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tahanson43206
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For Void re study of propulsion using ions...

From quick glances at your many posts I get the impression you are trying to learn about many subjects, and you share little bits of the experience with your readers.

In your recent investigation of propulsion using ions, I was inspired to wonder if any atom (metal or not) might be used for acceleration if it is stripped of electrons.  My impression is that cosmic rays are a category of objects which have been accelerated by stellar forces.  My impression is that magnetic fields in space must be the force that provides the acceleration our instruments record.

In your study of this phenomenon, have you discovered anything that humans are doing to replicate what nature does?

(th)

The payoff shows up in two places: the carbon sleeve rotor generates a stronger electromagnetic field than a metal-retained rotor – which is traditionally made from high-strength steel.

The other benefit is that the rotor can sustain higher RPM, since the carbon sleeve largely prevents the copper from expanding outward under radial acceleration.

Both of those things compound: a stronger EM field means more torque from the same amount of current, and higher sustainable RPM means more power from a physically smaller package.

Tesla’s design allows operation in the range of 20,000 rpm – roughly 25% higher than previous motor generations.

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Lightweight Solar Panels for Space Applications
Lightweight solar panels for space are ultra-thin, flexible, and often made from advanced polymers or thin-film cells, enabling deployment on delicate spacecraft surfaces and reducing launch mass.

Why Lightweight Panels Matter in Space
In space, every kilogram of mass affects launch costs and mission design. Traditional rigid panels with glass substrates are heavy and can damage delicate spacecraft surfaces. Lightweight panels reduce structural load, allow for more flexible deployment, and can be integrated into spacecraft skins or deployable structures Renogy+1.

Key Technologies
Thin-film photovoltaics: Materials like amorphous silicon, cadmium telluride, or copper indium gallium selenide (CIGS) are used to make cells thin and flexible Renogy.

Polymer substrates: Instead of glass, advanced polymers or ultra-thin glass reduce weight while maintaining durability Renogy+1.

Flexible cell designs: Apollo Power’s patented flexible solar cells show minimal efficiency loss after impact (0.7% vs. 4.9% for semi-flexible panels) Apollo Power.

Bifacial and high-efficiency cells: Some portable space-grade panels use N-type cells with up to 25% efficiency, capturing more sunlight in constrained orbits energyreservoir.com.

Space-Specific Benefits
Lower launch mass: Reduces fuel and cost for satellite and spacecraft missions.

Adaptability: Can be mounted on curved or non-load-bearing surfaces without structural reinforcement Apollo Power.

Durability: Designed to withstand space radiation, thermal cycling, and micrometeoroid impacts.

Integration: Can be part of deployable solar arrays or integrated into spacecraft hulls for dual-purpose energy and protection.

Examples & Innovations
Apollo Power flexible panels: Fire-resistant, ultra-lightweight, and suitable for industrial, transportation, and space-like mounting environments Apollo Power.

Starpath ultra-thin space solar panels: Recently unveiled, optimized for low-mass, high-efficiency space deployment Payload.

NASA SBSP research: While not yet operational, NASA studies space-based solar power systems that could benefit from lightweight, high-efficiency panels for in-orbit energy collection NASA.

Considerations for Space Use
Radiation hardening: Essential for long-duration missions.

Thermal management: Lightweight panels must handle extreme temperature swings in space.

Deployment reliability: Must unfold or integrate without snagging or damage.

Efficiency vs. weight trade-off: High-efficiency cells are preferred, but ultra-thin designs can match or exceed terrestrial lightweight panel performance Renogy.

In summary, lightweight solar panels for space combine advanced thin-film or polymer-based cells with ultra-low mass and high durability, enabling more efficient spacecraft design, reduced launch costs, and new deployment possibilities. For mission-critical applications, choosing panels with proven radiation and thermal resilience is key.

Space Systems
Super Magdrive rocket thrusters run on heavy metal
By Joe Salas
October 05, 2024

New metal-eating thrusters gobble iron to power spacecraft forever
Any metal, including iron
Magdrive, a space tech startup, has developed a new kind of space thruster that can use any metal, including iron, as a fuel source. The new thruster could, in theory, refuel on the hop by mining asteroids, providing near-infinite ranges if ever deployed.

Melting point    370.944 K (97.794 °C, 208.029 °F)

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Sodium (Na) is a highly reactive, soft, silvery-white alkali metal with atomic number 11, essential for both industrial applications and biological functions.
Basic Properties
Sodium has the chemical symbol Na, derived from the Neo-Latin natrium, and an atomic number of 11. It has an atomic mass of approximately 22.98977 and consists of 11 protons, 12 neutrons, and 11 electrons arranged in three electron shells ([Ne]3s¹)
Wikipedia
Wikipedia
+1
. Sodium is a soft, silvery metal that can be cut with a knife at room temperature and is highly reactive, especially with water, forming sodium hydroxide and hydrogen gas
Wikipedia
Wikipedia
+1
. Its crystal structure is body-centered cubic (BCC) with a lattice constant of 4.23 Å
ChemicalAid
ChemicalAid
.

Occurrence and Compounds
Sodium does not occur freely in nature due to its high reactivity. It is commonly found in minerals such as halite (NaCl), feldspars, sodalite, and natron. Sodium compounds are highly soluble in water, making sodium and chlorine the most abundant dissolved elements in oceans
Wikipedia
Wikipedia
+2
. Common sodium compounds include:

Sodium chloride (NaCl) – table salt, used in food and de-icing roads.
Sodium carbonate (Na₂CO₃) – used in glass, detergents, and water softening.
Sodium hydroxide (NaOH) – used in soap and chemical manufacturing.
Sodium sulfate (Na₂SO₄) – used in paper, glass, and detergents
Encyclopedia Britannica
Encyclopedia Britannica
+1
.
Physical and Chemical Characteristics
Density: 0.97 g/cm³
Melting point: 97.8°C
Boiling point: 882.9°C
Mohs hardness: 0.5
Highly reactive with water and oxygen, forming oxides and hydroxides
Science Notes and Projects
Science Notes and Projects
+1
.
Sodium is lighter than water and must be stored under oil to prevent reaction with moisture in the air
Encyclopedia Britannica
Encyclopedia Britannica
.

Boiling point   
316 °C (601 °F; 589 K) (anhydrous, decomposes)[1]
280 °C (536 °F; 553 K) (hexahydrate, decomposes)

This topic would appear to have significant upside potential, as NewMars members track research and development of more powerful systems.

RobertDyck
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From: Winnipeg, Canada
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Mars Odyssey used a gamma ray sensor to detect thorium. It produced a map of thorium concentration across the surface of Mars. Again, this is based on gamma ray emissions, with assumption that gamma is produced by thorium. On Earth, thorium is used as an indicator element to find uranium. That means, when there's thorium, there's a good likelihood there's also uranium. I have argued thorium itself can be used as fuel in a nuclear reactor.

JPL March 2003: Map of Martian Thorium at Mid-Latitudes  https://www.jpl.nasa.gov/images/pia0425 … latitudes/

NASA same map, but 2 resolutions: Map of Martian Thorium at Mid-Latitudes https://science.nasa.gov/photojournal/m … latitudes/

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Microwave Power Beaming Through Martian Dust Storms
Microwave power beaming — sending energy from a transmitter (e.g., in orbit or on Mars) to a receiver via a focused microwave beam — could work on Mars, even during dust storms, but with important caveats.

How it works
Space power beaming converts electricity into a directed microwave beam, aimed at a rectenna (rectifying antenna) that converts it back into usable power www.satnow.com+1. On Mars, a space-based transmitter could beam energy to a surface receiver, avoiding the need to carry large onboard power systems.

Why dust storms are a concern
Martian dust storms can block sunlight and severely reduce solar array output, as seen with the Opportunity rover in 2018 NASA+1. However, dust particles are small (about 3 micrometers) and the atmosphere is very thin (~6 mbar vs. Earth’s 1000 mbar) space.sciencearray.com. This means scattering of microwaves is less severe than for sunlight, especially at lower frequencies (e.g., 3–6 GHz) Reddit. Lower frequencies penetrate dust better and are less affected by particle size.

Efficiency trade-offs
Studies suggest that even under clear skies, microwave beaming efficiency from orbit to Mars is low — for example, a 6.28 MW satellite source might deliver only 100 kW at the surface Reddit. Dust storms could further reduce efficiency due to beam scattering and absorption, but the effect is likely less than for solar panels, which can be rendered nearly useless during global storms space.sciencearray.com.

Feasibility in storms

Advantage: Microwave beams are less sensitive to dust than sunlight, so they can remain operational during storms, unlike solar arrays Reddit.

Challenge: Atmospheric scattering still occurs, and beam alignment and receiver design must account for dust-induced signal degradation.

Comparison: Surface solar panels are still viable for short-term or local use, but for long-duration or remote operations, beaming could be more reliable Reddit.
Bottom line
Microwave power beaming can work on Mars during dust storms, especially at lower microwave frequencies, but it will be less efficient than in clear conditions. It’s a promising complement to solar power for missions that need continuous energy, but the system design must optimize for low-scattering frequencies, beam stability, and receiver robustness. For now, it’s more of a backup or supplement than a complete replacement for solar in most scenarios.

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Carbon in Electric Devices
Carbon is a versatile material in electrical engineering, used in both traditional and cutting-edge devices due to its unique combination of electrical, thermal, and mechanical properties.

Traditional electrical applications

Filaments in incandescent lamps: Carbon filaments (often from graphite or carbonized materials) have high resistivity and a melting point around 3500°C, making them suitable for lighting applications Electrical4U.

Electrical contacts: Carbon fibers or graphite enhance contact strength, reduce wear, and lower contact resistance in switches and relays Electrical4U.

Resistors: Carbon’s high resistivity, high melting point, and low temperature coefficient make it ideal for fixed resistors in electronic circuits Electrical4U.

Brushes for DC machines and alternators: Graphite carbon brushes offer high thermal stability and improved commutation Electrical4U.

Electrodes: Used in arc lighting, welding, electric furnaces, and battery cell elements Electrical4U.

Electromagnetic shielding: Carbon composites can block electromagnetic interference Personal websites at UB.

Modern and advanced uses

Conductive additives: Carbon black or fibers are added to polymers to improve electrical conductivity in composites Personal websites at UB.

All-carbon conductors: Carbon nanotubes, graphene, and carbon fibers can replace or supplement metal wiring, offering lightweight, flexible, and corrosion-resistant alternatives Frontiers.

Electronic devices: Functionalized carbon materials (graphene, CNTs) are used in sensors, supercapacitors, inkjet printer inks, and wearable electronics MDPI.

High-performance electronics: Carbon nanotubes are being explored as post-silicon transistors, offering high gate controllability and potential to overcome silicon scaling limits MDPI.

Why carbon works
Carbon’s electrical conductivity depends on its structure—graphite conducts well in-plane, while amorphous or low-crystallinity forms are less conductive but mechanically robust Personal websites at UB. Its high thermal stability, chemical inertness, and ability to be engineered at the nanoscale make it adaptable for both simple and complex devices.

In summary, carbon—from graphite filaments to nanotube-based transistors—plays a key role in electric devices, spanning from everyday lighting and contacts to next-generation flexible and high-performance electronics.

Quote:

So, from my point of view we want all three options for Mars:

tahanson43206
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For Void ... in a recent post, in mid July 2026, you offered an intriguing idea that Uranium might be found in the oceans of objects other than the Earth.

This is an idea that needs to be pursued to see if can be supported by evidence, or if it must be labeled as pure speculation.

Please see if one of the AI systems can find evidence to support your interesting idea.

(th)

Uranium on Mars: Potential and Implications
Author: NSE Staff | Published: 12/30/24

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While uranium likely exists on Mars, there is no direct evidence that ancient Martian seas contained uranium salts, though geochemical conditions could have allowed trace amounts to dissolve or precipitate.
Uranium on Mars
Mars is known to contain uranium in its crust, though in lower concentrations than Earth. Geological studies suggest that volcanic activity, sedimentary processes, and hydrothermal systems could have concentrated uranium in certain regions of the Martian crust
newspaceeconomy.ca
newspaceeconomy.ca
+1
. Martian meteorites analyzed on Earth contain trace amounts of uranium, indicating that the element is present in Martian rocks
newspaceeconomy.ca
newspaceeconomy.ca
. Remote sensing has also detected elements like thorium and potassium, which often co-occur with uranium on Earth, suggesting that uranium may exist in similar contexts on Mars
newspaceeconomy.ca
newspaceeconomy.ca
+1
.

Ancient Martian Water and Salt Deposits
Evidence indicates that Mars once had large bodies of liquid water, including oceans in the northern hemisphere and lakes in craters like Jezero
Wikipedia
Wikipedia
+1
. Salt deposits on Mars, primarily composed of magnesium and sulfur compounds similar to Epsom salts, suggest repeated cycles of water evaporation and mineral precipitation
The University of Chicago
The University of Chicago
. These salts formed under conditions that allowed dissolved minerals to concentrate as water evaporated, but analyses so far have not identified uranium salts among them
The University of Chicago
The University of Chicago
.

Possibility of Uranium Salts
On Earth, uranium can form soluble salts in water, particularly under oxidizing conditions, and precipitate as minerals like uraninite or carnotite in sedimentary environments. If Martian seas were chemically similar to terrestrial waters, trace uranium could have dissolved and potentially precipitated as salts in localized areas, especially where hydrothermal activity or volcanic inputs enriched the water with uranium
newspaceeconomy.ca
newspaceeconomy.ca
+1
. However, the dominant salts detected on Mars are magnesium and sulfate-based, and no direct detection of uranium salts has been reported in Martian sediments or evaporites
The University of Chicago
The University of Chicago
.

Conclusion
While Mars has uranium in its crust and ancient seas existed, there is currently no direct evidence that uranium salts were a significant component of Martian waters. It remains plausible that trace amounts could have been present, particularly in regions influenced by volcanic or hydrothermal activity, but the primary salts identified in Martian deposits are magnesium and sulfate compounds
newspaceeconomy.ca
newspaceeconomy.ca
+1
. Future in-situ analyses by rovers or sample return missions may clarify whether uranium ever formed salts in Martian aquatic environments.

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Maximum Warmth of Mars’ North Pole at Extreme Axial Tilt
If Mars’ axial tilt were at its maximum historical value — around 80° — the planet would be nearly “pole-on” to the Sun, with the north pole receiving direct, year-round sunlight Mars Odyssey Mission THEMIS. This would be the opposite of today’s climate, when the north pole is in permanent winter darkness.

At such an extreme tilt, the north pole would be the warmest region on Mars, while the equator and southern hemisphere would be in prolonged darkness and extreme cold Mars Odyssey Mission THEMIS. The warmth would be driven by:

Direct solar irradiance: The north pole would be exposed to sunlight for most of the Martian year, avoiding the long winter shadows that dominate today.

Seasonal CO₂ ice sublimation: In spring, the CO₂ frost covering the north pole would sublimate into the atmosphere, thickening it and potentially triggering dust storms CompleteEra.

Atmospheric circulation: Warm air from the equator would flow toward the pole, but the extreme tilt would still keep the pole in the Sun’s direct beam.

While exact surface temperatures at 80° tilt are not directly measured, climate models suggest that the north pole could warm to several degrees Celsius above today’s average winter temperatures — perhaps in the –20°C to –10°C range in spring/summer — compared to today’s –125°C winter lows CompleteEra+1. This is still far colder than Earth’s tropics, but it would be dramatically warmer than the current Martian north pole.

Key points:

Current north pole winter: ~–125°C, permanent darkness CompleteEra.

At 80° tilt: Direct sunlight year-round, CO₂ ice sublimation, possible dust storms.

Estimated warmth: –20°C to –10°C in spring/summer, much milder than today’s pole.

In short, at maximum tilt, the Martian north pole could become a relatively warm, sunlit region — but still far colder than Earth’s equatorial zones — with seasonal CO₂-driven atmospheric changes.

Does the North Polar ice Cap of Mars press the crust of Mars down?

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Yes — the North Polar ice cap of Mars does press the crust down, but the effect is much smaller and slower than on Earth because of Mars’s cold, stiff interior.

Recent geophysical studies using orbital radar data have shown that the ~3km‑thick ice sheet at Mars’s north pole bends the rocky crust beneath it at a rate of about 0.13mm per year DLR Portal. This is a measurable deformation, but it is far slower than the glacial isostatic adjustment seen on Earth, where ice sheets can depress the crust by many metres over thousands of years.

The reason for this slow response is that Mars’s mantle is highly viscous — roughly 10 to 100 times more viscous than Earth’s DLR Portal. This stiffness means the crust deforms little under the ice’s weight, and the depression is still not large enough to be easily detected from orbit. The ice cap itself is also relatively young, having formed only 2–12million years ago, so the crust has not had enough time to settle significantly TU Delft+1.

In short:

Yes, the ice cap depresses the crust.

The depression is small and slow due to Mars’s cold, stiff mantle.

The ice is young, so the crust is still adjusting downward rather than having fully settled.

This process is similar to glacial isostatic adjustment on Earth, but on Mars it’s a much more gradual and subtle effect.

2–12million years ago

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Formation Timing of Mars’ Mid-Latitude Ice Sheets
Recent research indicates that the mid-latitude subsurface ice on Mars is the remnant of a past ice sheet that formed when the planet’s obliquity (axial tilt) was higher than today, allowing ice to accumulate at lower latitudes arXiv.org.

Using improved Mars climate models, scientists estimate that the ice was emplaced about 630,000 years ago at latitudes of 40–55°N, when obliquity was around 35–40° arXiv.org. This timing explains why the ice today is buried 25–150cm (and up to 255cm in some cases) beneath regolith, with depth variations matching observations. The study concludes that the ice is younger than 4 million years arXiv.org.

However, broader geological and climate modeling shows that Mars was once covered by thick, widespread ice sheets during periods of high obliquity. Around 640 million years ago, the planet likely had a much wetter, colder climate with extensive ice coverage www.t.u-tokyo.ac.jp. Over hundreds of millions of years, obliquity cycles caused ice to advance and retreat, with the most recent major accumulation event occurring about 98 million years ago, when ice was deposited in localized “cold traps” in mid-latitude craters www.t.u-tokyo.ac.jp.

In summary:

Recent buried ice: ~630kyr ago, during a high-obliquity phase (~35–40°) arXiv.org.

Earlier ice sheets: As far back as ~640Myr ago, during a much colder, wetter climate www.t.u-tokyo.ac.jp.

Latest major accumulation: ~98Myr ago, in localized mid-latitude cold traps www.t.u-tokyo.ac.jp.

These findings show that Mars’ mid-latitude ice has a long, multi-stage history, tied directly to changes in the planet’s orbital and axial parameters.

High Altitude Clouds May have warmed Mars in the Past?

Warm early Mars surface enabled by high-altitude water ice clouds
Edwin S. Kite https://orcid.org/0000-0002-1426-1186 kite@uchicago.edu, Liam J. Steele https://orcid.org/0000-0002-6611-0179, Michael A. Mischna https://orcid.org/0000-0002-8022-5319, and Mark I. Richardson https://orcid.org/0000-0001-9633-4141Authors Info & Affiliations
Edited by Mark Thiemens, University of California San Diego, La Jolla, CA, and approved March 10, 2021 (received for review February 4, 2021)
April 26, 2021
118 (18) e2101959118
https://doi.org/10.1073/pnas.2101959118

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High‑Altitude Icy Clouds May Have Warmed Early Mars
A new study suggests that thin layers of icy, high‑altitude clouds could have kept early Mars warm enough to support lakes and rivers for hundreds of years, despite the planet receiving only about one‑third of today’s sunlight University of Chicago News+1.

The Climate Puzzle
Mars today is a cold desert, but geological evidence shows it once had flowing rivers and lakes. Models of a simple greenhouse effect using CO₂ and water vapor alone predict temperatures too cold for liquid water. Earlier ideas, such as asteroid impacts, could not explain the long‑term warmth seen in the geologic record University of Chicago News+1.

The Cloud Greenhouse Hypothesis
The University of Chicago team, led by Edwin Kite, revisited the idea of radiatively active water ice clouds in the upper atmosphere, similar to cirrus clouds on Earth. These clouds can trap heat and create a greenhouse effect, even if they are thin SYFY Official Site.

Why Patchy Ice Matters
The key finding was that warm, stable climates only emerged when surface water ice was patchy, not widespread.

Extensive surface ice led to thick, low clouds that reflected sunlight and cooled the planet.

Patchy ice meant less surface moisture, allowing high‑altitude clouds to form and persist. These clouds warmed the planet by trapping heat, while the arid conditions prevented excessive cloud formation pmc.ncbi.nlm.nih.gov+1.

How the Model Works
Using a 3D global climate model, the researchers simulated:

A dynamic water cycle with cloud particle sedimentation and snow‑out thresholds.

Sublimation of ice particles as they fell, moistening the subcloud layer.

Modest updrafts sustaining large amounts of high‑altitude cloud sseh.uchicago.edu.

The simulations showed Mars could reach average annual temperatures around 265K—warm enough for low‑latitude lakes—and stay that way for centuries pmc.ncbi.nlm.nih.gov.

Implications
This mechanism supports the idea of a warm, arid early Mars climate, consistent with geological data. It also suggests that lakes could have been fed by groundwater upwelling or melting ice during a cold‑to‑warm transition sseh.uchicago.edu.

In short, high‑altitude icy clouds may have been the missing piece in explaining how Mars stayed habitable for so long before it became the cold desert we see today.

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Yes — both Phobos and Deimos contain carbon, but it’s not in the form of free elemental carbon; instead, the carbon is part of carbon-rich surface materials that give them their dark, low-albedo appearance.

Reflectance spectroscopy of both moons shows abundant carbon, which is consistent with a composition similar to carbonaceous chondrites — a type of meteorite rich in organic compounds and carbon-bearing minerals NASA Technical Reports Server (NTRS). This carbon content is not typical of Martian surface materials, suggesting that the moons’ bulk composition is different from Mars itself.

Two main origin scenarios are debated:

Mars-impact origin: The moons may have formed from debris after a giant impact on Mars, with carbon-rich material added later by interplanetary dust particles (IDPs). These IDPs are rich in carbon and are delivered in much higher flux to Mars and its moons than to Earth, so Phobos and Deimos have accumulated significant carbon-rich surface layers over time NASA Technical Reports Server (NTRS).

Captured asteroids: They could be small asteroids from the outer solar system that were captured by Mars’s gravity, bringing their carbon-rich compositions with them.

In either case, the surface of both moons is coated with carbon-rich regolith from IDP infall, which explains their dark color and spectral signature. The carbon is chemically bound in minerals and organic compounds, not as pure elemental carbon.

In summary: Phobos and Deimos do contain carbon, primarily in the form of carbonaceous minerals and organic compounds, with much of the carbon delivered to their surfaces by interplanetary dust over time NASA Technical Reports Server (NTRS). Wikipedia

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Combustion of CO and Methane with Oxygen in Rocket Engines
Yes — a rocket engine can burn a mixture of carbon monoxide (CO) and methane (CH₄) with oxygen (LOX), but the performance and practicality depend on how the two fuels are combined and the operating conditions.

1. CO/O₂ combustion
Carbon monoxide burns readily with liquid oxygen. NASA experiments have shown that CO and LOX can ignite and sustain steady combustion in rocket engine simulations, with ignition boundaries determined for various inlet temperatures NASA Technical Reports Server (NTRS). The specific impulse (Isp) for LOX/CO is relatively low — around 200–290 depending on chamber pressure Space Exploration Stack Exchange — compared to LOX/CH₄ (~299 Isp) Space Exploration Stack Exchange. This means CO/O₂ offers less thrust efficiency per unit of propellant mass.

2. Methane/O₂ combustion
Methane is a well‑tested rocket fuel with LOX, producing high Isp and good stability. It is commonly used in engines like SpaceX’s Raptor.

3. Combining CO and CH₄ with O₂
If you mix CO and CH₄ before injecting into an LOX engine, the mixture will combust, but the performance will be intermediate between the two pure fuel cases. The exact Isp and combustion stability depend on the mole ratio of CO to CH₄, the oxygen enrichment level, and the chamber pressure.

Advantages: CO can be produced in situ from CO₂ (e.g., on Mars via photochemical reduction) without consuming water, unlike the Sabatier reaction for methane Space Exploration Stack Exchange.

Disadvantages: CO has lower energy density than CH₄, so adding it reduces overall Isp unless compensated by higher oxygen enrichment or staged combustion.

Ignition: Both CO and CH₄ ignite with LOX, so a mixture should ignite if the overall mixture ratio is within the LOX/CO ignition range and the CH₄ content is not so high as to shift the mixture outside the LOX/CH₄ range.

4. Practical considerations

Storage: CO liquefies at about -191.5°C, colder than LOX (-183°C), so LOX tanks would need to be insulated to prevent CO from freezing Space Exploration Stack Exchange.

Engine design: Mixing CO and CH₄ in the feed system requires careful control to avoid local fuel-rich or fuel-lean zones.

Mission use: On Mars, CO could be used as a supplement or primary fuel if water is scarce, but for high‑performance missions, LOX/CH₄ remains the preferred choice.

Conclusion
A rocket engine can burn a mix of CO and CH₄ with LOX, but the performance will be lower than pure LOX/CH₄ unless the mixture is optimized for LOX/CO combustion. For in‑situ propellant production on Mars, CO could be a viable alternative or supplement, but it will require careful engineering to match the performance and storage needs of conventional LOX/CH₄ systems

Scientists Have Figured Out How Floating Islands Work
Spongy rocks don’t exactly act like sponges.
by Kelsey Kennedy
May 26, 2017

Pumice rafts
There are islands in the ocean that don’t show up on any map and that no one will also ever set foot on. Known as pumice rafts, these “islands” are made of volcanic rocks, and instead of being anchored to the seafloor they float wherever the currents take them.

The Rock That Floats – Inside Pumice Formation

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Regolith Requirements for Lunar Radiation Protection
For long‑term lunar habitation, lunar regolith is the most practical radiation shield because it’s abundant in place and avoids the high cost of launching shielding from Earth ResearchGate. The amount needed depends on the target radiation dose, regolith density, and the type of radiation (Galactic Cosmic Rays vs. Solar Particle Events).

Typical thicknesses and doses

Galactic Cosmic Rays (GCRs): At least 2m of regolith is needed to reduce exposure to about 150mSv per 180‑day mission. Increasing to 3m reduces this to roughly 100mSv ResearchGate.

Solar Particle Events (SEPs): Regolith is highly effective at stopping SEPs; even 1–2m can significantly reduce dose, with effectiveness increasing with depth ResearchGate.

Optimal depth: NASA simulations show a peak in secondary radiation between 1.0–1.5m, so 2–3m is often used to balance GCR and secondary radiation effects ResearchGate.

Mass estimates

Loose surface regolith has a density of about 1.5–1.8g/cm³ agentcalc.com.

For a 2m layer over 1m²:

Volume = 2m × 1m² = 2m³

Mass ≈ 2m³ × 1.6g/cm³ × 10⁶ cm³/m³ = 3.2tonnes per square meter.

For a 3m layer: ≈ 4.8tonnes/m².
These figures scale with habitat area — a 100m² habitat with 2m regolith shielding would require ~320tonnes of regolith.

Engineering considerations

Compression: Compressing regolith increases density and reduces required thickness, improving both radiation and thermal insulation MDPI.

Mixed materials: Combining regolith with polyethylene or aluminum can improve GCR shielding efficiency ResearchGate.

Secondary radiation: Deeper layers reduce GCR dose but can increase secondary particle production; 2–3m is a common compromise ResearchGate.

Construction logistics: Excavating and placing regolith over large areas requires significant robotic excavation, power, and time agentcalc.com.

Summary table

Regolith thickness    Approx. GCR dose (180d)    Mass per m² (loose)   
Notes

1.0m    ~200–250mSv    1.6tonnes   
Good for SEPs, less for GCRs

2.0m    ~150mSv    3.2tonnes   
Common target for GCR/SEP

3.0m    ~100mSv    4.8tonnes   
Best for GCR, more mass

Bottom line: For a safe long‑term lunar base, 2–3m of regolith is a practical shielding depth, requiring ~3–5 tonnes per square meter of loose material. Compression can reduce this mass, but excavation and placement remain major engineering challenges ResearchGate+1.

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Water Requirements for Radiation Protection on the Moon
On the Moon, there is no atmosphere or magnetic field to shield against space radiation, so lunar regolith (soil) is the primary shielding material. Water can be incorporated into regolith to improve its radiation shielding effectiveness.

1. Water’s role in shielding
Water is effective at absorbing ionizing radiation, especially secondary neutrons produced when high-energy particles strike regolith. Adding water to regolith can increase its shielding efficiency. NASA and other studies found that adding about 2wt% water to regolith particles can improve shielding by roughly 6% NASA Technical Reports Server (NTRS)+1. This is because water has a high hydrogen content, which is excellent for slowing down and absorbing neutrons.

2. How much water is needed
The exact amount depends on the target radiation dose reduction and the baseline shielding. For example:

A two‑meter regolith layer is sufficient for background radiation, but more is needed for major solar particle events lunarpedia.org.

If you want to enhance regolith shielding, 2wt% water (about 20g of water per kilogram of regolith) is a practical starting point for modest improvements NASA Technical Reports Server (NTRS)+1.

For larger dose reductions, higher water content or thicker regolith layers may be required, but water content is limited by the natural water content of the regolith (LCROSS found up to ~5.6wt% in some areas) NASA Technical Reports Server (NTRS).

3. Practical considerations

In-situ water: If water is already present in the regolith (e.g., in permanently shadowed polar craters), it can be used directly.

Ex-situ water: If not available, water must be brought from Earth or produced via in-situ resource utilization (e.g., electrolysis of water ice).

Structural integration: Water can be mixed into regolith during construction or stored in water-rich regolith layers within habitat walls.

4. Summary
For modest radiation shielding improvements, adding ~2wt% water to regolith can boost protection by ~6% NASA Technical Reports Server (NTRS)+1. For full protection, a 2m regolith layer is the baseline, with water content optimized to enhance neutron shielding. The total water mass needed depends on the habitat size and desired dose reduction, but even small percentages can make a significant difference in long-term lunar habitation safety.

China's New Ammonia Powered Engine Has Big Oil In Panic

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Nuclear Rocket Using Liquid CO and Methane Propellants
A nuclear rocket using liquid carbon monoxide (CO) and methane (CH₄) is a concept that blends nuclear thermal propulsion (NTP) with methane–carbon monoxide–liquid oxygen (McLOx) fuel cycles. This approach is being explored for Mars ascent vehicles and other in‑situ propellant production (ISPP) applications.

Why CO + Methane?
Methane/CO mixtures are produced by Mars ISPP systems (e.g., Sabatier reaction byproducts) and can be used directly without costly separation Archive.

CO increases propellant density compared to pure methane, improving stage performance despite a slight drop in specific impulse (Isp) Archive.

Both CO and CH₄ are cryogenic, storable, and compatible with LOX, making them suitable for nuclear thermal engines.

Nuclear Thermal Propulsion (NTP) Basics
In NTP, a nuclear reactor heats a propellant (like liquid hydrogen or liquid methane) to very high temperatures before it expands through a nozzle.

This method can achieve Isp values above 900 s in vacuum, far exceeding chemical rockets (~300–450 s) newspaceeconomy.ca.

For McLOx, the reactor heats the CO/CH₄/LOX mixture, which is then expanded for thrust.
McLOx Advantages
Higher propellant density than pure methane or LOX, reducing tank volume and mass Archive.

Simpler ISPP — no need to purify methane from CO mixtures Archive.

Common storage temperature for CO, CH₄, and LOX allows lightweight, compact tanks Archive.

Potential for reprocessing organic waste from lunar or ISS operations Archive.

Performance Considerations
Isp: McLOx NTP could exceed 370 s in vacuum, with density benefits improving stage performance Archive.

Thrust: Depends on reactor power and propellant flow rate; NTP systems can deliver high, sustained thrust.

Efficiency: Higher Isp means less propellant mass for a given mission, but reactor mass and shielding add complexity.

Applications
Mars ascent vehicles using ISPP‑produced CO/CH₄ mixtures.

Lunar surface operations with waste‑derived propellants.

Future ISPP‑enabled missions where propellant production is done in‑situ.

Challenges
Reactor integration with cryogenic CO/CH₄/LOX handling.

Material compatibility at high temperatures.

Radiation shielding and safety for crewed missions.

Testing infrastructure for nuclear‑powered liquid propellant engines.

In summary: A nuclear rocket using liquid CO and methane is a promising hybrid concept that leverages in‑situ propellant production, high propellant density, and nuclear thermal efficiency for deep‑space and planetary surface missions Archive.

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Iron Foil vs Steel Foil
Iron foil and steel foil are both ultra-thin metal foils, but they differ in composition, properties, and typical applications.

Composition and Purity
Iron foil: Made from high-purity iron (99.5%–99.99% Fe) Goodfellow. It is a pure elemental metal, not an alloy, which gives it excellent magnetic properties.

Steel foil: Made from an alloy of iron and carbon (and sometimes other elements like chromium, nickel, etc.) www.astmsteel.com. Steel’s alloying improves strength, hardness, and corrosion resistance compared to pure iron.

Thickness and Form
Both can be made in very thin gauges (down to ~0.0005 mm for iron foil Goodfellow), but steel foil can be produced in a wider range of alloys and thicknesses, including ultra-thin precision foils for electronics Hamilton Precision Metals.

Iron foil is often supplied in light-tight, pinhole-free forms for sensitive applications Goodfellow.

Key Properties
Iron foil:

High magnetic permeability and low coercivity — ideal for magnetic shielding and electromagnetic devices Goodfellow.

High ductility and formability for thin fabrication.

Moderate electrical and thermal conductivity.

Used in transformers, inductors, magnetic yokes, particle accelerators, and as a substrate for material growth Goodfellow.

Steel foil:

Combines iron’s base properties with alloy-enhanced strength, hardness, and corrosion resistance.

Can be tailored for specific applications like strain gauges, precision resistors, medical devices, and aerospace components Hamilton Precision Metals.

Thicker steel foils may be used for structural or shielding roles, but ultra-thin steel foils are common in electronics and sensors.

Applications
Iron foil: Magnetic shielding, electromagnetic devices, scientific instrumentation, energy systems, and as a substrate for advanced materials Goodfellow.

Steel foil: Electronics (strain gauges, resistors), medical devices, aerospace, automotive sensors, and decorative or protective foils Hamilton Precision Metals+1.

Choosing Between Them
Choose iron foil if your application requires maximum magnetic performance and you can tolerate its lower strength and corrosion resistance.

Choose steel foil if you need strength, durability, and corrosion resistance in a thin form, or if you require alloy-specific properties (e.g., stainless steel for corrosion resistance).

In short, iron foil is the pure, magnetic specialist, while steel foil is the versatile, alloy-enhanced option for a broader range of engineering and industrial uses.

o get started humble beginnings are likely:

Investigation of the Radiation Shielding Capacity of Asphalt and Sand for Fast Neutron Sources

Abstract
The internal wall of the cavity of experimental assemblies, involved with high energy fusion neutrons, can be covered by an asphalt-sand layer for radiation protection purposes. The calculations have demonstrated that asphalt has a radiation protection capability superior to that of concrete, on equivalent weight basis.

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Phobos experiences extreme temperature variations, ranging from about −4°C (25°F) on the sunlit side to −112°C (−170°F) on the shadowed side.
Phobos, the larger and closer of Mars' two moons, has no atmosphere, which contributes to its dramatic temperature fluctuations between day and night
Wikipedia
Wikipedia
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. The sunlit side can reach temperatures comparable to a mild winter day on Earth, around −4°C (25°F), while the shadowed side plunges to −112°C (−170°F), colder than the harshest Antarctic nights
NASA
NASA
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. These extremes are intensified by the moon's fine regolith, which cannot retain heat, and its lack of atmospheric insulation
NASA
NASA
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Because Phobos is tidally locked to Mars, the same side always faces the planet, but temperatures still vary significantly depending on whether a region is exposed to sunlight or in shadow
Answers
Answers
. The average surface temperature is estimated to be around 233K (−40°C)
Answers
Answers
. These conditions make the surface environment extremely challenging for potential landers or human exploration, as equipment must withstand both intense cold and rapid thermal changes.
Phobos’ small size and low gravity also mean it cannot retain heat, and its surface is heavily cratered, with features like the Stickney crater influencing local temperature variations
Wikipedia
Wikipedia
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. Overall, the moon’s temperature extremes are a direct result of its lack of atmosphere, small size, and proximity to the Sun, making it one of the coldest and most thermally variable bodies in the inner Solar System
Wikipedia
Wikipedia
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Tar-Like Substances in Carbonaceous Asteroids
Carbonaceous asteroids — especially C-type asteroids and their meteorite counterparts like CI and CM chondrites — are known for their high carbon content, which includes organic compounds and water-bearing minerals. These materials can appear in forms that resemble tar or sticky organic residues when examined in detail.

Organic carbon and hydrocarbons
Carbonaceous asteroids contain complex organic molecules, including hydrocarbons and aromatic compounds, which can form viscous, tar-like substances under certain conditions. These organics are thought to have formed in the early solar system and may have contributed to the carbon inventory of Earth Science Times. In meteorite samples, such organics are often found in fine-grained, carbon-rich matrices that can look dark and sticky under the microscope.

Water-bearing minerals
Many carbonaceous asteroids host hydrated silicates (e.g., phyllosilicates) and other minerals that contain bound water. When these minerals are altered by heat or water, they can release water and organic compounds, sometimes leaving behind carbonaceous residues that resemble tar Wikipedia. This is especially common in asteroids that experienced aqueous alteration on their parent bodies.

Spectral and compositional evidence
Spectroscopic studies of C-type asteroids show absorption features consistent with both carbonaceous material and water-bearing minerals. The presence of these features supports the idea that their surfaces and interiors contain volatile-rich, organically complex materials Wikipedia. In meteorites, detailed chemical analysis confirms high abundances of carbon, hydrogen, oxygen, nitrogen, and sulfur — elements that are key to forming organic compounds.

Why it matters
These tar-like substances are not just scientific curiosities — they are potential sources of prebiotic chemistry and may have delivered water and organic molecules to early Earth. They also represent a class of materials that could be targeted in future asteroid resource missions, though their low density and fragility make mining challenging ScienceDaily.

In summary:
Yes — carbonaceous asteroids contain tar-like organic substances in the form of hydrocarbons, aromatic compounds, and altered carbonaceous minerals. These are part of their volatile-rich, organically complex makeup and are central to their scientific and potential resource value.

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Tar-Like Substances in Bennu and Ryugu Asteroids
Recent high-resolution infrared (IR) and spectroscopic analyses of samples from the carbonaceous asteroids Bennu (OSIRIS-REx) and Ryugu (Hayabusa2) have revealed a range of complex organic and hydrated phases, including carbonate-rich regions and hydrated ammonium-magnesium-phosphorus (NH₄Mg₂P₂O₇·nH₂O) grains pmc.ncbi.nlm.nih.gov+1. These hydrated ammonium compounds are structurally and chemically similar to certain ammonium-based organics that can form in water-rich environments and, in some cases, resemble the molecular complexity found in terrestrial “tar-like” or keratinized organic matter.

What “Tar-Like” Means in This Context
In planetary science, “tar-like” substances often refer to complex, carbon-rich, hydrogen-rich organic compounds that are insoluble in water, often containing nitrogen, oxygen, and sometimes sulfur. They can form through aqueous alteration of simpler organics in the presence of water and ammonia, and are common in carbonaceous chondrites and other primitive solar system materials.

Evidence in Bennu and Ryugu
Hydrated ammonium-magnesium-phosphorus grains: Detected in both Bennu and Ryugu samples, these are rare in meteorites and suggest localized aqueous environments rich in ammonia and phosphorus pmc.ncbi.nlm.nih.gov+1. Such compounds can be precursors to more complex nitrogen-containing organics.

Carbonate inclusions: Found in both asteroids, these indicate past interactions with water and CO₂, which can drive organic synthesis pathways Astrobiology.

Phyllosilicate-rich matrix: Both asteroids are dominated by hydrated silicates, which can host and protect organic molecules from degradation pmc.ncbi.nlm.nih.gov.

Organic matter: Bennu samples contain interstellar organic matter and pre-solar stardust, some of which may have undergone aqueous alteration to form more complex, “tar-like” organics Science Mission Directorate.
Implications
The presence of these hydrated ammonium and carbonate phases, along with the organic-rich matrix, suggests that aqueous alteration processes on the parent bodies of Bennu and Ryugu could have produced complex nitrogen- and phosphorus-bearing organics—molecular analogs to terrestrial tar-like compounds. These materials may have been delivered to early Earth and contributed to the chemical inventory that eventually led to life.

In summary: While no exact “tar” has been directly imaged, the hydrated ammonium-magnesium-phosphorus grains and other complex organics in Bennu and Ryugu samples are strong indicators of the types of aqueous-altered, nitrogen-rich organic matter that could be considered “tar-like” in a planetary chemistry sense pmc.ncbi.nlm.nih.gov+2.

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Bitumen (UK: /ˈbɪtʃʊmɪn/ BIH-chuum-in, US: /bɪˈtjuːmɪn, baɪ-/ ⓘ bih-TEW-min, by-)[1] is an immensely viscous constituent of petroleum. Depending on its exact composition, it can be a sticky, black liquid or an apparently solid mass that behaves as a liquid over very large time scales. In American English, the material is commonly referred to as asphalt. Whether found in natural deposits or refined from petroleum, the substance is classed as a pitch.[2] Prior to the 20th century, the term asphaltum was in general use.[3] The word derives from the Ancient Greek word ἄσφαλτος (ásphaltos), which referred to natural bitumen or pitch. The largest natural deposit of bitumen in the world is the Pitch Lake of southwest Trinidad, which is estimated to contain 10 million tons.[4]

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Bitumen is a complex petroleum-derived mixture of hydrocarbons, primarily composed of asphaltenes, resins, aromatics, and saturates, with carbon and hydrogen as dominant elements.
Chemical Composition
Bitumen is primarily made up of hydrocarbons, with elemental composition typically around 80–85% carbon, 8–11% hydrogen, and smaller amounts of sulfur, nitrogen, and oxygen. Trace metals such as nickel and vanadium may also be present in natural bitumen
Wikipedia
Wikipedia
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. Its molecular structure is highly complex, containing thousands of different molecules, which makes complete separation and identification nearly impossible
Wikipedia
Wikipedia
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SARA Fractionation
Bitumen’s molecules are commonly classified into four chemical families, known as SARA fractions:

Saturates: Waxy, non-polar hydrocarbons that contribute to hardness and temperature sensitivity
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Aromatics: Ring-shaped hydrocarbons that provide fluidity and workability, balancing the stiffness of asphaltenes
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Resins: Semi-solid, adhesive molecules that enhance ductility, flexibility, and bonding with aggregates
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Asphaltenes: High-molecular-weight, solid-like molecules responsible for bitumen’s dark color, viscosity, and structural stability
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These fractions interact to form a colloidal system, with asphaltenes dispersed in a maltene (resins, aromatics, and saturates) continuous phase, which explains bitumen’s viscoelastic behavior
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Molecular Structure and Properties
Bitumen behaves as a viscoelastic material, meaning it exhibits both solid-like and liquid-like properties depending on temperature and time scale. Its adhesive and waterproofing properties arise from the balance between rigid asphaltenes and fluid maltenes
Vedantu
Vedantu
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. Functional groups containing nitrogen, sulfur, and oxygen influence viscosity, oxidation resistance, and adhesion to aggregates
Vedantu
Vedantu
. Over time, oxidation can make bitumen brittle, affecting its performance in pavements
Vedantu
Vedantu
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Natural vs. Refined Bitumen
Natural bitumen occurs in deposits such as oil sands or ancient lake beds and may contain minerals like limestone in addition to hydrocarbons
Vedantu
Vedantu
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Refined bitumen is obtained from crude oil distillation, removing lighter fractions like gasoline and diesel, and may undergo further refining to improve grade and performance
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Vedantu
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Applications and Chemical Relevance
The chemical composition of bitumen directly affects its performance in road construction, roofing, and industrial applications. The proportion of asphaltenes, resins, aromatics, and saturates determines viscosity, temperature susceptibility, and durability. Understanding its chemistry is essential for modifying bitumen with polymers or additives to enhance properties such as rutting resistance, water damage resistance, and longevity
goldbitumen.com
goldbitumen.com
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Durability of Polyethylene in a Vacuum
Polyethylene (PE) is generally highly durable in vacuum environments because its non-polar, saturated carbon–carbon backbone is chemically inert and does not react with most gases, including oxygen and nitrogen sciencewatch.blog. In a vacuum, the absence of oxygen and moisture significantly reduces the risk of oxidation, hydrolysis, and environmental stress cracking (ESC), which are the main degradation pathways for PE in air sciencewatch.blog.

Why PE Performs Well in Vacuum
Chemical inertness: PE resists most acids, bases, salts, and solvents, and in a vacuum, it is not exposed to reactive gases that could cause chain scission scienceinsights.org+1.

No moisture absorption: PE’s hydrophobic nature means it does not swell or degrade from water ingress, a concern in humid or atmospheric conditions sciencewatch.blog.

Thermal stability: HDPE, in particular, maintains its mechanical properties at elevated temperatures without rapid degradation in vacuum scienceinsights.org.

Impact and abrasion resistance: PE types like HDPE and UHMWPE can withstand significant mechanical stress without fracturing scienceinsights.org.

Potential Limitations
While PE is stable in vacuum, its long-term durability still depends on:

Material type: HDPE is more rigid and thermally stable than LDPE; UHMWPE offers superior wear resistance but is less crystalline, so oxygen can penetrate more easily if exposed to air scienceinsights.org.

Temperature: At very high temperatures, even in vacuum, PE can soften or degrade if thermal stress is applied.

Surface effects: In space-like vacuum, UV radiation from sunlight (if present) can cause photo-oxidation, but in a true vacuum without UV, this is not a concern sciencewatch.blog.

Practical Applications
PE is widely used in vacuum forming and vacuum-sealed products because it:

Maintains shape and integrity under vacuum pressure dtplx.com+1.

Resists chemical attack in sealed environments.

Is recyclable and environmentally stable over long service lives dtplx.com.

In summary: In a vacuum, polyethylene’s chemical inertness, moisture resistance, and mechanical strength make it extremely durable, with minimal degradation risk. Its performance is best when combined with proper material selection (e.g., HDPE for structural parts) and temperature control.

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Asphalt typically contains about 5% to 10% bitumen, which serves as the binding agent that holds the aggregate together and provides durability and flexibility to the pavement.
Composition of Asphalt
Aggregate: Asphalt is primarily composed of aggregates, which make up about 90% to 95% of the mixture. This includes materials like gravel, sand, and crushed stone.
Bitumen: The remaining 5% to 10% is bitumen, a viscous black substance derived from petroleum distillation. Bitumen acts as a binder, providing essential properties such as waterproofing and flexibility to the asphalt
petronaftco.com
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Importance of Bitumen Content
The percentage of bitumen in asphalt is crucial for several reasons:

Durability: Proper bitumen content enhances the longevity of the pavement, reducing the need for repairs and maintenance.
Flexibility: Bitumen allows the asphalt to remain pliable under varying temperatures, preventing cracking and deformation.
Performance: The right balance of bitumen ensures that the asphalt can withstand different traffic loads and environmental conditions
petronaftco.com
petronaftco.com
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Factors Influencing Bitumen Percentage
Several factors can influence the optimal bitumen content in asphalt mixtures, including:

Traffic Load: Heavier traffic areas may require a higher bitumen content for increased durability.
Climate Conditions: In warmer climates, more bitumen may be used to prevent softening, while colder regions may require higher content to avoid cracking.
Project Specifications: Different types of roads (e.g., highways vs. residential streets) may have varying requirements for bitumen content to achieve desired performance characteristics
petronaftco.com
petronaftco.com
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In summary, the typical bitumen content in asphalt ranges from 5% to 10%, and optimizing this percentage is essential for creating durable and effective road surfaces.

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Oil Spill Feature on Mars and the Hebes Mensa Salt Dome
On Mars, the “Oil Spill” is a dark, flowing feature located at the eastern collapsed side of the Hebes Mensa salt dome in Hebes Chasma oilonmars.blogspot.com. The Hebes Mensa is a large, dome-shaped structure formed by diapirism — the upward movement of salt through overlying rock layers due to its lower density Wikipedia+1. This process can create domes that trap and sometimes release fluids, including hydrocarbons.

The “Oil Spill” Feature
The official interpretation from Adams et al. (2009) suggests the dark fluid is liquid brines tinted black by dust particles martinhovland.weebly.com. However, some researchers, such as Martin Hovland, argue that the physical characteristics — including the way the fluid flows and pools — are more consistent with crude oil seeping from the collapsed salt dome oilonmars.blogspot.com. On Earth, similar seeps occur in natural oil fields, such as the McKittrick oil field in California, where crude oil and bitumen emerge from the ground oilonmars.blogspot.com.

Why Salt Domes Are Relevant
Salt domes are important in petroleum geology because they can act as traps for oil and gas. As salt rises through sediment layers, it can create cavities and faults that collect hydrocarbons diversedaily.com+1. On Mars, the Hebes Mensa salt dome may have similarly trapped and released fluids, possibly including hydrocarbons, through collapse and venting.

Earth Analogues
Natural oil seeps on Earth, especially near salt domes, often show:

Braided or braided-branch flow patterns in brines or oil oilonmars.blogspot.com.

Pools that may solidify or corrode over time.

Vents where fluid emerges and spreads.

These features are used to interpret Martian seep-like formations, even though the Martian environment is vastly different.

In summary: The “Oil Spill” on Mars is linked to the Hebes Mensa salt dome, a geological structure that may have released hydrocarbons. While some scientists see it as brine-dust, others believe it is crude oil, drawing parallels to natural seeps on Earth where salt domes are known to host oil and gas martinhovland.weebly.com+3.