So now that we’ve been here for two solid years - that’s four whole years back on Earth! - after we’ve driven across the floor and over the delta and into the valley and all the way up the rim - NOW you decide you want a pet rock? After His Lordship has decided that he’s going to tariff anything Martian?

sighs He’s always like this with the shiny ones. He thinks it might be desert varnish. You think it’s desert varnish, don’t you? Do you know what’ll happen if we actually do find any of that stuff? The handling procedures. The import licenses. The biohazard protocols! Endless arguments over G-band spectroscopy from the damn scientists, they’ll be at it for years. How are you going to feel if your small rock happens to be the first with active biological entities? Come on, that’s the last thing we want.

I can’t take you anywhere, Paul.

My mama always said old crater rims was like a box of chocolates. You never know what you’re gonna get.

Regular readers will remember the “white rocks” that Percy was spotting in little clusters a few months ago, which Mars Guy, among others, was speculating might be quartz. The paper confirms that the first rock examined in detail in the video does contain that mineral, and is not simply another whitish mineral you might expect to find in this environment, like gypsum.

Part of the significance of this mineral being identified is the fact that it seems to comprise most of the rock being analyzed. Quartz-like material (“silica”) has been discovered by Spirit, Curiosity and even Zhurong, thousands of km away from Jezero Crater, and Percy itself has already identified some in Sample 24, which we grabbed down in Neretva Vallis. Finding this much silicon dioxide, in multiple forms, in a rock that appears silica-dominated, however, is something new. That’s water activity on another level - this is basically very refined silica that nature has cooked up. As the paper mentions, it would be very, very sweet to find an exposure of the source bedrock for these loose pebbles and cobbles, because that stuff we could drill for return to Earth.

Shortest answer: quartz has to be separated from other rocks/minerals. Water action is one of the easiest ways to manage that. In addition, opal/chalcedony is actually quartz with water directly attached on a molecular level, so that’s a direct discovery.

Medium answer: Igneous (“volcanic”) rock already contains the silicon and oxygen that quartz is made of, but they’re usually bonded with other elements, not just each other. In other words, they don’t exist as “free quartz” - meaning independent grains that are made of pure SiO2. As @athairmor alluded to, free quartz can form directly from magma when it solidifies and forms igneous rock. However, that is what you would expect from particular kinds of volcanic rock, which are absent or rare on Mars (e.g. granite). The igneous rock around Jezero Crater is not the type to contain “free quartz”. If the regional geology hasn’t served up any free quartz grains directly, you can still separate out the silicon and oxygen by breaking down the larger, more complicated minerals they’re attached to, but that would take a significant amount of chemical breakdown - i.e. significant amounts of water. This process is quite common on Earth, of course, where it yields up “white sand” on beaches - which is simply rounded grains of quartz.

Longest reply: I should probably just read the EPSL paper, and I’d be happy to summarize it here if people are interested.

So that means all four sampling attempts made here on Witch Hazel Hill have been difficult in some way. Two of the attempts were outright failures, the last successful one only filled half the tube, and this latest one, #27, “overflowing” to the point of rendering the seal difficult.

I count four “difficult” sampling operations from the entire mission prior to reaching the Hill (Sample 1 an outright failure, Sample 15 difficult to seal as Mars Guy refers to in the video, and two outright failures on the delta fan around sol 810-813), maybe five if you count that problem with the pebbles getting stuck in the bit carousel after successfully snagging Sample 6.

It may have taken 37 sols, but they finally did seal Sample 15, so I’m not overly worried about this problem with Sample 27. What I find striking about all of this is the intersection of the geology with the engineering. The problem we encountered with the very first sample (the stuff simply crumbling and escaping the tube before we could seal it) was a warning shot to the rover operations team, but a fascinating sign to the geologists: this stuff has seen some serious alteration since it was originally laid down! And that weak, friable Sample 1 material saw much less transformation by water, mineralogically speaking, than Sample 27…

We knew that we were going to find igneous (“volcanic”) geology combined with sedimentary geology (old river mud and sandstone) on this mission, but the intersection of the two giving us these kinds of problems is going to become part of the legend of Mars exploration. It may not be as controversial or unexpected as the Disappearing Methane Hunt or the Viking-era “biosignature” tease, but this sampling difficulty shows us just how tricky Mars is going to be.

Given this Mars Guy episode and the unusual interest that the science team is showing in the tailings (drill debris) for this latest core sample, I’ve created a quick-and-dirty guide to the tailings produced at the various secured-sample sites to date.

I don’t have too much to add in terms of analysis here at the moment, but I will say that the tailings from the crater rim (#26 and #27) are notably brighter than almost every other tailings pile taken earlier (down in the crater). Tailings from the same environment (e.g. the crater floor, the top of the delta) tend to look similar, despite their notable geological differences. The science of colour in solid materials is actually pretty complex, as any spectroscopist can tell you, so there aren’t always simple explanations for why some materials look different before and after drilling, aside from the fact that the tailings are made of very fine particles.

I’m still working on a (much more detailed) guide for the abrasion patches, which unlike the tailings have received extensive analysis, but I’m happy to take any constructive feedback for this short guide.

The coring seems to have been successful on this occasion.

For reference, the abrasion patch on the right is the latest one (#35), the fourth taken here at Witch Hazel Hill. I do hope that forthcoming mission updates will share more, at least qualitatively, about the drill data for all the recent coring attempts. It would be pretty illuminating to know which rocks have required the most time and force, given the sampling failures and unpredictable nature of the geology here.

I raise my tube
Only for a moment
And the sample’s gone
All my dreams
Flee before my eyes
Like Ingenuity

Dust in the wind
All they are is
Dust in the wind

Same old song
One more grain of basalt
in an endless flow
All we drill
crumbles to the ground
Though we refuse to see

Dust in the wind
All we are is
Dust in the wind

Thanks for adding in the arrows, it does help! Mapping is so key on missions like this…

😃 Yes, these comparisons are pretty illuminating. I feel like the rover wheels really tell the tale here. If you squint hard enough, Curiosity is almost like Spirit - it faces rougher terrain than its “twin”, and has faced more adversity. Mt. Sharp/Aeolis is pretty unique geologically, and the place is just so mountainous, that the ripped-up wheels seem justified, somehow. Percy is kind of like “Oppy”, the golden child that was sent to a more benign environment, and literally bounced onto on the very thing we had dreamed of finding. Sample acquisition problems aside, Jezero Crater has been pretty good to us, as you can see from those very healthy wheels that Percy’s still sporting. I’d say Curiosity has fully earned those extra 30 metres 😁

Ah hahahahahahahahaah

• We have 3rd-gen satellites that can correctly identify minerals from orbit, hundreds of kilometres away
• We launch a huge, complex lander with an outstanding geology toolset, far better than the Apollo generation could have dreamed of
• We send this technological marvel to a dry, eroded, pockmarked river delta billions of years old
• The sampling system flawlessly acquires samples of “weak”, sometimes heavily-altered rocks that started off as loose sand, some even containing clay
• We can plan the vehicle’s traverse so accurately that rover drivers can take weekends off without killing productivity

… and even now, years after landing, this planet still throws us!

I’m not even mad. I’m fascinated. The most difficult samples to acquire, our biggest “failures”, have been found at the literal lowest and highest elevations the rover has reached. Seriously, this apparent failure on 1409 has happened at a site almost 800 metres above the crater floor Percy first sampled in 2021. And both of these “problem” sampling sites clearly read as volcanic rocks… stuff that you’d think would be much easier to collect than old river sediment.

Oh yes, this is Mars.

For reference, we are within sight of the patch abraded on sol 1360 (abrasion patch #32), the first Percy made on this side the rim.

Being near the rim crest, #32 is the highest-elevation hole we’ve made, and will probably remain so, at least for a long while. As the highest bedrock layer on Witch Hazel Hill, it has something to say about the formation of Jezero, long before Neretva Vallis ever formed. 32 looks markedly different from the other three we’ve made on the hill, with all the well-defined brown grains on the right side and “fuzzy” whitish material in the middle. It looks quite different even from the two that are only slightly lower in elevation (famously crumbly #33 and the uniform-looking #35), only ~150 m away. It’s not entirely surprising to see the variety on display among the different patches we’ve sampled, but it is super neat to see the geologic diversity that this one hillside has to offer, considering that we haven’t even seen half of it yet!

I don’t take sass from people who have the names of prominent Nazis in their username. Care to explain why you took such a step?

I haven’t read the entire paper yet, but these bits in the intro caught my eye:

the Ingenuity helicopter carries no scientific instrumentation, has a mass of less than 2 kg, and can only fly a few hundred meters at a stretch. Better-equipped aircraft may be possible on Mars, but even with a specialized entry-descent-and-landing approach to maximize the feasible payload, Mars rotorcraft will likely be limited to only a few kilograms, in part due to limitations of motor cooling in the thin Mars atmosphere.

These limitations for Mars aerial exploration mean that any way to reduce payload without reducing scientific output would be advantageous, and one obvious avenue is using the drone itself as an environmental probe. Motivated by these considerations, B. Jackson recently explored using a drone to measure the near-surface wind profile, i.e., wind speed as a function of altitude. As a proof of concept, this effort followed on considerable previous work that showed that the tilt of a stably hovering drone can scale with wind speed—since a rotorcraft generates forward thrust, in part, by tilting into the thrust direction, the rotorcraft would have to tilt more into a stronger headwind. Drone attitude, including yaw, pitch, and roll, must be recorded for successful navigation on Mars anyway, so these data could be a way of retrieving the near-surface wind vector without requiring additional instrumentation.

EDITED TO ADD: the paper surprisingly doesn’t mention dust devils, which would be a very exciting and important avenue of research for a drone. Long live Ingenuity!

Well, the atmosphere types aren’t going to be unhappy with this sample, anyway. I understand they had already collected the minimum mass that was specified pre-launch, but I was sure the mission would collect more, and I can’t blame the atmosphere people for asking. So I suppose having more “headspace” in this sample tube is OK.

Assuming, though, that Steve Ruff (Mars Guy) is correct about this material being created or modified by the original Jezero impact event - I wonder if this much rock sample will be enough. The very thing that makes impact breccia/melt/glass so exotic and sexy is the same thing that makes it difficult to contextualize, i.e. the stuff is a mess! It could be a big grab bag of materials from different sources, and this site is already on the edge of Nili Planum, purportedly one of the oldest surfaces on Mars.

On the other hand… if this stuff allows us to get a firm date on the Jezero impact itself… yeah, it would definitely be worth it.

This is one of the best dust devil videos ever captured, IMO. Spirit used to catch whole packs of them roaming the great prairie-like floor of Gusev Crater (back when that rover was perched up in the Columbia Hills, I believe), but this devil in the foreground here shows a lot of detail, and is quite close to the camera, unlike those in old shots from Spirit. From what I recall, Percy has been able to capture some nearby dust devils in similar detail, which is unsurprising given that the Jezero region is supposed to be the windiest site we’ve visited on Mars… but awesome nonetheless.

Just looking at the shadows it casts is very revealing, and watching the thick white patches of the vortex really gives you an idea of the turbulence involved here. It’s really cool that we can see the entire length of the shadows being cast; I wonder if this is one reason why these shots were taken near noon, rather than later in the afternoon, around the time of maximum daily heating.

For scale, the crater at the bottom left is 300 m across from left to right, so you can tell that the “foot” of the foreground devil is quite a bit bigger than Percy itself. So much to see here!

Hahaha I hear you, Paul. In the end, I’m just going to have to bite the bullet and learn how to work with images myself. I didn’t mean to put everything off onto you 😄

As for people not appreciating the images, or the general stream of information from the rover(s), I’m proceeding on the theory that it’s hard to appreciate what these missions do without the context being readily available. Even in sifting through aaaall the images I needed to assemble my overview of the abrasion patches, I could see that I needed to rapidly compare and contrast several different abrasion sites to get a quick visual feel for the differences between them. And if someone like me feels this way, I can only imagine how difficult it might be for the casual social media user to see how exciting “another red rock” might be. Geologists aren’t always the best at outreach, but I believe the attempt is worth it in my case.

I can’t help with the 3D images just yet, but I’ll see what I can do after I post my overview.

Thank you! I’ve seen some of these before when looking at 3D models of the abrasion patches, but those shape models are quite useful in general.

I was thinking specifically of the “anaglyph” images we used to get from the MER PanCams and NavCams (such as the “Legacy Pan” from Opportunity). Even individual 3D frames could be quite mind-blowing in demonstrating the true ruggedness of those landscapes. The environments in and around Jezero, let alone Mt. Sharp, can’t be any less rugged than those were.

In other news, it does seem that the skies are finally clearing up a bit, now that we’re well into spring. This shot, from the mid-afternoon on sol 1359, shows how heavily obscured the distant hills on the western horizon were relative to the 1397 shot taken at nearly the same hour, and included above in Paul’s mosaic.

As Paul Hammond mentions, the “melting” is due to material sliding downhill. During the abrasion, which works partly by percussion, you can actually see a pebble sliding downhill (between this frame and this frame, which were taken only one minute apart), to the bottom right of the abrasion bit itself (near the centre of the image).

It’s not always apparent from the images, but the rover is currently on a fairly steep slope; we’re still parked on the exterior/outboard side of the Jezero Crater rim. I wonder how difficult it would be to make the 3D images I used to see from earlier rover missions…