
Houston, We Have a Podcast: next-generation spacesuits Why NASA’s Perseverance rover carries spacesuit materials News Media Contact
Melissa Pamer
Jet Propulsion Laboratory, Pasadena, Calif.
626-314-4928
melissa.pamer@jpl.nasa.gov
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Last Updated Apr 24, 2025 Related Terms
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By USH
UVB-76, widely known by its nickname "The Buzzer," is a mysterious shortwave Russian radio station radio broadcasts in the world. It began broadcasting in the mid-1970s and is still active today, broadcasting cryptic signals at 4625 kHz.
This Russian shortwave station usual broadcast consists of a monotonous buzzing tone that occasionally breaks for cryptic voice messages in Russian. The station is widely believed to be operated by the Russian military, possibly as part of the Strategic Rocket Forces’ communication network.
The use of shortwave radio enables the signal to travel vast distances, potentially covering all of Russia and extending far beyond its borders.
Due to the high transmission power of UVB-76’s antenna, some theorize that the station’s signals could even reach outer space. This possibility opens the door to even more extraordinary speculation: that satellites might receive these signals and relay them to submarines, remote military units, or even unidentified aerial phenomena (UFOs). One theory even posits that UVB-76 could be part of an experimental system designed to scan or communicate with extraterrestrial life.
Under normal circumstances, UVB-76’s broadcasts are infrequent and minimal, just the repetitive buzz and the rare coded message. However, something highly unusual happened just ten hours ago. Within a single day, the station transmitted four coded voice messages, an event considered extremely rare and potentially significant.
These are the messages: NZHTI - 33 702 - NEPTUN - 66-52-20-75 NZHTI - 8002 361 - TIMUS - 56-85 NZHTI - 7000 0 8002 - LISOPLASH - 67-203-0808-0809 NZHTI - 62 505 - NUTOBAKS - 78 15 92 71
While the true meaning of these messages remains classified or unknown, some analysts believe they could be activation codes, operational signals, or test messages for military units. The repeated prefix "NZHTI" could be a call sign or an authentication marker. The names—NEPTUN, TIMUS, LISOPLASH, and NUTOBAKS, might refer to code-named operations, geographic regions, or military assets. The numeric sequences could represent coordinates, timestamps, or identification numbers.
Given the timing and unusual frequency of these messages, some suspect that UVB-76 is ramping up activity in preparation for a significant event. While there's no confirmation of any immediate threat, the sudden uptick in coded communications suggests that something serious could be developing.
Many experts believe UVB-76 is maintained as a wartime contingency channel, ready to relay commands in the event of nuclear war or a catastrophic loss of national communications. Its consistent presence, even during peacetime, supports the theory that it serves as an emergency or fail-safe communication method for defense forces.
The sudden surge of messages within one day suggests that something serious is happening, or about to. But who are they intended for? And more importantly, what comes next?" View the full article
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By NASA
NASA Men stand in front of turning vanes inside the Altitude Wind Tunnel (AWT) at the National Advisory Committee for Aeronautics Aircraft Engine Research Laboratory in this February 1944 publicity photo. The photo was taken just weeks after the tunnel became operational.
The AWT was the only wind tunnel capable of testing full-size aircraft engines in simulated altitude conditions. A large wooden drive fan, located on the other side of these vanes, created wind speeds up to 500 miles per hour. Each corner of the rectangular tunnel had turning vanes, which straightened the airflow and directed it around the corners. This set of vanes was in the 31-foot-diameter southeast corner of the tunnel. These elliptical panels consisted of 36 to 42 vertical vanes that were supported by three horizontal supports. The individual vanes were 2.5 feet long and half-moon shaped. Each set of vanes took weeks to assemble before they were installed during the summer of 1943.
The Aircraft Engine Research Laboratory went through several name updates and changes through NACA and NASA history; it is now NASA’s Glenn Research Center in Cleveland.
Image credit: NASA
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By NASA
NASA The instrument enclosure of NASA’s Near-Earth Object Surveyor is prepared for critical environmental tests inside the historic Chamber A at the Space Environment Simulation Laboratory at NASA’s Johnson Space Center in Houston in December 2024. Wrapped in silver thermal blanketing, the 12-foot-long (3.7-meter-long) angular structure was subjected to the frigid, airless conditions that the spacecraft will experience when in deep space. The cavernous thermal-vacuum test facility is famous for testing the Apollo spacecraft that traveled to the Moon in the 1960s and ’70s.
The instrument enclosure is designed to protect the spacecraft’s infrared telescope while also removing heat from it during operations. After environmental testing was completed, the enclosure returned to NASA’s Jet Propulsion Laboratory in Southern California for further work, after which it will ship to the Space Dynamics Laboratory (SDL) in Logan, Utah, and be joined to the telescope. Both the instrument enclosure and telescope were assembled at JPL.
As NASA’s first space-based detection mission specifically designed for planetary defense, NEO Surveyor will seek out, measure, and characterize the hardest-to-find asteroids and comets that might pose a hazard to Earth. While many near-Earth objects don’t reflect much visible light, they glow brightly in infrared light due to heating by the Sun. The spacecraft’s telescope, which has an aperture of nearly 20 inches (50 centimeters), features detectors sensitive to two infrared wavelengths in which near-Earth objects re-radiate solar heat.
More information about NEO Surveyor is available at: https://science.nasa.gov/mission/neo-surveyor/
Image credit: NASA
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By NASA
Explore This Section Webb News Latest News Latest Images Blog (offsite) Awards X (offsite – login reqd) Instagram (offsite – login reqd) Facebook (offsite- login reqd) Youtube (offsite) Overview About Who is James Webb? Fact Sheet Impacts+Benefits FAQ Science Overview and Goals Early Universe Galaxies Over Time Star Lifecycle Other Worlds Observatory Overview Launch Orbit Mirrors Sunshield Instrument: NIRCam Instrument: MIRI Instrument: NIRSpec Instrument: FGS/NIRISS Optical Telescope Element Backplane Spacecraft Bus Instrument Module Multimedia About Webb Images Images Videos What is Webb Observing? 3d Webb in 3d Solar System Podcasts Webb Image Sonifications Team International Team People Of Webb More For the Media For Scientists For Educators For Fun/Learning 6 Min Read NASA’s Webb Peers Deeper into Mysterious Flame Nebula
This collage of images from the Flame Nebula shows a near-infrared light view from NASA’s Hubble Space Telescope on the left, while the two insets at the right show the near-infrared view taken by NASA’s James Webb Space Telescope. Credits:
NASA, ESA, CSA, M. Meyer (University of Michigan), A. Pagan (STScI) The Flame Nebula, located about 1,400 light-years away from Earth, is a hotbed of star formation less than 1 million years old. Within the Flame Nebula, there are objects so small that their cores will never be able to fuse hydrogen like full-fledged stars—brown dwarfs.
Brown dwarfs, often called “failed stars,” over time become very dim and much cooler than stars. These factors make observing brown dwarfs with most telescopes difficult, if not impossible, even at cosmically short distances from the Sun. When they are very young, however, they are still relatively warmer and brighter and therefore easier to observe despite the obscuring, dense dust and gas that comprises the Flame Nebula in this case.
NASA’s James Webb Space Telescope can pierce this dense, dusty region and see the faint infrared glow from young brown dwarfs. A team of astronomers used this capability to explore the lowest mass limit of brown dwarfs within the Flame Nebula. The result, they found, were free-floating objects roughly two to three times the mass of Jupiter, although they were sensitive down to 0.5 times the mass of Jupiter.
“The goal of this project was to explore the fundamental low-mass limit of the star and brown dwarf formation process. With Webb, we’re able to probe the faintest and lowest mass objects,” said lead study author Matthew De Furio of the University of Texas at Austin.
Image A: Flame Nebula: Hubble and Webb Observations
This collage of images from the Flame Nebula shows a near-infrared light view from NASA’s Hubble Space Telescope on the left, while the two insets at the right show the near-infrared view taken by NASA’s James Webb Space Telescope. Much of the dark, dense gas and dust, as well as the surrounding white clouds within the Hubble image, have been cleared in the Webb images, giving us a view into a more translucent cloud pierced by the infrared-producing objects within that are young stars and brown dwarfs. Astronomers used Webb to take a census of the lowest-mass objects within this star-forming region.
The Hubble image on the left represents light at wavelengths of 1.05 microns (filter F105W) as blue, 1.3 microns (F130N) as green, and 1.39 microns (F129M) as red. The two Webb images on the right represent light at wavelengths of 1.15 microns and 1.4 microns (filters F115W and F140M) as blue, 1.82 microns (F182M) as green, 3.6 microns (F360M) as orange, and 4.3 microns (F430M) as red. NASA, ESA, CSA, M. Meyer (University of Michigan), A. Pagan (STScI) Smaller Fragments
The low-mass limit the team sought is set by a process called fragmentation. In this process large molecular clouds, from which both stars and brown dwarfs are born, break apart into smaller and smaller units, or fragments.
Fragmentation is highly dependent on several factors with the balance between temperature, thermal pressure, and gravity being among the most important. More specifically, as fragments contract under the force of gravity, their cores heat up. If a core is massive enough, it will begin to fuse hydrogen. The outward pressure created by that fusion counteracts gravity, stopping collapse and stabilizing the object (then known as a star). However, fragments whose cores are not compact and hot enough to burn hydrogen continue to contract as long as they radiate away their internal heat.
“The cooling of these clouds is important because if you have enough internal energy, it will fight that gravity,” says Michael Meyer of the University of Michigan. “If the clouds cool efficiently, they collapse and break apart.”
Fragmentation stops when a fragment becomes opaque enough to reabsorb its own radiation, thereby stopping the cooling and preventing further collapse. Theories placed the lower limit of these fragments anywhere between one and ten Jupiter masses. This study significantly shrinks that range as Webb’s census counted up fragments of different masses within the nebula.
“As found in many previous studies, as you go to lower masses, you actually get more objects up to about ten times the mass of Jupiter. In our study with the James Webb Space Telescope, we are sensitive down to 0.5 times the mass of Jupiter, and we are finding significantly fewer and fewer things as you go below ten times the mass of Jupiter,” De Furio explained. “We find fewer five-Jupiter-mass objects than ten-Jupiter-mass objects, and we find way fewer three-Jupiter-mass objects than five-Jupiter-mass objects. We don’t really find any objects below two or three Jupiter masses, and we expect to see them if they are there, so we are hypothesizing that this could be the limit itself.”
Meyer added, “Webb, for the first time, has been able to probe up to and beyond that limit. If that limit is real, there really shouldn’t be any one-Jupiter-mass objects free-floating out in our Milky Way galaxy, unless they were formed as planets and then ejected out of a planetary system.”
Image B: Low Mass Objects within the Flame Nebula in Infrared Light
This near-infrared image of a portion of the Flame Nebula from NASA’s James Webb Space Telescope highlights three low-mass objects, seen in the insets to the right. These objects, which are much colder than protostars, require the sensitivity of Webb’s instruments to detect them. These objects were studied as part of an effort to explore the lowest mass limit of brown dwarfs within the Flame Nebula.
The Webb images represent light at wavelengths of 1.15 microns and 1.4 microns (filters F115W and F140M) as blue, 1.82 microns (F182M) as green, 3.6 microns (F360M) as orange, and 4.3 microns (F430M) as red. NASA, ESA, CSA, STScI, M. Meyer (University of Michigan) Building on Hubble’s Legacy
Brown dwarfs, given the difficulty of finding them, have a wealth of information to provide, particularly in star formation and planetary research given their similarities to both stars and planets. NASA’s Hubble Space Telescope has been on the hunt for these brown dwarfs for decades.
Even though Hubble can’t observe the brown dwarfs in the Flame Nebula to as low a mass as Webb can, it was crucial in identifying candidates for further study. This study is an example of how Webb took the baton—decades of Hubble data from the Orion Molecular Cloud Complex—and enabled in-depth research.
“It’s really difficult to do this work, looking at brown dwarfs down to even ten Jupiter masses, from the ground, especially in regions like this. And having existing Hubble data over the last 30 years or so allowed us to know that this is a really useful star-forming region to target. We needed to have Webb to be able to study this particular science topic,” said De Furio.
“It’s a quantum leap in our capabilities between understanding what was going on from Hubble. Webb is really opening an entirely new realm of possibilities, understanding these objects,” explained astronomer Massimo Robberto of the Space Telescope Science Institute.
This team is continuing to study the Flame Nebula, using Webb’s spectroscopic tools to further characterize the different objects within its dusty cocoon.
“There’s a big overlap between the things that could be planets and the things that are very, very low mass brown dwarfs,” Meyer stated. “And that’s our job in the next five years: to figure out which is which and why.”
These results are accepted for publication in The Astrophysical Journal Letters.
Image C (Animated): Flame Nebula (Hubble and Webb Comparison)
This animated image alternates between a Hubble Space Telescope and a James Webb Space Telescope observation of the Flame Nebula, a nearby star-forming nebula less than 1 million years old. In this comparison, three low-mass objects are highlighted. In Hubble’s observation, the low-mass objects are hidden by the region’s dense dust and gas. However, the objects are brought out in the Webb observation due to Webb’s sensitivity to faint infrared light. NASA, ESA, CSA, Alyssa Pagan (STScI) The James Webb Space Telescope is the world’s premier space science observatory. Webb is solving mysteries in our solar system, looking beyond to distant worlds around other stars, and probing the mysterious structures and origins of our universe and our place in it. Webb is an international program led by NASA with its partners, ESA (European Space Agency) and CSA (Canadian Space Agency).
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Media Contacts
Laura Betz – laura.e.betz@nasa.gov
NASA’s Goddard Space Flight Center, Greenbelt, Md.
Matthew Brown – mabrown@stsci.edu
Space Telescope Science Institute, Baltimore, Md.
Christine Pulliam – cpulliam@stsci.edu
Space Telescope Science Institute, Baltimore, Md.
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Last Updated Mar 10, 2025 Editor Marty McCoy Contact Laura Betz laura.e.betz@nasa.gov Related Terms
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