Grabens, evidence for widespread recent tectonism on Mercury

Post contributed by Ben Man, The Open University @AstroBenjamin

Mercury is a contracting world as evidenced by the abundance of shortening structures observed across the surface of the planet (Image 1). Global contraction as a result of secular cooling of the planetary interior is most likely responsible for widespread compressional tectonism with shortening structures seen cutting all surface materials at all latitudes and longitudes. Shortening structures are accepted as the surface manifestation of thrust faults and folding. Grabens, such as those observed in the images (Image 1-3), are secondary structures found on top of parent shortening structures. The presence of these grabens provide evidence for recent widespread tectonism on Mercury, confirming that global contraction is ongoing.

Image 1: Aspect view of Alpha Crucis Rūpes with horst and grabens present in the foreground of the image. Alpha Crucis Rūpes is located in H09 Eminescu, an equatorial quadrangle. The image is comprised of the H09 south east high incidence west mosaic tile and five individual narrow-angle camera frames (EN0231136925M, EN0231136927M, EN0231136960M, EN0231136962M, EN0231136998M). The image has not been vertically exaggerated and the scale bar is computed for the centre of the image. Image source: NASA/JHUAPL/CIW made by Benjamin Man. Image frames and mosaic tiles are available from NASA’s Planetary Data System Geosciences Node (https://pds-geosciences.wustl.edu/) and the Cartography and Imaging Sciences Node (https://pds-imaging.jpl.nasa.gov/).

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Flow deposits on Mercury – Impact ejecta flows or landslides?

Post contributed by Alistair Blance, The Open University, UK

During an impact on Mercury’s surface, material is ejected from the forming impact crater. As Mercury has only a tenuous atmosphere, ejected material travels predominantly ballistically, creating an ejecta deposit around the crater that thins gradually with increasing distance. However, large deposits emplaced by ground-hugging flows can be found around some impact craters on Mercury (Image 1). Evidence for flow includes material being diverted around obstacles, a steep edge or distal ridge at deposit margins, and a lobate shape to several examples. Some flow deposits extend outwards around a whole crater, but often they are confined within topographic lows adjacent to the crater. To help assess the origin of these features, it is useful to compare them to similar features across the Solar System. This comparison may also indicate how differences between the planets can influence the development of flows around craters.

Image 1: Flow deposits around craters on Mercury. Deposit boundaries indicated with red triangles. (A) Flow deposit extending from the central crater into an underlying crater in the top right of the image. Steep margins with a lobate shape suggest emplacement by flow. Image taken from MESSENGER MDIS BDR Global Basemap. (B) A crater with two sections of flow deposit extending into the underlying crater in the bottom right of the image. Image taken from MESSENGER MDIS frame EW0260906588G. (C) Sketch map of the image in B. Shows the two sections of flow deposit in red, with hypothesised direction of emplacement shown with red arrows. The deposit appears to have been diverted around a central peak within the underlying crater, providing evidence for emplacement via ground-hugging flow.

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BepiColombo: the challenge is at dawn

Post contributed by Dr Valentina Galluzzi – National Institute of Astrophysics, Institute for Space Astrophysics and Planetology (INAF-IAPS), Italy.

The ESA/JAXA BepiColombo spacecraft is on a long journey into orbit around Mercury. This journey includes six flybys of the planet before orbital insertion in 2025. On 23 June 2022, BepiColombo accomplished its second flyby of Mercury by approaching the planet as close as 200 km from the surface. Unfortunately, this happened when night shadows were still hiding the surface from sight. It was just 5 minutes after closest approach that the Monitoring Cameras (M-CAMs, three in total) mounted on the BepiColombo’s Mercury Transfer Module (MTM) could start taking the first snapshots of the planet with enough light. This caused the pictures to show dramatic sunrise shadows along the terminator. One of the first regions to be imaged was the Eminescu area of Mercury, as seen in Image 1.

Image 1: Composite image of the Eminescu region of Mercury made with BepiColombo/MTM M-CAM#2 “Image 02” taken during BepiColombo’s second Mercury flyby (credits: ESA) overlain by MESSENGER/MDIS enhanced colors (Denevi et al., 2018). Some spacecraft parts are visible near the frame margins. North is to the left. For scale reference, Izquierdo crater diameter is about 150 km (see Image 2).

In this picture, the shadow-enhanced morphology comes from the original M-CAM#2 frame taken at 09:24 UTC. By georeferencing the original M-CAM photo onto the Mercury’s spatial frame (Galluzzi et al., 2022) it was possible to overlay terrain color using the MESSENGER/MDIS enhanced color mosaic (Denevi et al., 2018). The composite image helps to highlight the terrain diversity in this area, from the yellowish young smooth plains to the dark blue and rougher intercrater plains.

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Ice Deposits Revealed by Radar Within Craters on Mercury

Post contributed by Dr. Edgard G. Rivera-Valentín, Lunar and Planetary Institute, Universities Space Research Association.

Although its surface can reach 800°F (427°C), some of Mercury’s craters conceal vast ice deposits that, in a sense, “sparkle” in the light of radar (Image 1). The so-called radar bright features were first identified in 1992 using ground-based observatories, in particular the Arecibo Observatory in Puerto Rico, which provided magnificent views down to craters tens-of-kilometers in diameter all the way from Earth. The ice lies within craters whose morphology and location results in areas that do not receive direct sunlight (i.e., permanently shadowed regions). This allows for the low temperatures needed to retain ice over millions of years.

Image 1: Radar image of Mercury’s north polar terrain (> 75°N) in polar stereographic projection. The five notable craters, Chesterton (88.5°N, 126.9°W), Tolkien (88.8°N, 211.1°W), Tryggvadóttir (89.6°N, 171.6°W), Kandinsky (87.9°N, 281.2°W), and Prokofiev (85.7°N, 297.1°W) are labeled. Radar backscatter is noted in grayscale from black (below noise levels) to white (high backscatter). All bright areas are radar bright features, which are located within craters that have permanently shadowed regions. These are the locations of ice deposits on Mercury. For scaling reference, Chesterton crater has a diameter of 37.2 km. Image credit: Figure 2 in Rivera-Valentín et al. (2022) PSJ 3,62.

The discovery of the radar bright features at Mercury’s poles was one of the motivators of NASA’s MESSENGER (Mercury Surface, Space Environment, Geochemistry, and Ranging) mission, which studied Mercury between 2011 – 2015. That is because although the radar scattering properties of the features were reminiscent of observations of the Martian polar layered ice deposits, as well as of the icy moons of Jupiter, they alone did not uniquely indicate the presence of water ice. The detailed studies by MESSENGER along with the earlier radar observations together now strongly suggest deposits of water ice. This is due to their location, evidence from high resolution and long exposure imaging, and measurements of epithermal and fast neutron fluxes.

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Volatile-rich impact ejecta on Mercury

Post contributed by Dr Jack Wright, School of Physical Sciences, The Open University, UK.

The Caloris basin is the largest (~1,500 km across), well-preserved impact structure on Mercury (Image 1a; Fassett et al., 2009). Hummocky plains around Caloris host numerous, steep-looking, conical knobs (Image 1b). The obvious explanation for the hummocky plains is that they formed from material ejected by the Caloris impact ~3.8 billion years ago. It follows that the knobs probably formed from discrete ejecta blocks. What isn’t obvious is why many of these blocks, which hypothetically could have formed with a variety of shapes, exist as steep cones in the present day. If these knobs really did form as Caloris ejecta, then they offer a rare opportunity to study materials ejected from Mercury’s interior with remote sensing techniques.

Image 1: Mercury and the circum-Caloris knobs. (a) Enhanced colour limb view of Mercury from the MESSENGER spacecraft. The Caloris basin’s interior is made of volcanic plains that appear orange in this data product. The arrow indicates the location of (b). (b) Examples of circum-Caloris knobs just outside the Caloris rim. Mosaic of MESSENGER MDIS WAC frames EW0220807059G, EW0220807071G, and EW0220763870G. ~86 m/pixel.

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Impact Crater Degradation on Mercury

Post by Mallory Kinczyk, PhD candidate, Department of Marine, Earth, and Atmospheric Sciences, North Carolina State University

The formation of impact craters may be the most ubiquitous exogenic surface process in the Solar System. These craters take on many shapes and sizes and can hint at underlying rock types, tell us about the nature of the impactor, and can shed light on the body’s geological history. Even on bodies without atmospheres, erosive forces are at play, changing the crater shape through time via processes such as seismic shaking and disruption from debris thrown outward by subsequent, nearby impacts. Because Mercury is the only terrestrial planet without an atmosphere, it maintains a unique snapshot of the inner Solar System’s impactor population (Image 1) and, in turn, can shed light onto Earth’s own geological history.

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Image 1: View of Mercury from the MESSENGER spacecraft, which orbited Mercury between 2011 and 2015 (Image PIA17280). A variety of impact crater sizes and shapes are evident from very fresh craters to subdued to almost completely obliterated crater forms. Bach crater (arrow) hosts a well-defined central peak ring, but its subdued form indicates that it has been disrupted by subsequent craters. Image Credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington.

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It is Mercury’s fault(s)…

Post contributed by Valentina Galluzzi, INAF, Istituto di Astrofisica e Planetologia Spaziali (IAPS), Rome, Italy

Any celestial body that possesses a rigid crust, be it made of rock (e.g. terrestrial planets, asteroids) or ice (e.g. icy satellites), is subject to both endogenic and exogenic forces that cause the deformation of crustal materials. As a result of the mass movement, the brittle layers often break and slide along “planes” commonly known as faults. In particular, tensional, compressional and shear forces form normal, reverse and strike-slip faults, respectively. On Earth, plate tectonics is the main source of these stresses, being a balanced process that causes the lithospheric plates to diverge, converge and slide with respect to each other. On Mercury, there are no plates and therefore the tectonics work differently. Instead its surface is dominated by widespread lobate scarps, which are the surface expression of contractional thrust faults (i.e. reverse faults whose dip angle is less than 45°) and this small planet is in a state of global contraction.

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Image 1. Endeavour Rupes area on Mercury, image is centred at 37.5°N, 31.7°W. Top: MESSENGER MDIS High-Incidence angle basemap illuminated from the West (HIW) at 166 m/pixel. Bottom: MESSENGER global DEM v2 with a 665m grid [USGS Astrogeology Science Center] on HIW basemap, the purple to brown colour ramp represents low to high elevations, respectively. Endeavour Rupes scarp is high ~500 m. For scale, Holbein crater diameter is approximately 110 km.

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Recent vents and channels on the Cerberus plains of Mars: lava or water?

Posted by Rebecca Thomas, Department of Physical Sciences, The Open University, UK.

Recent channelized flows from vents in the Cerberus plains of Mars demonstrate the difficulties of uniquely ascribing process to landforms on other planets.  The image below shows two fissures emanating from a wrinkle ridge. Both fissures appear to be sources of approximately contemporaneous channels running down onto the surrounding plains (Thomas, 2013). The channel in the west is constructive and differs from that in the east which is clearly shows several phases of incision (Image 1).

Image 1: a. Vents and channels in the Cerberus plains, Mars (156.9° E, 7.1° N); b. incised channel; c. constructed, leveed channel. (HiRISE ESP_016361_1870)

Image 1: a. Vents and channels in the Cerberus plains, Mars (156.9° E, 7.1° N); b. incised channel; c. constructed, leveed channel. (HiRISE ESP_016361_1870)

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Young volcanism on Mercury

Post by Carolyn Ernst, Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA.

Prior to 2008, less than half of Mercury’s surface had been imaged at close range, during the flybys of Mariner 10 in the mid-1970s. The MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft completed three flybys of the planet in 2008 and 2009 on its way to insertion into orbit about Mercury on 18 March 2010 and viewed most of the planet’s surface that had never before been seen by a spacecraft. These MESSENGER images have helped to confirm some Mariner-10-based hypotheses and have elicited new science questions to be investigated.

September

Image 1: Narrow-angle camera mosaic of Rachmaninoff basin, 290 km in diameter, as seen during MESSENGER’s third Mercury flyby on 29 September 2009. Orthographic projection, ~ 440 m/pixel, centered at ~28ºN, 58ºE. MESSENGER images 0162744128 and 0162744150, credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie Institution of Washington.

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Mercury’s Mighty Valles

Post by Dr. Paul K. Byrne, Carnegie Institution of Washington, USA

 Channel-like landforms termed “valles” (sing. “vallis”) have been observed on the Moon, Mars, and Venus, and recent results from the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) mission show that the innermost planet hosts its own brand of valles, too. Resembling the broad outflow channels on Mars and Venus, five shallow, linear depressions form a channelized network at high latitudes in Mercury’s northern hemisphere. These valles are situated adjacent to expansive northern volcanic plains that cover some 6% of the planet’s surface, and likely conducted voluminous, low-viscosity lavas from these plains southward.

Image 1: This vallis has the steep sides, smooth floors, and erosional residuals characteristic of Mercury’s broad valles, and likely channeled lavas from left to right across the image. The image has a field of view of ca. 150 km. The 57°N parallel and 115°E meridian are shown, and Kofi basin is labeled. The image is a portion of MESSENGER’s Mercury Dual Imaging System (MDIS) global monochrome basemap, which has a resolution of 250 meters per pixel.

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