Planetary surface
A planetary surface is where the solid (or liquid) material of the outer crust on certain types of astronomical objects contacts the atmosphere or outer space; planetary surfaces are found on solid objects of planetary mass (PMO)s, including terrestrial planets, dwarf planets, natural satellites, planetesimals and many other Small Solar System bodies (SSSB)s.[1][2][3] The study of planetary surfaces is a field of planetary geology known as surface geology but also a focus of a number of fields including planetary cartography, topography, geomorphology, atmospheric sciences and astronomy. Land (or ground) is the term given to non-liquid planetary surfaces. The term "landing" is used to describe the collision of an object with a planetary surface and is usually at a velocity in which the object can remain intact and remain attached.
In differentiated bodies, the surface is where the crust meets the planetary boundary layer. Anything below this is regarded as being sub-surface or sub-marine. Most bodies more massive than Super-Earths, including stars and gas giants, as well as smaller gas dwarfs, transition contiguously between phases including gas, liquid and solids. As such they are generally regarded as lacking surfaces.
Planetary surfaces and surface life are of particular interest to humans as it the primary habitat of the species, which has evolved to move over land and breathe air. Human space exploration and space colonization therefore focuses heavily on them. Humans have only directly explored the surface of the Earth and Moon. The vast distances of space and the complexities of makes direct exporation of even Near-Earth objects dangerous and expensive. As such, all other exploration has been indirect via Space probes.
Indirect observations by flyby or orbit currently provide insufficient information to confirm the composition and properties of planetary surfaces. Much of what is known is from the use of techniques such as astronomical spectroscopy. Lander spacecraft have explored the surfaces of planets Mars and Venus. Mars is the only other planet to have had its surface explored by a mobile surface probe (rover). Titan is the only non-planetary object of planetary mass to have been explored by lander. Landers have explored several smaller bodies including 433 Eros, 25143 Itokawa, Tempel 1 and 67P/Churyumov–Gerasimenko.
Distribution and conditions
Planetary surfaces are found throughout the Solar System, from the inner terrestrial planets, to the asteroid belt, the natural satellites of the gas giant planets and beyond to the Trans-Neptunian objects. Surface conditions, temperatures and terrain vary significantly due to a number of factors including Albedo often generated by the surfaces itself. Measures of surface conditions include surface area, surface gravity, surface temperature and surface pressure. Surface stability may be affected by erosion through Aeolian processes, hydrology, subduction, volcanism, sediment or seismic activity. Some surfaces are dynamic while others remain unchanged for millions of years.
Exploration
Distance, gravity, atmospheric conditions (extremely low or extremely high atmospheric pressure) and unknown factors make exploration is both costly and risky. This necessitates the space probes for early exploration of planetary surfaces. Many probes are stationary have a limited study range and generally survive on extraterrestrial surfaces for a short period, however mobile probes (rovers) have surveyed larger surface areas. Sample return missions allow scientist to study extraterrestrial surface materials on Earth without having to send a manned mission, however is generally only feasible for objects with low gravity and atmosphere.
Past missions
The first extraterrestrial planetary surface to be explored was the lunar surface by Luna 2 in 1959. The first and only human exploration of an extraterrestrial surface was the Moon, the Apollo program included the first moonwalk on July 20, 1969 and successful return of extraterrestrial surface samples to Earth. Venera 7 was the first landing of a probe on another planet on December 15, 1970. Mars 3 "soft landed" and returned data from Mars on August 22, 1972, the first rover on Mars was Mars Pathfinder in 1997, the Mars Exploration Rover has been studying the surface of the red planet since 2004. NEAR Shoemaker was the first to soft land on an asteroid - 433 Eros in February 2001 while Hayabusa was the first to return samples from 25143 Itokawa on 13 June 2010. Huygens soft landed and returned data from Titan on January 14, 2005.
There have been many failed attempts, more recently Fobos-Grunt, a sample return mission aimed at exploring the surface of Phobos.
Future missions
In May 2011, NASA announced the OSIRIS-REx sample return mission to asteroid 1999 RQ36, and is expected to launch in 2016.
Surface materials
| Some planetary surfaces of the Solar System and their compositions | ||||||||
|---|---|---|---|---|---|---|---|---|
|
The most common planetary surface material in the Solar System appears to be water ice. Surface ice is found as close to the Sun as Mercury but is more abundant beyond Mars. Other surfaces include solid matter in combinations of rock, regolith and frozen chemical elements and chemical compounds. In general, ice predominates planetary surfaces beyond the frost line, while closer to the sun, rock and regolith predominate. Minerals and hydrates may also be present in smaller quantities on many planetary surfaces.
Rare surface occurrences
Surface liquid, while abundant on Earth (the largest body of surface liquid being the World Ocean) is rare elsewhere, a notable exception being Titan which has the largest known hydrocarbon lake system (Lakes of Titan) while surface water, abundant on Earth and essential to all known forms of life is thought only to exist as Seasonal flows on warm Martian slopes and in the habitable zones of other planetary systems.
Volcanism can cause flows such as lava on the surface of geologically active bodies (the largest being the Amirani (volcano) flow on Io). Many of Earth's Igneous rocks are formed through processes rare elsewhere, such as the presence of volcanic magma and water. Surface mineral deposits such as olivine and hematite discovered on Mars by lunar rovers provide direct evidence of past stable water on the surface of Mars.
Apart from water, many other abundant surface materials are unique to Earth in the Solar System as they are not only organic but have formed due to the presence of life - these include carbonate hardgrounds, limestone, vegetation and artificial structures although the latter is present due to probe exploration (see also List of artificial objects on extra-terrestrial surfaces).
List of common surface materials
The following is a non-exhaustive list of surface materials that occur on more than one planetary surface along with their locations in order of distance from the Sun. Some have been detected by spectroscopy or direct imaging from orbit or flyby.
- Ice - Mercury (polar); Earth-Moon system;[4] Mars (polar); Ceres and some asteroids such as 24 Themis;[5] Jupiter moons - Europa,[6] Ganymede and Callisto; Triton,;[7] Saturn moons - Titan, Enceladus and Miranda; Uranus moons - Umbriel, Oberon; Kuiper belt objects including Pluto-Charon system, Haumea, 28978 Ixion, 90482 Orcus, 50000 Quaoar
- Silicate rock - Mercury, Venus, Earth, Mars, asteroids, Ganymede, Callisto, Moon, Triton
- Regolith - Mercury;[8] Venus,[9] Earth-Moon system; Mars (and its moons Phobos and Deimos); asteroids (including 4 Vesta[10]); Titan
- Methane clathrate - Oberon, Titania, Umbriel, Pluto, 90482 Orcus
- Tholins - many Trans Neptunian Objects including Titan, Triton, Eris, Sedna, 28978 Ixion, 90482 Orcus
- Nitrogen ice - Pluto-Charon,[11] Triton,[12] Kuiper belt objects, Plutinos
- Sulphur - Mercury; Earth; Mars; Jupiter moons - Io and Europa
- Dry ice - Mars (polar), Umbriel
- Sand - Earth, Mars, Titan
- Clays - Earth, Mars,[13] Ceres[14] Europa[15]
- Water - Earth
- Liquid Hydrocarbons - Titan
Landforms
Common surface features include: impact craters (though rarer on bodies with thick atmospheres, the largest being Hellas Planitia on Mars), rilles, mountains (the highest being Rheasilvia on 4 Vesta), escarpments, canyons and valleys (the largest being Valles Marineris on Mars). Some subsurface features that puncture the surface include caves and lava tubes.
Surface of gas giants
Normally, gas giants are considered to not have a surface, although they might have a solid core of rock or various types of ice, or a liquid core of metallic hydrogen. However, the core, if it exists, does not include enough of the planet's mass to be actually considered a surface. Some scientists consider the point at which the atmospheric pressure is equal to 1 bar, equivalent to the atmospheric pressure at Earth’s surface, to be the surface of the planet.
References
- ↑ Charles Meyer; Allan H. Treiman; Theodor Kostiuk, eds. (May 12–13, 1995), "Planetary Surface Instruments Workshop" (PDF), Planetary Surface Instruments Workshop (PDF), Houston, Texas: Lunar and Planetary Institute, p. 3, retrieved 2012-02-10
- ↑ "Planetary Surface materials". Haskin Research Group. Retrieved 2012-02-10.
- ↑ Melosh, Jay (August 2007). Planetary Surface Processes. Cambridge Planetary Science. p. 9. ISBN 978-0-521-51418-7.
- ↑ http://nssdc.gsfc.nasa.gov/planetary/ice/ice_moon.html
- ↑ http://www.space.com/8305-water-ice-discovered-asteroid-time.html
- ↑ "Europa: Another Water World?". Project Galileo: Moons and Rings of Jupiter. NASA, Jet Propulsion Laboratory. 2001. Retrieved 9 August 2007.
- ↑ McKinnon, William B.; Kirk, Randolph L. (2007). "Triton". In Lucy Ann Adams McFadden; Lucy-Ann Adams; Paul Robert Weissman; Torrence V. Johnson. Encyclopedia of the Solar System (2nd ed.). Amsterdam; Boston: Academic Press. pp. 483–502. ISBN 978-0-12-088589-3.
- ↑ "The regolith of Mercury: present knowledge and implications for the Mercury Orbiter mission". Planetary and Space Science 45: 31–37. 1997. Bibcode:1997P&SS...45...31L. doi:10.1016/s0032-0633(96)00098-0.
- ↑ Keith Scott; Colin Pain (18 August 2009). Regolith Science. Csiro Publishing. pp. 390–. ISBN 978-0-643-09996-8.
- ↑ Pieters, C. M.; Ammannito, E.; Blewett, D. T.; Denevi, B. W.; De Sanctis, M. C.; Gaffey, M. J.; Le Corre, L.; Li, J. -Y.; Marchi, S.; McCord, T. B.; McFadden, L. A.; Mittlefehldt, D. W.; Nathues, A.; Palmer, E.; Reddy, V.; Raymond, C. A.; Russell, C. T. (2012). "Distinctive space weathering on Vesta from regolith mixing processes". Nature 491 (7422): 79–82. Bibcode:2012Natur.491...79P. doi:10.1038/nature11534. PMID 23128227.
- ↑ "Flowing nitrogen ice glaciers seen on surface of Pluto after New Horizons flyby". ABC. 25 July 2015. Retrieved 6 October 2015.
- ↑ McKinnon, William B.; Kirk, Randolph L. (2014). "Triton". In Spohn, Tilman; Breuer, Doris; Johnson, Torrence. Encyclopedia of the Solar System (3rd ed.). Amsterdam; Boston: Elsevier. pp. 861–882. ISBN 978-0-12-416034-7.
- ↑ Clays On Mars: More Plentiful Than Expected Science Daily. Dec. 20, 2012
- ↑ A.S. Rivkina, E.L. Volquardsenb, B.E. Clark. 'The surface composition of Ceres: Discovery of carbonates and iron-rich clays'
- ↑ "Clay-Like Minerals Found on Icy Crust of Europa". JPL, NASA.gov. December 11, 2013.
- ↑ Gipson, Lillian (24 July 2015). "New Horizons Discovers Flowing Ices on Pluto". NASA. Retrieved 24 July 2015.