{"id":5073,"date":"2022-11-15T22:00:00","date_gmt":"2022-11-15T22:00:00","guid":{"rendered":"https:\/\/modernsciences.org\/staging\/4414\/?p=5073"},"modified":"2022-11-04T06:43:57","modified_gmt":"2022-11-04T06:43:57","slug":"the-perseverance-rover-is-collecting-rock-samples-from-mars-to-bring-back-to-earth","status":"publish","type":"post","link":"https:\/\/modernsciences.org\/staging\/4414\/the-perseverance-rover-is-collecting-rock-samples-from-mars-to-bring-back-to-earth\/","title":{"rendered":"The Perseverance rover is collecting rock samples from Mars to bring back to Earth"},"content":{"rendered":"\n
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\n Concept illustration for research robots that could bring samples of Mars rocks to Earth-based labs.\n (NASA\/JPL-Caltech)<\/a><\/span>\n <\/figcaption>\n <\/figure>\n\nMariek Schmidt<\/a>, Brock University<\/a><\/em> and Chris Herd<\/a>, University of Alberta<\/a><\/em><\/span>\n\n

Hidden in the minerals and textures that make up rocks are clues about how and when they formed and were later altered. These changes can occur due to the presence of water-rich fluids and may also be influenced by biological processes. <\/p>\n\n

We are planetary petrologists (rock scientists) and participating scientists on the Mars 2020 Perseverance rover mission<\/a>. Our research involves exploring and interpreting the data sent back by the Perseverance rover from its landing site in Jezero Crater<\/a>.<\/p>\n\n

A mysterious lake<\/h2>\n\n

Orbital images show that Jezero Crater was once the site of a standing body of water. It held a lake that was fed by water from an ~170 km-long river channel<\/a>, and images show a delta \u2014 a fan-shaped platform of sediment \u2014 at the mouth of the channel. This delta is made up of layers of finer sediments mixed with boulder-rich layers that suggest that the river flow fluctuated from relatively calm conditions to large floods<\/a>.<\/p>\n\n

More of a mystery, however, were rock units exposed in Jezero Crater\u2019s floor, where Perseverance landed on Feb. 18, 2021. Of particular interest was an enigmatic unit, identified by the presence of olivine its spectral signatures (measurements of the amount of radiation it reflects).<\/p>\n\n

\n \"a<\/a>\n
\n A panorama of Brac, captured by the Mastcam-Z camera system aboard NASA\u2019s Perseverance Mars rover between Nov. 6 and 17, 2021. The panorama is made up of a total of 64 images stitched together after being sent back to Earth.<\/span>\n (NASA\/JPL-Caltech\/ASU\/MSSS)<\/a><\/span>\n <\/figcaption>\n <\/figure>\n\n

Evidence of history<\/h2>\n\n

Olivine is a vitreous, green mineral (its gem variety is peridot) that usually crystallizes in high-temperature magmas. In contrast, carbonate minerals can form from high to low temperatures, usually from melts or fluids that may have been favourable for life<\/a>. <\/p>\n\n

The olivine-rich unit is widespread in the region beyond Jezero, covering approximately 70,000 square kilometres<\/a>, and exposed within the crater just to the north and west of Perseverance\u2019s landing site, in a region dubbed S\u00e9\u00edtah<\/a>. <\/p>\n\n

S\u00e9\u00edtah (meaning \u201camidst the sand\u201d in Navajo<\/a>) is covered by a network of sand dunes, making it difficult for the rover to navigate. However, it was considered a compelling target for understanding the history of this region of Mars and because its carbonate minerals could preserve evidence of ancient life. <\/p>\n\n

Perseverance entered S\u00e9\u00edtah in September 2021 and readily confirmed the occurrence of olivine by its remote-sensing instruments<\/a>. The microscopic cameras saw two- to three-millimeter olivine grains, but their origin was unknown.<\/p>\n\n

On Earth, olivine grains of this size and shape may be concentrated by various geologic ways, including as wind- or water-borne sands sourced from olivine-rich regions, explosive volcanic eruptions, material ejected by meteorite impact, or they can form as crystals in cooling magma.<\/p>\n\n

Additional information was needed to interpret the history of the olivine, but engineering challenges initially impeded the mission\u2019s ability to use its X-ray fluorescence (XRF) spectrometer on S\u00e9\u00edtah rocks.<\/p>\n\n

\n \"extreme<\/a>\n
\n A close-up of a rock named Dourbes, taken by the WATSON (Wide Angle Topographic Sensor for Operations and eNgineering) camera on the end of the robotic arm aboard NASA\u2019s Perseverance Mars rover.<\/span>\n (NASA\/JPL-Caltech\/MSSS)<\/a><\/span>\n <\/figcaption>\n <\/figure>\n\n

Sophisticated equipment<\/h2>\n\n

XRF spectrometers<\/a> have been important instruments for determining the elemental compositions (sodium to iron, and some trace elements) of rock surfaces on Mars. <\/p>\n\n

Alpha Particle X-ray Spectrometers (APXS) onboard Pathfinder<\/a>, the two Mars Exploration Rovers Spirit and Opportunity<\/a>, and the Mars Science Laboratory rover Curiosity<\/a> provided bulk chemistries of ~1.5 cm circular spots that helped geologic interpretations. <\/p>\n\n

But for some Martian rocks, uncertainties have lingered about small-scale features and fine rock textures that are critical for interpreting what minerals are present, whether they are igneous or sedimentary, or their alteration histories. <\/p>\n\n

The PIXL onboard Perseverance is a big improvement in this regard<\/a>: PIXL generates ~120 micron grid maps that not only provide rock and mineral chemistries, but textures that can be used to infer the origin, processes and relative timing of the various minerals and other components present.<\/p>\n\n

The first PIXL scan of a rock surface at a S\u00e9\u00edtah outcrop called Brac<\/a> finally nailed the unit\u2019s origin as igneous<\/a>. The olivine grains are well-formed crystals with straight edges. Other high-temperature minerals, including feldspar, and larger minerals enclose or occur in the spaces between the olivine crystals, indicating slow cooling of a magma. <\/p>\n\n

Brac is a type of rock called an olivine cumulate that formed when olivine crystallized near the top of a magma, and settled and accumulated downward due to its higher density. Olivine cumulates are well known to form on Mars because they are found among the Martian meteorites, comprising a group known as chassignites<\/a>, that was ejected from Mars by an impact event and eventually fell to Earth.<\/p>\n\n

On Earth, olivine cumulates occur in large layered intrusions, such as the Skaergaard Intrusion in East Greenland<\/a>, and in thick lava flows, such as found in the Abitibi, Ont. area<\/a>.<\/p>\n\n

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