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Sand dunes meet stacked ice at Mars’s north pole
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By European Space Agency
ESA’s Mars Express has captured an astonishing array of landforms emerging from a thick winter blanket of frost as spring arrives in the south polar region of Mars. Some of these features are surprisingly dark compared with their icy surroundings, earning their nickname of ‘cryptic terrain’.
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By NASA
Curiosity Navigation Curiosity Home Mission Overview Where is Curiosity? Mission Updates Science Overview Instruments Highlights Exploration Goals News and Features Multimedia Curiosity Raw Images Images Videos Audio More Resources Mars Missions Mars Sample Return Mars Perseverance Rover Mars Curiosity Rover MAVEN Mars Reconnaissance Orbiter Mars Odyssey More Mars Missions The Solar System The Sun Mercury Venus Earth The Moon Mars Jupiter Saturn Uranus Neptune Pluto & Dwarf Planets Asteroids, Comets & Meteors The Kuiper Belt The Oort Cloud 3 min read
Sols 4325-4326: (Not Quite) Dipping Our Toes in the Sand
NASA’s Mars rover Curiosity captured this image using its Left Navigation Camera on Sol 4323 — Martian day 4,323 of the Mars Science Laboratory mission — on Oct. 4, 2024, at 00:29:40 UTC. NASA/JPL-Caltech Earth planning date: Friday, Oct. 4, 2024
If you read this blog very often, you know that nearly every time the rover stops for science, MAHLI and APXS focus on interesting (and accessible!) rocks as targets. The rover science team is, after all, built with a lot of geologists. But geology is not all rocks, all the time — sand is former rock that if buried and pressurized long enough will become rock again. Today was time for sand to shine, as the workspace was cut by troughs of sand of different colors and brightnesses, and it had been nearly 500 sols since we acquired our last dedicated sand measurement with APXS and MAHLI. The “Pumice Flat” target was one of the brighter sand patches while “Kidney Lake” was one of the darker sand patches. APXS uses a special placement mode over sand targets so the instrument gets close, but not too close, to the loose material which could foul up the instrument. Not-rock was also the purview of our environmental observations. Navcam is scheduled for imaging seeking out clouds and dust devils, and changes in the sand and dust on top of the rover deck. Both Navcam and Mastcam will make observations to measure the amount of dust in the atmosphere. REMS will keep track of our weather with regular measurements, RAD will monitor our radiation environment, and DAN will look through rock for signs of water beneath our drive path.
Unsurprisingly, the rest of the rover could not ignore bedrock. We managed to squeeze in DRT cleaning of a nice bedrock slab, “Ribbon Fall,” for MAHLI-only imaging. In places, the bedrock slabs were cut by thin veins of darker gray material, similar to dark gray materials we saw in the bedrock on the other side of Gediz Vallis. ChemCam targeted one of these dark gray examples at “Black Divide,” and also rastered across some of the prominent layers visible in the vertical faces in the workspace at the aptly named “Profile View.”
Our imaging efforts could be roughly divided between looking back at our path through Gediz Vallis from our new and higher perspective, and looking ahead to what awaits us. ChemCam planned RMI mosaics back toward a field of the white stones we spent time studying in Gediz Vallis and toward a part of the edge of Gediz Vallis that we did not explore previously. Mastcam looked back at the part of the edge of Gediz Vallis we just traversed, “Pilot Peak,” for clues as to why it sits higher than the bedrock farther from the channel edge. They also targeted “Clyde Spires,” which was a gravel ridge in Gediz Vallis of interest as we drove by it initially. Looking ahead, Mastcam imaged a puzzling gray rock sitting atop the bedrock slabs south of us at target “Buena Vista Grove,” and further south still, they planned a large mosaic covering a very big rock — the spectacular “Texoli” butte that has loomed and will continue to loom over our path for months to come.
Written by Michelle Minitti, Planetary Geologist at Framework
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Last Updated Oct 07, 2024 Related Terms
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NASA’s LRO: Lunar Ice Deposits are Widespread
Deposits of ice in lunar dust and rock (regolith) are more extensive than previously thought, according to a new analysis of data from NASA’s LRO (Lunar Reconnaissance Orbiter) mission. Ice would be a valuable resource for future lunar expeditions. Water could be used for radiation protection and supporting human explorers, or broken into its hydrogen and oxygen components to make rocket fuel, energy, and breathable air.
Prior studies found signs of ice in the larger permanently shadowed regions (PSRs) near the lunar South Pole, including areas within Cabeus, Haworth, Shoemaker and Faustini craters. In the new work, “We find that there is widespread evidence of water ice within PSRs outside the South Pole, towards at least 77 degrees south latitude,” said Dr. Timothy P. McClanahan of NASA’s Goddard Space Flight Center in Greenbelt, Maryland, and lead author of a paper on this research published October 2 in the Planetary Science Journal.
The study further aids lunar mission planners by providing maps and identifying the surface characteristics that show where ice is likely and less likely to be found, with evidence for why that should be. “Our model and analysis show that greatest ice concentrations are expected to occur near the PSRs’ coldest locations below 75 Kelvin (-198°C or -325°F) and near the base of the PSRs’ poleward-facing slopes,” said McClanahan.
This illustration shows the distribution of permanently shadowed regions (in blue) on the Moon poleward of 80 degrees South latitude. They are superimposed on a digital elevation map of the lunar surface (grey) from the Lunar Orbiter Laser Altimeter instrument on board NASA’s Lunar Reconnaissance Orbiter spacecraft. NASA/GSFC/Timothy P. McClanahan “We can’t accurately determine the volume of the PSRs’ ice deposits or identify if they might be buried under a dry layer of regolith. However, we expect that for each surface 1.2 square yards (square meter) residing over these deposits there should be at least about five more quarts (five more liters) of ice within the surface top 3.3 feet (meter), as compared to their surrounding areas,” said McClanahan. The study also mapped where fewer, smaller, or lower-concentration ice deposits would be expected, occurring primarily towards warmer, periodically illuminated areas.
Ice could become implanted in lunar regolith through comet and meteor impacts, released as vapor (gas) from the lunar interior, or be formed by chemical reactions between hydrogen in the solar wind and oxygen in the regolith. PSRs typically occur in topographic depressions near the lunar poles. Because of the low Sun angle, these areas haven’t seen sunlight for up to billions of years, so are perpetually in extreme cold. Ice molecules are thought to be repeatedly dislodged from the regolith by meteorites, space radiation, or sunlight and travel across the lunar surface until they land in a PSR where they are entrapped by extreme cold. The PSR’s continuously cold surfaces can preserve ice molecules near the surface for perhaps billions of years, where they may accumulate into a deposit that is rich enough to mine. Ice is thought to be quickly lost on surfaces that are exposed to direct sunlight, which precludes their accumulations.
The team used LRO’s Lunar Exploration Neutron Detector (LEND) instrument to detect signs of ice deposits by measuring moderate-energy, “epithermal” neutrons. Specifically, the team used LEND’s Collimated Sensor for Epithermal Neutrons (CSETN) that has a fixed 18.6-mile (30-kilometer) diameter field-of-view. Neutrons are created by high-energy galactic cosmic rays that come from powerful deep-space events such as exploding stars, that impact the lunar surface, break up regolith atoms, and scatter subatomic particles called neutrons. The neutrons, which can originate from up to about a 3.3-foot (meter’s) depth, ping-pong their way through the regolith, running into other atoms. Some get directed into space, where they can be detected by LEND. Since hydrogen is about the same mass as a neutron, a collision with hydrogen causes the neutron to lose relatively more energy than a collision with most common regolith elements. So, where hydrogen is present in regolith, its concentration creates a corresponding reduction in the observed number of moderate-energy neutrons.
“We hypothesized that if all PSRs have the same hydrogen concentration, then CSETN should proportionally detect their hydrogen concentrations as a function of their areas. So, more hydrogen should be observed towards the larger-area PSRs,” said McClanahan.
The model was developed from a theoretical study that demonstrated how similarly hydrogen-enhanced PSRs would be detected by CSETNs fixed-area field-of-view. The correlation was demonstrated using the neutron emissions from 502 PSRs with areas ranging from 1.5 square miles (4 km2) to 417 square miles (1079 km2) that contrasted against their surrounding less hydrogen-enhanced areas. The correlation was expectedly weak for the small PSRs but increased towards the larger-area PSRs.
The research was sponsored by the LRO project science team, NASA’s Goddard Space Flight Center’s Artificial Intelligence Working Group, and NASA grant award number 80GSFC21M0002. The study was conducted using NASA’s LRO Diviner radiometer and Lunar Orbiter Laser Altimeter instruments. The LEND instrument was developed by the Russian Space Agency, Roscosmos by its Space Research Institute (IKI). LEND was integrated to the LRO spacecraft at the NASA Goddard Space Flight Center. LRO is managed by NASA’s Goddard Space Flight Center in Greenbelt, Maryland, for the Science Mission Directorate at NASA Headquarters in Washington.
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Last Updated Oct 03, 2024 Editor wasteigerwald Contact wasteigerwald william.a.steigerwald@nasa.gov Location Goddard Space Flight Center Related Terms
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By European Space Agency
To achieve truly global connectivity, telecommunications satellites are essential. Through the Sunrise Partnership Project with Eutelsat OneWeb – part of Eutelsat Group – and support from the UK Space Agency, ESA is extending advanced 5G connectivity to areas beyond the reach of traditional ground networks.
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By NASA
As systems integration team lead for NASA’s Commercial Low Earth Orbit Development Program (CLDP), Hector Chavez helps build a future where NASA and private industry work together to push the boundaries of space exploration.
With the rise of commercial providers in the space sector, Chavez’s team works to ensure that these companies can develop end-to-end systems to support NASA’s low Earth orbit operations—from transporting crew and cargo to operating mission centers. His team’s role is to assess how commercial providers are using their systems engineering processes to achieve program goals and objectives.
Official portrait of Hector Chavez. NASA/David DeHoyos With a background that spans both the National Nuclear Security Administration and NASA, Chavez brings knowledge and insight into working with interdisciplinary teams to create complex, reliable systems. He has collaborated across organizations, contracts, and government to ensure design and operational improvements were carried out safely and reliably.
“Systems integration brings different systems together to deliver capabilities that can’t be achieved alone,” said Chavez.
His previous role in NASA’s Safety and Mission Assurance office deepened his expertise in mitigating technical risks in human spaceflight by integrating engineering, health, and safety considerations into the development of space exploration vehicles.
Hector Chavez and the team prepare to lift and install a receiver telescope assembly for the Optical Development System, used to test the alignment and performance of the optical systems for NASA’s Ice, Cloud, and land Elevation Satellite-2 mission, in a clean room at Goddard Space Flight Center in Greenbelt, Maryland.NASA Now with CLDP, Chavez helps these companies navigate NASA’s design processes without stifling innovation. “Our challenge is to communicate what we’ve identified during technical reviews without prohibiting commercial partners from developing innovative solutions,” he said.
One recent success was the team’s development of two technical standards for docking systems and payload interfaces that will help ensure these systems’ compatibility with existing technologies. This work is essential in allowing commercial low Earth orbit systems to seamlessly integrate with NASA’s heritage designs, a key step toward realizing the agency’s vision for sustained commercial operations in space.
When asked about the biggest opportunities and challenges in his role, Chavez emphasizes the importance of early collaboration. By engaging with commercial partners at the early stages of the system development life cycle, NASA can provide feedback that shapes the future of commercial low Earth orbit architecture.
“We identify technical issues and lessons learned without dictating design solutions, allowing for innovation while ensuring safety and reliability,” explained Chavez.
Hector Chavez receives an award from the U.S. Department of Energy. Chavez’s approach to leadership and teamwork is rooted in his values of perseverance, integrity, and encouragement. These principles have helped guide the development of CLDP’s mission and vision statements, creating an environment that promotes collaboration and creativity.
He is passionate about building a team culture where people feel empowered to take responsible risks and explore solutions.
Hector Chavez receives a Silver Snoopy Award with his family at NASA’s Johnson Space Center in Houston. NASA As NASA prepares for Artemis missions and the next generation of space explorers, Chavez offers advice to the Artemis Generation: “Never do it alone. Build a community and find common ground to share a vision.”
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