Shiny parabolic or mirror use

[FOQ1]

For SpaceNut ... the purpose of the bricks is to stop sand storms. Why would it matter if they crack or look funny?

It appears to me that the brick you showed us would work well as a dust prevention device.

(th)

The purpose is two-fold. Ideally, the bricks would be load bearing construction material. Save that, they are stackable radiation shields. Just piling up the dust is no use because it can blow away. Turning it into a (even crude) brick solves that. And of course, they lock up a nuisance until proper Terraforming can produce a hydrology that binds the dust passively.

[tahanson43206]

For SpaceNut ... the purpose of the bricks is to stop sand storms. Why would it matter if they crack or look funny?

It appears to me that the brick you showed us would work well as a dust prevention device.

(th)

[SpaceNut]

so far the compression brick crack when removing them as seen with the sulfur binder and they are not regular shaped

[FOQ1]

Marspedia references

Poor quality bricks can be made with simple compression, tho stronger bricks can be made with gentle heating. See Brick for more information.
https://marspedia.org/Brick

https://marspedia.org/Dust

https://marspedia.org/Sand

https://marspedia.org/Regolith

here is the copilot output for mars mission sites<snip>

@SpaceNut what a great resource.

So, what I get from your above posts and the attached links... We can't rely on cold sintering with local materials in all locations because perchlorates are not uniformly distributed. All locations (so far) are primarily Silica and Iron. This could be quite handy! If I understand the chemistry right, simple CEB can be used. This unfortunately requires about 48,000 PSI to get a properly fused brick. The press would most likely be a piston "ram" type that operates at high RPM. Quick but lots of down time for maintenance. Also a domain for machines only as it would be both dangerous and noisy.

Hot sintering and glassification could be used at higher energy cost for additional chemistries. But if the goal is twofold creation of a radiation shielding building brick and locking up problematic dust by the megaton, we are golden. The process could be made fully (or nearly) robotic and automated in short order with a convoy of 'street sweeper' type drones bringing in dust to a central location for press, heat, or hybrid processing.

[SpaceNut]

Marspedia references

Poor quality bricks can be made with simple compression, tho stronger bricks can be made with gentle heating. See Brick for more information.
https://marspedia.org/Brick

https://marspedia.org/Dust

https://marspedia.org/Sand

https://marspedia.org/Regolith

here is the copilot output for mars mission sites

• Mission / Site: Viking 1 & 2 – Chryse / Utopia soils
  • SiO2 (wt%): ~43–47
  • FeO (wt%): ~17–20
  • MgO (wt%): ~8–10
  • Al2O3 (wt%): ~8–10
  • CaO (wt%): ~5–7
  • SO3 (wt%): ~6–8
  • Cl (wt%): ~0.5–0.8
  • Perchlorate (wt%): ~0 (not resolved)
  • Carbonate (wt%): ≤1 (inferred, poorly constrained)
  • Organics (mg C/g): n/a (no direct quantification)
  • Notes: Basaltic soil; high S and Cl; Fe-oxides (crystalline + poorly crystalline); trace meteoritic Ni.
• Mission / Site: Mars Pathfinder – Ares Vallis soils/rocks
  • SiO2 (wt%): ~45–50
  • FeO (wt%): ~16–19
  • MgO (wt%): ~8–11
  • Al2O3 (wt%): ~8–11
  • CaO (wt%): ~5–7
  • SO3 (wt%): ~5–7
  • Cl (wt%): ~0.5–0.8
  • Perchlorate (wt%): ~0 (not resolved)
  • Carbonate (wt%): ≤1 (inferred)
  • Organics (mg C/g): n/a
  • Notes: Basaltic rocks; soils similar to Viking global dust; Fe-oxides, pyroxene, feldspar.
• Mission / Site: MER Spirit – Gusev plains
  • SiO2 (wt%): ~45–50
  • FeO (wt%): ~16–20
  • MgO (wt%): ~8–12
  • Al2O3 (wt%): ~8–11
  • CaO (wt%): ~5–7
  • SO3 (wt%): ~4–7
  • Cl (wt%): ~0.5–0.8
  • Perchlorate (wt%): ~0 (not resolved)
  • Carbonate (wt%): ≤1
  • Organics (mg C/g): n/a
  • Notes: Primitive basalts; olivine, pyroxene, magnetite; global dust–like soil chemistry.
• Mission / Site: MER Spirit – Columbia Hills altered rocks
  • SiO2 (wt%): ~40–50 (variable)
  • FeO (wt%): ~12–18
  • MgO (wt%): ~6–10
  • Al2O3 (wt%): ~8–12
  • CaO (wt%): ~5–8
  • SO3 (wt%): up to ~10–15
  • Cl (wt%): ~0.5–1
  • Perchlorate (wt%): ~0 (not resolved)
  • Carbonate (wt%): 1–3 (locally higher)
  • Organics (mg C/g): n/a
  • Notes: Weathered basalts; sulfate-cemented rocks; P, S, Cl, Br enrichments; evidence for aqueous alteration and some clays.
• Mission / Site: MER Opportunity – Meridiani Planum soils
  • SiO2 (wt%): ~45–50
  • FeO (wt%): ~16–20
  • MgO (wt%): ~8–11
  • Al2O3 (wt%): ~8–11
  • CaO (wt%): ~5–7
  • SO3 (wt%): ~5–8
  • Cl (wt%): ~0.5–0.8
  • Perchlorate (wt%): ~0 (not resolved)
  • Carbonate (wt%): ≤1
  • Organics (mg C/g): n/a
  • Notes: Soils dominated by hematitic spherules (“blueberries”) mixed with basaltic fines; Br enrichment; meteoritic Ni.
• Mission / Site: MER Opportunity – Sulfate sandstones
  • SiO2 (wt%): ~35–45
  • FeO (wt%): ~12–18
  • MgO (wt%): ~6–10
  • Al2O3 (wt%): ~6–10
  • CaO (wt%): ~5–8
  • SO3 (wt%): up to ~15–20
  • Cl (wt%): ~0.5–1
  • Perchlorate (wt%): ~0 (not resolved)
  • Carbonate (wt%): 1–3
  • Organics (mg C/g): n/a
  • Notes: Layered sulfate-rich sedimentary rocks; hematite; jarosite and other Fe-sulfates; strong aqueous alteration signature.
• Mission / Site: Phoenix – Polar soils
  • SiO2 (wt%): ~40–45
  • FeO (wt%): ~15–18
  • MgO (wt%): ~7–10
  • Al2O3 (wt%): ~8–11
  • CaO (wt%): ~5–7
  • SO3 (wt%): ~3–6
  • Cl (wt%): ~0.5–1
  • Perchlorate (wt%): ~0.5–0.6
  • Carbonate (wt%): ~3–5
  • Organics (mg C/g): ~500
  • Notes: Alkaline soil (pH ~7.7); Ca-carbonate; perchlorate ~0.6 wt%; oxidized organics; ice-rich subsurface.
• Mission / Site: Curiosity – Gale Crater basaltic sandstones (Rocknest / Yellowknife Bay)
  • SiO2 (wt%): ~45–50
  • FeO (wt%): ~16–20
  • MgO (wt%): ~8–12
  • Al2O3 (wt%): ~8–12
  • CaO (wt%): ~5–8
  • SO3 (wt%): ~3–6
  • Cl (wt%): ~0.5–1
  • Perchlorate (wt%): ~0.3–0.5
  • Carbonate (wt%): ~1–3
  • Organics (mg C/g): up to ~2000
  • Notes: Plagioclase, pyroxene, magnetite, hematite, anhydrite, minor sulfates; 30–40 wt% amorphous; perchlorate and nitrate; oxidized organic carbon.
• Mission / Site: Curiosity – Gale Crater mudstones (Sheepbed / Murray)
  • SiO2 (wt%): ~45–55
  • FeO (wt%): ~12–18
  • MgO (wt%): ~6–10
  • Al2O3 (wt%): ~10–15
  • CaO (wt%): ~4–7
  • SO3 (wt%): ~3–6
  • Cl (wt%): ~0.5–1
  • Perchlorate (wt%): ~0.3–0.5
  • Carbonate (wt%): ~1–3
  • Organics (mg C/g): up to ~2000
  • Notes: Fine-grained lacustrine mudstones; more Al-rich; clays, Fe-oxides, sulfates; organics detected by SAM.
• Mission / Site: Perseverance – Jezero Crater igneous rocks
  • SiO2 (wt%): ~45–50 (provisional)
  • FeO (wt%): ~15–20
  • MgO (wt%): ~8–12
  • Al2O3 (wt%): ~8–12
  • CaO (wt%): ~5–8
  • SO3 (wt%): ~3–6
  • Cl (wt%): ~0.5–1
  • Perchlorate (wt%): not yet well quantified
  • Carbonate (wt%): trace–few wt% (local carbonates)
  • Organics (mg C/g): n/a (no bulk mg/g yet)
  • Notes: Basaltic to ultramafic igneous rocks; olivine-rich units; corundum (Al2O3) with Cr/Ti/Fe impurities; carbonates in some units.
• Mission / Site: Perseverance – Jezero deltaic / sedimentary targets
  • SiO2 (wt%): ~45–55 (provisional)
  • FeO (wt%): ~12–18
  • MgO (wt%): ~6–10
  • Al2O3 (wt%): ~10–15
  • CaO (wt%): ~4–7
  • SO3 (wt%): ~3–6
  • Cl (wt%): ~0.5–1
  • Perchlorate (wt%): not yet well quantified
  • Carbonate (wt%): up to several wt% (carbonates, sulfates)

[SpaceNut]

Perseverance

Perseverance has identified a diverse mineral suite in Jezero Crater, pointing to a wet, formerly habitable environment. Key discoveries include olivine-rich igneous rock (Máaz and Séítah formations), carbonates, smectite clays, and hydrated silica. The rover recently discovered kaolinite, nickel-rich Fe-sulfides, and manganese hydroxide, indicating sustained watery conditions.
Key Mineralogical Findings:Carbonates & Clays: Detected early in the mission, these signify the presence of an ancient lake, acting as ideal materials to trap fossilized microscopic life.Igneous Minerals: The crater floor is composed of olivine and pyroxene-rich basaltic rock.Aqueous Alteration Minerals: Sulfate and perchlorate salts, along with Fe/Mg phyllosilicates, are found in the delta and crater floor deposits, indicating multiple water alteration episodes.Recent Discoveries:Kaolinite & Aluminum-rich rocks: Found as "white stones," suggesting long-term weathering in water.Nickel (Ni) Enrichment: Up to 1.1% nickel was found in Fe-sulfides in the Neretva Vallis area, associated with organic matter and similar to terrestrial microbial habitats.Manganese Hydroxide: Found in the "Kenmore" rock, indicating a highly oxidizing environment.Leopard Spots (Cheyava Falls): A rock containing olivine-rich, red-speckled material, including iron phosphate (vivianite) and iron sulfide (greigite), which are known to be potential biosignatures on Earth.

Rover Spirit

The Mars Exploration Rover Spirit, which landed in the Gusev Crater in 2004, discovered a variety of volcanic minerals and evidence of aqueous alteration, particularly in the Columbia Hills. The landing site was dominated by basaltic rocks rich in olivine, pyroxene, plagioclase, and magnetite. As Spirit explored, it found significant concentrations of iron, silicon, sulfur, chlorine, bromine, and phosphorus

Key Mineral and Elemental Findings:Plains Basaltic Rock: The initial landing site in the Gusev Crater was covered with olivine-rich basaltic rocks and volcanic dust containing magnetite (with titanium).Columbia Hills (Aqueous Mineralogy):Silica-Rich Soil: In areas like "Home Plate," Spirit discovered high concentrations (up to 90%) of pure silica (\(SiO_{2}\)), which likely formed in hot spring environments, indicating past volcanic activity in the presence of water.

Sulfates: The rover identified magnesium sulfates and other sulfate-rich soils, particularly in the "Paso Robles" class of soils, which indicates water-related processes.Carbonates: A major discovery in the "Comanche" outcrop was a high concentration of carbonate minerals, pointing to a formerly neutral pH, watery environment.Goethite: The iron-bearing mineral goethite was found, which is a known indicator of water-related oxidation.Mineral Weathering: The rocks in the Columbia Hills were significantly altered by water, featuring high levels of sulfur, chlorine, and bromine, suggesting a history of interaction with liquid water

Opportunity rover

The Opportunity rover landed in Meridiani Planum, finding extensive evidence of past liquid water through minerals like jarosite, hematite "blueberries," and various sulfate salts (kieserite, gypsum). The site, featuring sedimentary bedrock, revealed a highly acidic, wet environment in its early exploration, later discovering clay minerals indicating neutral water conditions

Key Mineral Elements and Findings:Jarosite & Sulfates: The Mössbauer spectrometer detected jarosite, a hydrated iron sulfate, confirming acidic water environments. Other sulfates include kieserite, sulfate anhydrate, bassanite, hexahydrite, and epsomite.Hematite: Abundant iron-rich spherules (blueberries) found on the surface were formed by iron oxidizing and accumulating in water, confirming a wet past.Clay Minerals (Phyllosilicates): Later in the mission, specifically at Matijevic Hill (Endeavour Crater), Opportunity found clay minerals (smectites), suggesting a more neutral, habitable, and older water environment.Other Minerals: The rover found magnesium, iron, and calcium salts, along with iron oxides. Silica (often indicating hot spring activity) was also identified in later exploration areas

[SpaceNut]

just a quick google AI the response is

Comparison to Actual Mars Fines/Dust
Composition: While simulants try to match the iron-rich composition, they rarely replicate the exact mineralogy, specifically missing the exact amorphous silicate structure and, until recently, lacking the toxic perchlorates found on Mars.Particle Size: Martian dust is an incredibly fine powder, with many particles below 100 micrometers. High-fidelity simulants like MGS-1 are specifically processed to match this grain size distribution.Environmental Factors: Real Mars dust is highly oxidized and often electrostatically charged, posing a risk of sticking to equipment and clogging seals. Simulants must be tested for similar electrostatic behavior, but rarely achieve the exact conditions.Physical Differences: Real Mars fines often form duricrusts (hard surface layers) due to interaction with water vapor, a property difficult to fully replicate in simulants

Martian Fine Dust: Elemental/Oxide Composition
Martian dust is essentially pulverized, weathered mafic (basaltic) rock and is relatively uniform across the planet.
The primary oxides (\(>90\%\)) in Martian fine dust are:
Silicon Dioxide (\(SiO_{2}\)): \(\approx 49.5\%\)
Iron (III) Oxide (\(Fe_{2}O_{3}\)): \(\approx 18\%\) (causes the red color)
Magnesium Oxide (\(MgO\)): \(\approx 7.7\%\)
Aluminum Oxide (\(Al_{2}O_{3}\)): \(\approx 7.2\%\)
Calcium Oxide (\(CaO\)): \(\approx 6.7\%\)

Landing site give different amounts and composition.
As seen some have no Basalt sands....

[FOQ1]

the issue is not that we can not glue mars together is that mars is not uniform at the sites we are visiting. They each have wide missing ingredients to make a unified regolith simulant once ground up that works as advertised.

Making a mental note to look deeper into the issue of what resources are homogeneously vs heterogeneously distributed.

I was working on an assumption that the 'dusty' parts of regolith are uniform. Since that has been blowing around for millions of years, it should be well mixed and all very round microscopically like the sand in Saudi Arabia. Anything too large to be wind blown should be expected to be heterogeneously distributed.

Need to know if that dust contains both perchlorates and iron. If so, they can be Cold Sintered (with the addition of water). I'm going out on a limb and stating that any locations chosen not near the poles will have a logistics system to get water to them. Else, at a location with trace subsurface water available.

[SpaceNut]

the issue is not that we can not glue mars together is that mars is not uniform at the sites we are visiting. They each have wide missing ingredients to make a unified regolith simulant once ground up that works as advertised.

[tahanson43206]

For FOQ1 re post:

Mylar could be a good choice. I think if I was tasked with designing such a thing, I'd want also a clear material that could used to form a mylar balloon. The balloon could be inflated to create a parabola with little effort of trussing with a focal point outside the clear material.

Just a thought .... GW Johnson showed us an image from the 1950's, of a research project along these lines ... the balloon spherical surface creates a column of energy density instead of a point. A column can accept heat as well as a point can, and the stress on the material is spread out.

Please continue your discussion with that small adjustment.

This forum has the ability to store images. That feature shows up when you are creating a post. You can see {Attachments} next to Options below the input window. If you click on Attachments, you'll have access to the image storage subsystem.

You can create your own images, and upload them. If an image is too large for 256 KiB, just convert from PNG to JPG and that will usually do the trick.

(th)