(Nov. 3, 2023) NASA astronauts and Expedition 70 Flight Engineers Loral O’Hara, left, and Jasmin Moghbeli, right, work on a spacesuit aboard the International Space Station’s Quest airlock.
NASA
Students from North Carolina and Virginia will have separate opportunities next week to each hear from a NASA astronaut living and working aboard the International Space Station.
The two Earth-to-space calls will air live Tuesday, Jan. 9, on NASA+, NASA Television, and the agency’s website. Learn how to stream NASA TV through a variety of platforms including social media. Follow events online at: https://www.nasa.gov/nasatv.
At 9:20 a.m. EST, NASA astronaut Jasmin Moghbeli will answer prerecorded questions from students at Thales Academy in Raleigh, North Carolina. In preparation for the education downlink, students will participate in an annual Science, Technology, Engineering, and Mathematics Day that will include presentations about the space station by Marc Fusco, one of NASA’s solar system ambassadors. Students also will participate in hands-on activities, including making space related art, building bottle rockets, and launching a model rocket.
Media interested in covering the North Carolina event RSVP no later than 5 p.m. Monday, Jan. 8., should contact Janice Holton at: janice.holton@thalesacademy.org or 919-882-2320.
At 1:05 p.m., NASA astronaut Loral O’Hara will answer prerecorded questions from students across the state of Virginia through an event hosted by the Virginia Space Grant Consortium. These students studied life aboard the space station and participated in a Plant the Moon Challenge where they worked to grow plants in lunar regolith simulant for the Artemis mission.
Media interested in covering the Virginia event must RSVP no later than 4 p.m. on Jan. 8., to Kristyn Damadeo at: kdamadeo@odu.edu or 202-465-5190.
For more than 23 years, astronauts have continuously lived and worked aboard the space station, testing technologies, performing science, and developing the skills needed to explore farther from Earth. Astronauts living in space aboard the orbiting laboratory communicate with NASA’s Mission Control Center in Houston 24 hours a day through the Space Communications and Navigation (SCaN) Near Space Network.
Important research and technology investigations taking place aboard the International Space Station benefits people on Earth and lays the groundwork for future exploration.
As part of Artemis, NASA will send astronauts to the Moon to prepare for future human exploration of Mars. Inspiring the next generation of explorers – the Artemis Generation – ensures America will continue to lead in space exploration and discovery.
See videos and lesson plans highlighting research on the space station at:
Preparations for Next Moonwalk Simulations Underway (and Underwater)
Montage of twelve illustrations depicting futuristic aerospace concepts, including a solar powered glider soaring over the clouds of Venus, a fixed wing electric aircraft flying above a Mars landscape, dish satellite probes scattered across the solar system, flat circular discs floating in space and dotted with hundreds of circle sensors, and a device on the lunar surface with sensing lasers.
Preparations for Next Moonwalk Simulations Underway (and Underwater)
Graphic depiction of Electro-luminescently cooled zero-boil-off propellant depots enabling crewed exploration of Mars
Aaswath Pattabhi Raman
Aaswath Pattabhi Raman University of California, Los Angeles
Exploration of Mars has captivated the public in recent decades with high-profile robotic missions and the images they have acquired seeding our collective imagination. NASA is actively planning for human exploration of Mars and laid out some of the key capabilities that must be developed to execute successful, cost-effective programs that would put human beings on the surface of another planet and bring them home safely. One crucial area where new missions and enabling technologies are needed is the long-duration storage of cryogenic propellants in various space environments; relevant propellants include liquid Hydrogen (LH2) for high specific impulse Nuclear Thermal Propulsion (NTP) which can be deployed in strategic locations in advance of a mission. Such LH2 storage tanks could be used to refill a crewed Mars Transfer Vehicle (MTV) to send and bring astronauts home quickly, safely, and cost-effectively.
We propose a breakthrough mission concept: a cryogenic liquid storage depot capable of storing LH2 with ZBO even in the severe and fluctuating thermal environment of LEO. Our innovative storage depot mission employs thin, lightweight, all-solid-state panels attached to the tank’s deep-space-facing surfaces that utilize a long-understood but as-yet-unrealized cooling technology known as Electro-Luminescent Cooling (ELC) to reject heat from cold solid surfaces as non-equilibrium thermal radiation with orders of magnitude more power density than Planck’s Law permits for equilibrium thermal radiation. Such a depot and tank would drastically lower the cost and complexity of propulsion systems for crewed Mars missions and other deep space exploration by allowing spacecraft to refill propellant tanks after reaching orbit rather than launching on the much larger rocket required to lift the spacecraft in a single-use stage. To achieve ZBO, a storage spacecraft must keep the storage tank’s temperature below the boiling point of the cryogen
(e.g., ≈20 K for liquid H2). Achieving this in LEO-like thermal environments requires both excellent reflectivity toward sunlight and thermal radiation from the Earth and other nearby bodies as well as a power-efficient cooling mechanism to remove what little heat inevitably does leak in, a pair of conditions ideally suited to the the ELC panel concept that enables our mission. By enabling ZBO LH2 storage in LEO, our mission will enable cost-effective, and flexible crewed exploration of Mars. Our mission will also demonstrate capabilities with ancillary benefits to cryogenic storage in terrestrial applications and solid-state cooling technologies more generally.
Preparations for Next Moonwalk Simulations Underway (and Underwater)
Graphic depiction of A revolutionary approach to interplanetary space travel: Studying Torpor in Animals for Space-health in Humans (STASH). Color images (top) and thermal images (bottom) show a model hibernation organism requiring low environmental temperatures for torpor study.
Ryan Sprenger
RyanSprenger Fauna Bio Inc.
The use of non-model organisms in medical research is an expanding field that has already made a significant impact on human health. Insights gleaned from the study of unique mammalian traits are being used to develop novel therapeutic agents. The remarkable phenotype of mammalian hibernation confers unique physiologic and metabolic benefits that are being actively investigated for potential human health applications on Earth. These benefits also hold promise for mitigating many of the physical and mental health risks of space travel. The essential feature of hibernation is an energy-conserving state called torpor, which involves an active and often deep reduction in metabolic rate from baseline homeostasis. Additional potential benefits include the preservation of muscle and bone despite prolonged immobilization and protection against radiation injury. Despite this remarkable potential, the space-based infrastructure needed to study torpor in laboratory rodents does not currently exist, and hibernation in microgravity has never been studied. This is a critical gap in our understanding of hibernation and its potential applications for human spaceflight. We propose to remedy this situation through the design and implementation of STASH, a novel microgravity hibernation laboratory for use aboard the ISS. Some unique and necessary design features include the ability to maintain STASH at temperatures as low as 4°C, adjustable recirculation of animal chamber air enabling the measurement of metabolism via oxygen consumption, and measurement of real-time total ventilation, body temperature, and heart rate. The STASH unit will also feature animal chamber sizes that will accommodate the expected variety of future hibernating and non-hibernating species, boosting its applicability to a variety of studies on the ISS by enabling real-time physiological measurements. The STASH unit is being designed in collaboration with BioServe Space Technologies to be integrated into the Space Automated Biological Laboratory (SABL) unit. This will allow for the achievable and practical application of this research to advance our understanding of both hibernation and mammalian physiology in space. The short-term goals of the STASH project are novel investigations into the basic science of hibernation in a microgravity environment, laying the foundation for application of its potential benefits to human health. These include determining whether hibernation provides the expected protection against bone and muscle loss. The medium-term goals of the project begin developing translational applications of hibernation research. These include using STASH both for testing bioactive molecules that mimic the transcriptional signatures of hibernation and for evaluating methods of inducing synthetic torpor for their ability to provide similar protection. As a long-term goal, during a crewed mission to Mars, human synthetic torpor could act as a relevant countermeasure that would change everything for space exploration, mitigating or eliminating every hazard included in NASA’s RIDGE acronym for the hazards of space travel: Space Radiation, Isolation and Confinement, Distance from Earth, Gravity Fields, and Hostile/Closed Environments. Research performed using STASH will be an essential first step toward acquiring fundamental knowledge about the ability of hibernation to lessen the health risks of space. This knowledge will inform development of both biomimetic drug countermeasures and the future infrastructure needed to support torpor-enabled human astronauts engaged in interplanetary missions. We feel that STASH is the epitome of the high-risk, high-reward projects for which NIAC was established.
Preparations for Next Moonwalk Simulations Underway (and Underwater)
Graphic depiction of LIFA: Lightweight Fiber-based Antenna for Small Sat-Compatible Radiometry
Beijia Zhang
Zhang, BeijiaZhang, Beijia Massachusetts Institute of Technology (MIT), Lincoln Lab
Very large space-based RF antennas can be large and expensive to manufacture and deploy. These problems become more challenging for cases when an array of antennas are needed such as for correlation interferometers that provide high spatial resolution of Earth and space. The proposal will specifically examine the potential applicability of novel fiber-based antennas to L-band radiometry for the purpose of generating high resolution soil moisture and sea surface salinity data. Initial estimates indicate that a x10 improvement on resolution may be possible with long fiber-based antenna arrays. Lincoln Laboratory has been investigating the ability to produce large flexible RF antenna arrays embedded in polymer fibers. These lightweight fibers are flexible enough to be coiled and uncoiled, thus facilitating transport and deployment. The metal that forms the antenna structure and other conductive elements is embedded inside a polymer boule that is heated and drawn to form a novel type of fiber. The resulting fiber thus has multiple materials embedded inside for the ability to support sensing capabilities and other functionalities. Thus, this fiber fabrication process may also lead to a cost-effective means to create very large antennas. This work will include analysis of the required antenna performance and the ability of fiber-based antennas to meet those requirements, deployment strategies, satellite specifics, space tolerance of components and materials, a preliminary system-level design, and concept of operations.
Preparations for Next Moonwalk Simulations Underway (and Underwater)
Graphic depiction of Swarming Proxima Centauri: Coherent Picospacecraft Swarms Over Interstellar Distances
Thomas Eubanks
ThomasEubanks Space Initiatives, Inc.
Tiny gram-scale interstellar probes pushed by laser light are likely to be the only technology capable of reaching another star this century. We presuppose availability by mid-century of a laser beamer powerful enough (~100-GW) to boost a few grams to relativistic speed, lasersails robust enough to survive launch, and terrestrial light buckets (~1-sq.km) big enough to catch our optical signals. Then our proposed representative mission, around the third quarter of this century, is to fly by our nearest neighbor, the potentially habitable world Proxima b, with a large autonomous swarm of 1000s of tiny probes.
Given extreme constraints on launch mass (grams), onboard power (milliwatts), and coms aperture (centimeters to meters), our team determined in our work over the last 3 years that only a large swarm of many probes acting in unison can generate an optical signal strong enough to cross the immense distance back to Earth. The 8-year round-trip time lag eliminates any practical control by Earth, therefore the swarm must possess an extraordinary degree of autonomy, for example, in order to prioritize which data is returned to Earth. Thus, the reader will see that coordinating the swarming of individuals into an effective whole is the dominant challenge for our representative mission to Proxima Centauri b. Coordination in turn rests on establishing a mesh network via low-power optical links and synchronizing probes’ on-board clocks with Earth and with each other to support accurate position-navigation-timing (PNT).
Our representative mission begins with a long string of probes launched one at a time to ~0.2c. After launch, the drive laser is used for signaling and clock synchronization, providing a continual time signal like a metronome. Initial boost is modulated so the tail of the string catches up with the head (“time on target”). Exploiting drag imparted by the interstellar medium (“velocity on target”) over the 20-year cruise keeps the group together once assembled. An initial string 100s to 1000s of AU long dynamically coalesces itself over time into a lens-shaped mesh network #100,000 km across, sufficient to account for ephemeris errors at Proxima, ensuring at least some probes pass close to the target.
A swarm whose members are in known spatial positions relative to each other, having state-of-the-art microminiaturized clocks to keep synchrony, can utilize its entire population to communicate with Earth, periodically building up a single short but extremely bright contemporaneous laser pulse from all of them. Operational coherence means each probe sends the same data but adjusts its emission time according to its relative position, such that all pulses arrive simultaneously at the receiving arrays on Earth. This effectively multiplies the power from any one probe by the number N of probes in the swarm, providing orders of magnitude greater data return.
A swarm would tolerate significant attrition en route, mitigating the risk of “putting all your eggs in one basket,” and enabling close observation of Proxima b from multiple vantage points. Fortunately, we don’t have to wait until mid-century to make practical progress – we can explore and test swarming techniques now in a simulated environment, which is what we propose to do in this work. We anticipate our innovations would have a profound effect on space exploration, complementing existing techniques and enabling entirely new types of missions, for example picospacecraft swarms covering all of cislunar space, or instrumenting an entire planetary magnetosphere. Well before mid-century we foresee a number of such missions, starting in Earth or lunar orbit, but in time extending deep into the outer Solar system. For example, such a swarm could explore the rapidly receding interstellar object 1I/’Oumuamua or the solar gravitational lens. These would both be precursors to the ultimate interstellar mission, but also scientifically valuable in their own right.
Preparations for Next Moonwalk Simulations Underway (and Underwater)
Graphic depiction of Detoxifying Mars: the biocatalytic elimination of omnipresent perchlorates
Lynn Rothschild
LynnRothschild NASA Ames Research Center (ARC)
Water is the lifeblood of human survival and civilization and is critical for our sustained exploration beyond Earth. Fortunately, Mars has plenty of water to sustain our aspirations in the form of subsurface ice. Unfortunately, it is not clean water – it is contaminated by toxic perchlorates. Perchlorate and chlorate are potent oxidizers that cause equipment corrosion and are hazardous to human health even at low concentrations. It is therefore critical that Martian water be detoxified to remove these contaminating solutes before it can be used in propellant production, food production, or human consumption. The scale of anticipated water demand on Mars highlights the shortcomings of traditional water purification approaches, which require either large amounts of consumable materials, high electrical draw, or water pretreatment.
What if we could make the perchlorates just vanish? This is the innovative solution we propose here, taking advantage of the reduction of chlorate and perchlorate to chloride and oxygen being thermodynamically favorable, if kinetically slow. This is the promise of our regenerative perchlorate reduction system, leveraging synthetic biology to take advantage of and improve upon natural perchlorate reducing bacteria. These terrestrial microbes are not directly suitable for off-world use, but their key genes pcrAB and cld, which catalyze the reduction of perchlorates to chloride and oxygen, have been previously identified and well-studied. This proposed work exploits the prior work studying perchlorate-reducing bacteria by engineering this perchlorate reduction pathway into the spaceflight proven Bacillus subtilis strain 168, under the control of a robust, active promoter. This solution is highly sustainable and scalable, and unlike traditional water purification approaches, outright eliminates perchlorates rather than filtering them to dump somewhere nearby.
For Phase I we will explore whether this approach is feasible through these objectives:
Engineer the genes PcrAB and cld into B. subtilis 168 under the control of the strong promoter pVeg and test and quantify the efficacy of perchlorate reduction under the modeled conditions.
Develop B. subtilis strains that secrete the enzymes to test intra- vs extracellular efficacy.
Perform a trade study comparing the performance of biological water detoxification from Objs. 1 & 2 to traditional engineering approaches in terms of mass, power, and crew time.
Delineate a plan to infuse this technology in human Mars missions. Development of our detoxification biotechnology will also lead to more efficient solutions to natural and particularly industrial terrestrial perchlorate contamination on Earth. It will also shine a spotlight on the potential of using life rather than only industrial solutions to address our environmental problems, which may spur further innovations for other terrestrial environmental challenges such as climate change. The system will be launched as inert, dried spores stable at room temperature for years. Upon arrival at Mars, spores will be rehydrated and grown in a bioreactor that meets planetary protection standards. Martian water will be processed by the bioreactor to accomplish perchlorate reduction. Processed water can then be used or further purified as required.
X-ray: NASA/CXC/Penn State Univ./L. Townsley et al.; Optical: NASA/STScI/HST; Infrared: NASA/JPL/CalTech/SST; Image Processing: NASA/CXC/SAO/J. Schmidt, N. Wolk, K. Arcand
A colorful, festive image shows different types of light containing the remains of not one, but at least two, exploded stars. This supernova remnant is known as 30 Doradus B (30 Dor B for short) and is part of a larger region of space where stars have been continuously forming for the past 8 to 10 million years. It is a complex landscape of dark clouds of gas, young stars, high-energy shocks, and superheated gas, located 160,000 light-years away from Earth in the Large Magellanic Cloud, a small satellite galaxy of the Milky Way.
The new image of 30 Dor B was made by combining X-ray data from NASA’s Chandra X-ray Observatory (purple), optical data from the Blanco 4-meter telescope in Chile (orange and cyan), and infrared data from NASA’s Spitzer Space Telescope (red). Optical data from NASA’s Hubble Space Telescope was also added in black and white to highlight sharp features in the image.
A team of astronomers led by Wei-An Chen from the National Taiwan University in Taipei, Taiwan, have used over two million seconds of Chandra observing time of 30 Dor B and its surroundings to analyze the region. They found a faint shell of X-rays that extends about 130 light-years across. (For context, the nearest star to the Sun is about 4 light-years away). The Chandra data also reveals that 30 Dor B contains winds of particles blowing away from a pulsar, creating what is known as a pulsar wind nebula.
When taken together with data from Hubble and other telescopes, the researchers determined that no single supernova explosion could explain what is being seen. Both the pulsar and the bright X-rays seen in the center of 30 Dor B likely resulted from a supernova explosion after the collapse of a massive star about 5,000 years ago. The larger, faint shell of X-rays, however, is too big to have resulted from the same supernova. Instead, the team thinks that at least two supernova explosions took place in 30 Dor B, with the X-ray shell produced by another supernova more than 5,000 years ago. It is also quite possible that even more happened in the past.
This result can help astronomers learn more about the lives of massive stars, and the effects of their supernova explosions.
The paper led by Wei-An Chen describing these results was recently published in the Astronomical Journal. The co-authors of the paper are Chuan-Jui Li, You-Hua Chu, Shutaro Ueda, Kuo-Song Wang, Sheng-Yuan Liu, all from the Institute of Astronomy and Astrophysics, Academia Sinica, in Taipei, Taiwan, and Bo-An Chen from National Taiwan University.
NASA’s Marshall Space Flight Center manages the Chandra program. The Smithsonian Astrophysical Observatory’s Chandra X-ray Center controls science operations from Cambridge, Massachusetts, and flight operations from Burlington, Massachusetts.
Today’s release features a spectacular composite image of a large region of space where stars have been continuously forming for the past eight to ten million years. At the center of this complex landscape of brilliant, colorful gas clouds is a supernova remnant. Known as 30 Doradus B, the remnant likely contains the remains of at least two exploded stars.
The entire image is awash in intricate clouds, and swathes of superheated gas. At our upper lefthand corner is a thick, coral pink and wine-colored cloud with a texture resembling cotton candy. At our lower and upper right is a network of deep red clouds that resemble streaks of thick red syrup floating in water. A layer of wispy blue cloud appears to be present across the entire image, but is most evident at our lower left which is free of overlapping gas. Glowing pink, orange, and purple specks of light, which are stars, dot the image.
In the center of the frame is a bright purple and pink cloud, aglow with brilliant white dots, and streaked with lightning-like veins. This is 30 Doradus B, which is delineated by a faint shell of X-rays identified by Chandra. Within this supernova remnant are high energy shocks and winds of particles blowing away from a pulsar.
News Media Contact
Megan Watzke Chandra X-ray Center Cambridge, Mass. 617-496-7998
Jonathan Deal Marshall Space Flight Center Huntsville, Ala. 256-544-0034
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Preparations for Next Moonwalk Simulations Underway (and Underwater)
While stationary for two weeks during Mars solar conjunction in November 2023, NASA’s Curiosity rover used its front and rear black-and-white Hazcams to capture 12 hours of a Martian day. The rover’s shadow is visible on the surface in these images taken by the front Hazcam.
Videos from the rover show its shadow moving across the Martian surface during a 12-hour sequence while Curiosity remained parked.
When NASA’s Curiosity Mars rover isn’t on the move, it works pretty well as a sundial, as seen in two black-and-white videos recorded on Nov. 8, the 4,002nd Martian day, or sol, of the mission. The rover captured its own shadow shifting across the surface of Mars using its black-and-white Hazard-Avoidance Cameras, or Hazcams.
Instructions to record the videos were part of the last set of commands beamed up to Curiosity just before the start of Mars solar conjunction, a period when the Sun is between Earth and Mars. Because plasma from the Sun can interfere with radio communications, missions hold off on sending commands to Mars spacecraft for several weeks during this time. (The missions weren’t totally out of contact: They still radioed back regular health check-ins throughout conjunction.)
Rover drivers normally rely on Curiosity’s Hazcams to spot rocks, slopes, and other hazards that may be risky to traverse. But because the rover’s other activities were intentionally scaled back just prior to conjunction, the team decided to use the Hazcams to record 12 hours of snapshots for the first time, hoping to capture clouds or dust devils that could reveal more about the Red Planet’s weather.
When the images came down to Earth after conjunction, scientists didn’t see any weather of note, but the pair of 25-frame videos they put together do capture the passage of time. Extending from 5:30 a.m. to 5:30 p.m. local time, the videos show Curiosity’s silhouette shifting as the day moves from morning to afternoon to evening.
The first video, featuring images from the front Hazcam, looks southeast along Gediz Vallis, a valley found on Mount Sharp. Curiosity has been ascending the base of the 3-mile-tall (5-kilometer-tall) mountain, which sits in Gale Crater, since 2014.
As the sky brightens during sunrise, the shadow of the rover’s 7-foot (2-meter) robotic arm moves to the left, and Curiosity’s front wheels emerge from the darkness on either side of the frame. Also becoming visible at left is a circular calibration target mounted on the shoulder of the robotic arm. Engineers use the target to test the accuracy of the Alpha Particle X-ray Spectrometer, an instrument that detects chemical elements on the Martian surface.
In the middle of the day, the front Hazcam’s autoexposure algorithm settles on exposure times of around one-third of a second. By nightfall, that exposure time grows to more than a minute, causing the typical sensor noise known as “hot pixels” that appears as white snow across the final image.
Curiosity’s rear Hazcam captured the shadow of the back of the rover in this 12-hour view looking toward the floor of Gale Crater. A variety of factors caused several image artifacts, including a black speck, the distorted appearance of the Sun, and the rows of white pixels that streak out from the Sun.
NASA/JPL-Caltech
The second video shows the view of the rear Hazcam as it looks northwest down the slopes of Mount Sharp to the floor of Gale Crater. The rover’s right rear wheel is visible, along with the shadow of Curiosity’s power system. A small black artifact that appears at the left midway through the video, during the 17th frame, resulted from a cosmic ray hitting the camera sensor. Likewise, the bright flashing and other noise at the end of the video are the result of heat from the spacecraft’s power system affecting the Hazcam’s image sensor.
These images have been re-projected to correct the wide-angle lenses of the Hazcams. The speckled appearance of the images, especially prominent in the rear-camera video, is due to 11 years of Martian dust settling on the lenses.
More About the Mission
Curiosity was built by NASA’s Jet Propulsion Laboratory, which is managed by Caltech in Pasadena, California. JPL leads the mission on behalf of NASA’s Science Mission Directorate in Washington.
Preparations for Next Moonwalk Simulations Underway (and Underwater)
At the end of a long-haul road trip, it might be time to kick up your feet and rest awhile – especially if it was a seven-year, 4 billion-mile journey to bring Earth a sample of asteroid Bennu. But OSIRIS-REx (Origins, Spectral Interpretation, Resource Identification and Security – Regolith Explorer), the NASA mission that accomplished this feat in September, is already well on its way (with a new name) to explore a new destination.
When OSIRIS-REx left Bennu in May 2021 with a sample aboard, its instruments were in great condition, and it still had a quarter of its fuel left. So instead of shutting down the spacecraft after it delivered the sample, the team proposed to dispatch it on a bonus mission to asteroid Apophis, with an expected arrival in April 2029. NASA agreed, and OSIRIS-APEX (Origins, Spectral Interpretation, Resource Identification, and Security – Apophis Explorer) was born.
A Rare Opportunity at Apophis
After considering several destinations (including Venus and various comets), NASA chose to send the spacecraft to Apophis, an “S-type” asteroid made of silicate materials and nickel-iron – a fair bit different than the carbon-rich, “C-type” Bennu.
The intrigue of Apophis is its exceptionally close approach of our planet on April 13, 2029. Although Apophis will not hit Earth during this encounter or in the foreseeable future, the pass in 2029 will bring the asteroid within 20,000 miles (32,000 kilometers) of the surface – closer than some satellites, and close enough that it could be visible to the naked eye in the Eastern Hemisphere.
Scientists estimate that asteroids of Apophis’ size, about 367 yards across (about 340 meters), come this close to Earth only once every 7,500 years.
These images of asteroid Apophis were recorded in March 2021 by radio antennas at the Deep Space Network’s Goldstone complex in California and the Green Bank Telescope in West Virginia. The asteroid was 10.6 million miles (17 million kilometers) away, and each pixel has a resolution of 127 feet (38.75 meters).
Credit: NASA/JPL-Caltech and NSF/AUI/GBO
“OSIRIS-APEX will study Apophis immediately after such a pass, allowing us to see how its surface changes by interacting with Earth’s gravity,” said Amy Simon, the mission’s project scientist based at NASA’s Goddard Space Flight Center in Greenbelt, Maryland.
Apophis’ close encounter with Earth will change the asteroid’s orbit and the length of its 30.6-hour day. The encounter also may cause quakes and landslides on the asteroid’s surface that could churn up material and uncover what lies beneath.
“The close approach is a great natural experiment,” said Dani Mendoza DellaGiustina, principal investigator for OSIRIS-APEX at the University of Arizona in Tucson. “We know that tidal forces and the accumulation of rubble pile material are foundational processes that could play a role in planet formation. They could inform how we got from debris in the early solar system to full-blown planets.”
Apophis represents more than just the opportunity to learn more about how solar systems and planets form: As it happens, most of the known potentially hazardous asteroids (those whose orbits come within 4.6 million miles of Earth) are also S-types. What the team learns about Apophis can inform planetary defense research, a top priority for NASA.
OSIRIS-APEX: Travel Itinerary
By April 2, 2029 – around two weeks before Apophis’ close encounter with Earth – OSIRIS-APEX’s cameras will begin taking images of the asteroid as the spacecraft catches up to it. Apophis will also be closely observed by Earth-based telescopes during this time. But in the hours after the close encounter, Apophis will appear too near the Sun in the sky to be observed by ground-based optical telescopes. This means any changes triggered by the close encounter will be best detected by the spacecraft.
This animation depicts the orbital trajectory of asteroid 99942 Apophis as it zooms safely past Earth on April 13, 2029. Earth’s gravity will slightly deflect the trajectory as the 1,100-foot-wide (340-meter-wide) near-Earth object comes within 20,000 miles (32,000 kilometers) of our planet’s surface. The motion has been sped up 2,000 times. Credit: NASA/JPL-Caltech
OSIRIS-APEX will arrive at the asteroid on April 13, 2029, and operate in its proximity for about the next 18 months. In addition to studying changes to Apophis caused by its Earth encounter, the spacecraft will conduct many of the same investigations OSIRIS-REx did at Bennu, including using its instrument suite of imagers, spectrometers, and a laser altimeter to closely map the surface and analyze its chemical makeup.
As an encore, OSIRIS-APEX will reprise one of OSIRIS-REx’s most impressive acts (minus sample collection), dipping within 16 feet of the asteroid’s surface and firing its thrusters downward. This maneuver will stir up surface rocks and dust to give scientists a peek at the material that lies below.
Although the rendezvous with Apophis is more than five years away, the next milestone on its journey is the first of six close Sun passes. Those near approaches, along with three gravity assists from Earth, will put OSIRIS-APEX on course to reach Apophis in April 2029.
What OSIRIS-APEX will discover about Apophis remains to be seen, but if the mission’s previous incarnation is any indication, surprising science lies ahead. “We learned a lot at Bennu, but now we’re armed with even more questions for our next target,” Simon said.
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NASA’s Goddard Space Flight Center provides overall mission management, systems engineering, and the safety and mission assurance for OSIRIS-APEX. Dani Mendoza DellaGiustina of the University of Arizona, Tucson, is the principal investigator. The university leads the science team and the mission’s science observation planning and data processing. Lockheed Martin Space in Littleton, Colorado, built the spacecraft and provides flight operations. Goddard and KinetX Aerospace are responsible for navigating the OSIRIS-APEX spacecraft. International partnerships on this mission include the spacecraft’s laser altimeter instrument from CSA (the Canadian Space Agency) and science collaboration with JAXA’s (the Japan Aerospace Exploration Agency) Hayabusa2 mission. OSIRIS-APEX (previously named OSIRIS-REx) is the third mission in NASA’s New Frontiers Program, managed by NASA’s Marshall Space Flight Center in Huntsville, Alabama, for the agency’s Science Mission Directorate in Washington.
By Lonnie Shekhtman and Rob Garner NASA’s Goddard Space Flight Center, Greenbelt, Md.
This NASA Hubble Space Telescope photo of Saturn reveals the planet’s cloud bands and a phenomenon called ring spokes.
NASA, ESA, STScI, Amy Simon (NASA-GSFC)
This photo of Saturn was taken by NASA’s Hubble Space Telescope on October 22, 2023, when the ringed planet was approximately 850 million miles from Earth. Hubble’s ultra-sharp vision reveals a phenomenon called ring spokes.
Saturn’s spokes are transient features that rotate along with the rings. Their ghostly appearance only persists for two or three rotations around Saturn. During active periods, freshly-formed spokes continuously add to the pattern.
In 1981, NASA’s Voyager 2 first photographed the ring spokes. NASA’s Cassini orbiter also saw the spokes during its 13-year-long mission that ended in 2017.
Hubble continues observing Saturn annually as the spokes come and go. This cycle has been captured by Hubble’s Outer Planets Atmospheres Legacy (OPAL) program that began nearly a decade ago to annually monitor weather changes on all four gas-giant outer planets.
Hubble’s crisp images show that the frequency of spoke apparitions is seasonally driven, first appearing in OPAL data in 2021 but only on the morning (left) side of the rings. Long-term monitoring show that both the number and contrast of the spokes vary with Saturn’s seasons. Saturn is tilted on its axis like Earth and has seasons lasting approximately seven years.
“We are heading towards Saturn equinox, when we’d expect maximum spoke activity, with higher frequency and darker spokes appearing over the next few years,” said the OPAL program lead scientist, Amy Simon of NASA’s Goddard Space Flight Center in Greenbelt, Maryland.
This year, these ephemeral structures appear on both sides of the planet simultaneously as they spin around the giant world. Although they look small compared with Saturn, their length and width can stretch longer than Earth’s diameter!
“The leading theory is that spokes are tied to Saturn’s powerful magnetic field, with some sort of solar interaction with the magnetic field that gives you the spokes,” said Simon. When it’s near the equinox on Saturn, the planet and its rings are less tilted away from the Sun. In this configuration, the solar wind may more strongly batter Saturn’s immense magnetic field, enhancing spoke formation.
Planetary scientists think that electrostatic forces generated from this interaction levitate dust or ice above the ring to form the spokes, though after several decades no theory perfectly predicts the spokes. Continued Hubble observations may eventually help solve the mystery.
This Hubble Space Telescope time-lapse series of Saturn images (taken on October 22, 2023) resolves a phenomenon called ring spokes appearing on both sides of the planet simultaneously as they spin around the giant world. The video zooms into one set of spokes on the morning (left) side of the rings. The spokes are transient features that rotate along the ring plane. The spokes may be a product of electrostatic forces generated by the interaction of the planet’s magnetic field with the solar wind. This interaction levitates dust or ice above the ring to form the spokes. Credit: NASA, Amy Simon (NASA-GSFC);
Animation:
Joseph DePasquale (STScI)
The Hubble Space Telescope is a project of international cooperation between NASA and ESA. NASA’s Goddard Space Flight Center in Greenbelt, Maryland, manages the telescope. The Space Telescope Science Institute (STScI) in Baltimore, Maryland, conducts Hubble and Webb science operations. STScI is operated for NASA by the Association of Universities for Research in Astronomy, in Washington, D.C.
Preparations for Next Moonwalk Simulations Underway (and Underwater)
NASA Pathways Intern Raquel Cervantes Espinosa is pictured at NASA’s Stennis Space Center near the Fred Haise Test Stand, where she worked throughout the fall semester supporting RS-25 engine testing. Cervantes Espinosa will return to NASA Stennis in the summer following the spring semester at Duke University in Durham, North Carolina.
NASA/Danny Nowlin
A first-generation student from North Carolina will return to school in January feeling more motivated and better connected to her future thanks to time invested as a NASA Pathways Intern at NASA’s Stennis Space Center near Bay St. Louis, Mississippi.
Raquel Cervantes Espinosa, the first member of her family to attend college and a rising junior at Duke University, applied to the internship at NASA Stennis because of opportunities the site presented, such as working with large rocket engines. She admits to initially being nervous, having never traveled to Mississippi or the Gulf Coast area.
The electrical engineering major says she was welcomed with open arms. She grew fond of the diverse and highly skilled workforce that showed how her studies apply to working with NASA, which makes leaving after the fall semester bittersweet.
“It feels like NASA is really investing in me as an individual, and the people that I work with make it feel that way, too,” Cervantes Espinosa said. “I feel valued here and feel like I can grow with my career and degree studies in terms of what I want to do in the future. I really enjoyed my time at NASA Stennis during the fall and look forward to returning in the summer.”
During the fall semester, Cervantes Espinosa worked with test stand camera systems, including those in support of NASA’s certification test series of the RS-25 engine. The series will lead to production of updated engines that will help power future Artemis missions to the Moon and beyond on the SLS (Space Launch System) rocket.
“Raquel had a great first semester as a Pathways Intern learning about various electrical and mechanical systems,” said David Carver, deputy branch chief of the Electrical Operations Branch at NASA Stennis. “Her shining accomplishment for the semester was the new test operations video system that she helped design and bring online. The system will provide test engineers with new insight into the operation and health of critical propulsion systems. I look forward to seeing what she accomplishes in the future.”
The thermal visual cameras set up by Cervantes Espinosa at the Fred Haise Test Stand, where RS-25 hot fires take place, help ensure safe operations by allowing engineers to monitor key areas of the test stand, such as the liquid oxygen stalls and hydrogen systems. The cameras can also identify potential gas leaks not seen with the naked eye. Additionally, Cervantes Espinosa had the opportunity to analyze data and work on instruments that are used on the RS-25 engine.
“A lot of the experience I’m getting from working at NASA Stennis, a lot of the stuff I’m learning now, is really shaping how I see engineering differently than I used to,” she said.
The Duke student says one key takeaway from the fall semester was learning beyond electrical engineering and understanding how her physics minor can be applied in the aerospace industry – an industry she now wants to join following graduation.
On pace to graduate in 2026, Cervantes Espinosa said it can be challenging at times in unfamiliar territory, whether as an intern at NASA Stennis or as a first-generation engineering student.
“I would encourage other first-generation students to keep your head up and keep going,” Cervantes Espinosa said. “It sounds very cliché, but I think it’s really accurate for people like me and a lot of my friends who are first-generation students in engineering and beginning to immerse ourselves into the workforce and see what we need to do. Keep your head up, keep going, and really take advantage of such opportunities because they are out there, and people want the best for you and want to invest in you. You just have to go and seize the opportunity.”
The NASA Pathways Intern Program opens in the spring and fall each year with job postings on USAJobs.gov. The application windows open two times each year – typically around February and September.
For information about the NASA Pathways program, visit:
Stay connected with the mission on social media, and let people know you’re following it on X, Facebook, and Instagram using the hashtags #NASAStennis #Pathways #Artemis. Follow and tag these accounts:
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