Geology of Mercury

Source: Wikipedia, the free encyclopedia.

Peak ring impact basin
on Mercury.
Several areas on Mercury are extremely dark, such as a small crater within Hemingway crater in the lower right.

The geology of Mercury is the scientific study of the surface, crust, and interior of the planet Mercury. It emphasizes the composition, structure, history, and physical processes that shape the planet. It is analogous to the field of terrestrial geology. In planetary science, the term geology is used in its broadest sense to mean the study of the solid parts of planets and moons. The term incorporates aspects of geophysics, geochemistry, mineralogy, geodesy, and cartography.[1]

Historically, Mercury has been the least understood of all the

BepiColumbo
spacecraft, scheduled to go into orbit around Mercury in 2025, is expected to help answer many of the remaining questions about Mercury’s geology.

Mercury's surface is dominated by

lunar maria,[4][5] and locally by pyroclastic deposits.[6] Other notable features include vents which appear to be the source of magma-carved valleys, often-grouped irregular-shaped depressions termed "hollows" that are believed to be the result of collapsed magma chambers,[7] scarps indicative of thrust faulting, and mineral deposits (possibly ice) inside craters at the poles. Long thought to be geologically inactive, new evidence suggests there may still be some level of activity.[8][9]

Mercury's density implies a solid iron-rich core that accounts for about 60% of its volume (75% of its radius).[10] Mercury's magnetic equator is shifted nearly 20% of the planet's radius towards the north, the largest ratio of all planets.[11] This shift suggests there being one or more iron-rich molten layers surrounding the core producing a dynamo effect similar to that of Earth. Additionally, the offset magnetic dipole may result in uneven surface weathering by the solar wind, knocking more surface particles up into the southern exosphere and transporting them for deposit in the north. Scientists are gathering telemetry to determine if such is the case.[11]

After having completed the first solar day of its mission in September 2011, more than 99% of Mercury's surface had been mapped by NASA's MESSENGER probe in both color and monochrome with such detail that scientists' understanding of Mercury's geology has significantly surpassed the level achieved following the Mariner 10 flybys of the 1970s.[7]

Difficulties in exploration

Mariner 10 probe

Reaching Mercury from Earth poses significant technical challenges, because the planet orbits so much closer to the Sun than does the Earth. A Mercury-bound spacecraft launched from Earth must travel 91 million kilometers into the Sun's gravitational potential well.[12] Starting from the Earth's orbital speed of 30 km/s, the change in velocity (delta-v) the spacecraft must make to enter into a Hohmann transfer orbit that passes near Mercury is large compared to other planetary missions. The potential energy liberated by moving down the Sun's potential well becomes kinetic energy; requiring another large delta-v to do anything other than rapidly pass by Mercury. In order to land safely or enter a stable orbit the spacecraft must rely entirely on rocket motors because Mercury has negligible atmosphere. A direct trip to Mercury actually requires more rocket fuel than that required to escape the Solar System completely. As a result, only two space probes, Mariner 10 and MESSENGER, both by NASA, have visited Mercury so far.

Internal structure of Mercury

Furthermore, the space environment near Mercury is demanding, posing the double dangers to spacecraft of intense

solar radiation
and high temperatures.

Historically, a second obstacle has been that Mercury's

period of rotation is a slow 58 Earth days,[13] so that spacecraft flybys are restricted to viewing only a single illuminated hemisphere. In fact, unfortunately, even though Mariner 10
space probe flew past Mercury three times during 1974 and 1975, it observed the same area during each pass. This was because Mariner 10's orbital period was almost exactly 3 sidereal Mercury days, and the same face of the planet was lit at each of the close approaches. As a result, less than 45% of the planet's surface was mapped.

Earth-based observations are made difficult by Mercury's constant proximity to the Sun. This has several consequences:

  1. Whenever the sky is dark enough for viewing through telescopes, Mercury is always already near the horizon, where viewing conditions are poor anyway due to atmospheric factors.
  2. The Hubble Space Telescope and other space observatories are usually prevented from pointing close to the Sun for safety reasons (Erroneously pointing such sensitive instruments at the Sun is likely to cause permanent damage).

Mercury's geological history

Mercury – Gravity Anomalies – mass concentrations (red) suggest subsurface structure and evolution.

Like the Earth, Moon and

eras. From oldest to youngest, these are: the pre-Tolstojan, Tolstojan, Calorian, Mansurian, and Kuiperian. These ages are based on relative dating only.[14]

After the formation of Mercury along with the rest of the

Caloris Basin, were filled by magma eruptions from within the planet. These created smooth intercrater plains similar to the maria found on the Moon
. Later, as the planet cooled and contracted, its surface began to crack and form ridges; these surface cracks and ridges can be seen on top of other features, such as the craters and smoother plains—a clear indication that they are more recent. Mercury's period of volcanism ended when the planet's mantle had contracted enough to prevent further lava from breaking through to the surface. This probably occurred at some point during its first 700 or 800 million years of history.

Since then, the main surface processes have been intermittent impacts.

Timeline

Time unit: millions of years

Surface features

Mercury's surface is overall similar in appearance to that of the Moon, with extensive mare-like plains and heavily cratered terrains similar to the lunar highlands and made locally by accumulations of pyroclastic deposits.[6]

Topography
Map of Mercury's northern hemisphere by the MLA instrument on MESSENGER
lowest (purple) to 10 km (6.2 mi) highest (red).

Impact basins and craters

Main article:
Craters on Mercury
Caloris Basin
is one of the largest impact features in the Solar System

Craters on Mercury range in diameter from small bowl-shaped craters to

impact basins hundreds of kilometers across. They appear in all states of degradation, from relatively fresh rayed-craters, to highly degraded crater remnants. Mercurian craters differ subtly from Lunar craters – the extent of their ejecta blankets is much smaller, which is a consequence of the 2.5 times stronger surface gravity on Mercury.[14]

MASCS spectrum scan of Mercury's surface by MESSENGER
Caloris Basin
impact at its antipodal point

The largest known crater is the enormous

Skinakas Basin had been postulated from low resolution Earth-based observations of the non-Mariner-imaged hemisphere, but has not been observed in MESSENGER imagery of the corresponding terrain. The impact which created the Caloris Basin was so powerful that its effects are seen on a global scale. It caused lava eruptions and left a concentric ring over 2 km tall surrounding the impact crater. At the antipode of the Caloris Basin lies a large region of unusual, hilly and furrowed terrain, sometimes called "Weird Terrain". The favoured hypothesis for the origin of this geomorphologic unit is that shock waves generated during the impact traveled around the planet, and when they converged at the basin's antipode (180 degrees away) the high stresses were capable of fracturing the surface.[16]
A much less favoured idea was that this terrain formed as a result of the convergence of ejecta at this basin's antipode. Furthermore, the formation of the Caloris Basin appears to have produced a shallow depression concentric around the basin, which was later filled by the smooth plains (see below).

Overall about 15 impact basins have been identified on the imaged part of Mercury. Other notable basins include the 400 km wide, multi-ring,

Beethoven Basin also has a similar-sized ejecta blanket and a 625 km diameter rim.[14]

As on the Moon, fresh craters on Mercury show prominent bright ray systems. These are made by ejected debris, which tend to be brighter while they remain relatively fresh because of a lesser amount of space weathering than the surrounding older terrain.

Pit-floor craters

Some impact craters on Mercury have non-circular, irregularly shaped depressions or pits on their floors. Such craters have been termed pit-floor craters, and

lava flows but are typically distinctive in color. For example, the pits of Praxiteles have an orange hue.[17] Thought to be evidence of shallow magmatic activity, pit craters may have formed when subsurface magma drained elsewhere and left a roof area unsupported, leading to collapse and the formation of the pit. Major craters exhibiting these features include Beckett, Gibran, Lermontov, Picasso, and Navoi, among others.[18] It was suggested that these pits with associated brighter and redder deposits may be pyroclastic deposits caused by explosive volcanism.[6]

Interior of Abedin crater

Plains

There are two geologically distinct plains units on Mercury:[14][19]

The floor of the

Caloris Basin is also filled by a geologically distinct flat plain, broken up by ridges and fractures in a roughly polygonal pattern. It is not clear whether they are volcanic lavas induced by the impact, or a large sheet of impact melt.[14]

Tectonic features

Discovery Rupes.

One unusual feature of the planet's surface is the numerous compression folds which crisscross the plains. It is thought that as the planet's interior cooled, it contracted and its surface began to deform. The folds can be seen on top of other features, such as craters and smoother plains, indicating that they are more recent.

tidal bulges raised by the Sun—the Sun's tides on Mercury are about 17% stronger than the Moon's on Earth.[21]

Faculae

Faculae on Mercury are bright areas often surrounding irregular depressions. They are generally interpreted to be pyroclastic in nature.[22] The faculae on Mercury are all named using words in different languages meaning snake.

Terminology

Non-crater surface features are given the following names:

  • Albedo features – areas of markedly different reflectivity
  • List of ridges on Mercury
    )
  • Montes — mountains (see List of mountains on Mercury)
  • List of plains on Mercury
    )
  • List of scarps on Mercury
    )
  • List of valleys on Mercury
    )

High-albedo polar patches and possible presence of ice

The first radar observations of Mercury were carried out by the

Deep Space Network
site at Goldstone were at a power level of 460 kW at 8.51 GHz; the signals received by the VLA multi-dish array detected points of radar reflectivity (radar luminosity) with depolarized waves from Mercury's north pole.

Radar image of Mercury's north pole.

Radar maps of the surface of the planet were made using the Arecibo radiotelescope. The survey was conducted with 420 kW UHF band (2.4 GHz) radio waves which allowed for a 15 km resolution. This study not only confirmed the existence of the zones of high reflectivity and depolarization, but also found a number of new areas (bringing the total to 20) and was even able to survey the poles. It has been postulated that surface ice may be responsible for these high luminosity levels, as the silicate rocks that compose most of the surface of Mercury have exactly the opposite effect on luminosity.

In spite of its proximity to the Sun, Mercury may have surface ice, since temperatures near the poles are constantly below freezing point: On the polar plains, the temperature does not rise above −106 °C. Craters at Mercury's higher latitudes (discovered by radar surveys from Earth as well) may be deep enough to shield the ice from direct sunlight. Inside the craters, where there is no solar light, temperatures fall to −171 °C.[23]

Despite

sublimation
into the vacuum of space, the temperature in the permanently shadowed region is so low that this sublimation is slow enough to potentially preserve deposited ice for billions of years.

At the South Pole, the location of a large zone of high reflectivity coincides with the location of the Chao Meng-Fu crater, and other small craters containing reflective areas have also been identified. At the North Pole, a number of craters smaller than Chao-Meng Fu have these reflective properties.

The strength of the radar reflections seen on Mercury are small compared to that which would occur with pure ice. This may be due to powder deposition that does not cover the surface of the crater completely or other causes, e.g. a thin overlying surface layer. However, the evidence for ice on Mercury is not definitive. The anomalous reflective properties could also be due to the existence of deposits of

sulfates
or other materials with high reflectance.

Possible origin of ice

Mercury is not unique in having craters that stand in permanent shadow; at the south pole of Earth's

possible signs of the presence of ice have been seen (although their interpretation is disputed). It is thought by astronomers that ice on both Mercury and the Moon must have originated from external sources, mostly impacting comets. These are known to contain large amounts, or a majority, of ice. It is therefore conceivable for meteorite impacts to have deposited water in the permanently shadow craters, where it would remain unwarmed for possibly billions of years due to the lack of an atmosphere to efficiently conduct heat and stable orientation of Mercury's rotation axis
.

Mercury
Water ice (yellow) at Mercury's north polar region

Mercury's biological history

Habitability

There may be scientific support, based on studies reported in March 2020, for considering that parts of the planet Mercury may have been

life forms, albeit likely primitive microorganisms, may have existed on the planet.[24][25]

See also

References

  1. ISBN 0-412-05181-8
    .
  2. ^ Strom, R.G. in “Geology of the Terrestrial Planets,” M.H. Carr, Ed., Special Paper 469, NASA Scientific and Technical Information Branch:Washington D.C., 1984, p. 13. https://www.lpi.usra.edu/publications/books/geologyTerraPlanets/
  3. ^ MESSENGER website. Johns Hopkins Applied Physics Laboratory. https://messenger.jhuapl.edu/Explore/images/impressions/messenger-byTheNumbers-lg.jpg
  4. ^ "Solar System Exploration: Mercury". NASA. Archived from the original on 21 July 2011. Retrieved 17 February 2012.
  5. ^ "MESSENGER Team Presents New Mercury Findings". NASA. Archived from the original on 16 October 2011. Retrieved 16 February 2012.
  6. ^
    doi:10.1002/2014GL061224
    .
  7. ^ a b "Orbital Observations of Mercury". Johns Hopkins University Applied Physics Lab. Archived from the original on 26 June 2015. Retrieved 16 February 2012.
  8. ^ "The MESSENGER Gamma-Ray Spectrometer: A window into the formation and early evolution of Mercury". Johns Hopkins University Applied Physics Lab. Archived from the original on 12 December 2012. Retrieved 18 February 2012.
  9. ^ a b "Evidence of Volcanism on Mercury: It's the Pits". Johns Hopkins University Applied Physics Lab. Archived from the original on 28 April 2014. Retrieved 16 February 2012.
  10. ^ "Mercury: The Key to Terrestrial Planet Evolution". Johns Hopkins University Applied Physics Lab. Archived from the original on 4 September 2014. Retrieved 18 February 2012.
  11. ^ a b "Mercury's Oddly Offset Magnetic Field". Johns Hopkins University Applied Physics Lab. Archived from the original on 12 December 2012. Retrieved 18 February 2012.
  12. ^ "Topic: 1.2.c Mercury missions | CosmoLearning Astronomy". CosmoLearning. Retrieved 24 July 2023.
  13. ^ "Mercury Fact Sheet". nssdc.gsfc.nasa.gov. Retrieved 24 July 2023.
  14. ^
    Bibcode:2001mses.conf..100S
    .
  15. ^ Shiga, David (30 January 2008). "Bizarre spider scar found on Mercury's surface". NewScientist.com news service.
  16. S2CID 121225801
    .
  17. ^ "Overlaying Color onto Praxiteles Crater". Johns Hopkins University Applied Physics Lab. Archived from the original on 26 June 2015. Retrieved 16 February 2012.
  18. ^ "A Newly Pictured Pit-Floor Crater". Johns Hopkins University Applied Physics Lab. Archived from the original on 26 June 2015. Retrieved 16 February 2012.
  19. ^
    Bibcode:2001mses.conf..106W
    .
  20. doi:10.1029/JB083iB10p04883
    .
  21. doi:10.1029/2003JE002126
    .
  22. ^ PYROCLASTIC DEPOSITS ON MERCURY DETECTED WITH MASCS/MESSENGER DATA: IDENTIFICATION THROUGH SPECTRAL CHARACTERIZATION AND PRINCIPAL COMPONENT ANALYSIS (PCA). By A. Galiano, F. Capaccioni, G. Filacchione, C. Carli. 53rd Lunar and Planetary Science Conference (2022).
  23. ^ "Ice on Mercury". National Space Science Data Center. Retrieved 16 February 2012.
  24. ^ Hall, Shannon (24 March 2020). "Life on the Planet Mercury? 'It's Not Completely Nuts' - A new explanation for the rocky world's jumbled landscape opens a possibility that it could have had ingredients for habitability". The New York Times. Retrieved 26 March 2020.
  25. PMID 32179758
    .

Original references for Spanish article

  • Ciencias de la Tierra. Una Introducción a la Geología Física (Earth Sciences, an Introduction to Physical Geology), by Edward J. Tarbuck y Frederick K. Lutgens. Prentice Hall (1999).
  • "Hielo en Mercurio" ("Ice on Mercury"). El Universo, Enciclopedia de la Astronomía y el Espacio ("The Universe, Encyclopedia of Astronomy and the Space"), Editorial Planeta-De Agostini, p. 141–145. Volume 5. (1997)

External links

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