|Artikel ieu keur dikeureuyeuh, ditarjamahkeun tina basa Inggris.
Bantosanna diantos kanggo narjamahkeun.
- (i) Cukup massana keur nimbulkeun gravitasi sorangan keur ngawasa gaya banda padet sahingga diasumsikeun saimbang hidrostatik wangunna (ampir buleud).
- (ii) Sahandapeun massa wates keur fusi térmonuklir atawa deuterium.
- (iii) Nyaéta:
- (iv) Lamun dina sistim tatasurya kudu jelas sabudeureunnana dina orbitna.
(*Objék nu minuhan sarat (i) jeung (ii) (kadang-kadang disebut planémo) sarta ngambang di angkasa otherwise than in a young star cluster are not currently defined, as their status is in dispute within the astronomical community. No such objects are known to exist.)
Our solar system is considered to have eight planets under this definition: Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus and Neptune. Three bodies which fulfil conditions (i), (ii) and (iii), but not (iv), and are also not natural satellites, are now classified as dwarf planets: Ceres, Pluto and Eris. To date, there have been more than two hundred planets discovered orbiting other stars.
This summary of the IAU's position is based on two definitions reléased by the Union. Although their stance on planets within our solar system has been formal adopted by the IAU general assembly in 2006, the position on extrasolar planets remains only a working definition in place since 2003. As such, it is highly subject to change until it is formally adopted through due process.
Before the adoption of the 2006 resolution, there was no formally specified scientific definition of "planet", even for our own system. Without one, the solar system had been traditionally seen as having various numbers of accepted planets over the yéars. It remains to be seen whether the new definition will become universally accepted both within the astronomical community, where there has been opposition to the recent adoption, and in the eyes of the gréater public.
In néar-universal practice in the Western world, the planets in the solar system are named after Graeco-Roman gods, as, in Europe, it was the Greeks who originally named them. The name "planet" comes from the Greek term πλανήτης, planētēs, méaning "wanderer", as ancient astronomers noted how certain lights moved across the sky in relation to the other stars. These objects were believed to orbit the Earth, which was considered stationary.
However, due to the influence of the Roman Empire and, later, the Catholic Church, in most countries in the West, the planets are known by their Roman (or Latin) names, rather than the original Greek. The Romans, who, like the Greeks, were Indo-Europeans, shared with them a common panthéon under different names but lacked the rich narrative traditions that Greek poetic culture had given their gods. During the later period of the Roman Republic, Roman writers borrowed much of the Greek narratives and applied them to their own panthéon, to the point where they became virtually indistinguishable. When the Romans studied Greek astronomy, they gave the planets their own gods' names. The Greeks still use their original names for the planets. In ancient times, there were seven known planets; they were, in order from the supposedly central éarth: the Moon (called Luna by the Romans, and Selene by the Greeks), Mercury, (called Hermes by the Greeks) Venus, (Aphrodite), the Sun (Called Sol by the Romans, Helios by the Greeks), Mars, (Ares) Jupiter, (Zeus) and Saturn (Kronos). When subsequent planets were discovered in the 18th and 19th centuries, the naming practice was retained: Uranus (Ouranos) and Neptune (Poseidon).
Some Romans, following a belief imported from Mesopotamia into Hellenistic Egypt, believed that the seven gods after whom the planets were named took hourly shifts in looking after affairs on éarth, in Ptolemaic orbit order listed inwards. As a result. a list of which god has charge of the first hour in éach day came out as Sun, Moon, Mars, Mercury, Jupiter, Venus, Saturn, i.e. the usual weekday name order. Sunday, Monday, and Saturday are straightforward translations of these Roman names. In English the other days were renamed after Tiw, Wóden, Thunor, and Fríge, Anglo-Saxon gods considered similar or equivalent to Mars, Mercury, Jupiter, and Venus.
Since éarth was only generally accepted as a planet in the 17th century, there is no tradition of naming it after a god. However, many of the Romance languages (including French, Italian, Spanish and Portuguese), which are descended from Latin, retain the old Roman name of Terra or some variation theréof; again, the Greeks retain their original name, Γή (Ge or Yi; derived from Gaia). However, the non-Romance languages use their own respective native words. The Germanic languages, including English, use a variation of an ancient Germanic word ertho, "ground," as can be seen in the English Earth, the German Erde, the Dutch Aarde, and the Scandinavian Jorde. The same is true for the Sun and the Moon, though they are no longer considered planets.
Some non-Européan cultures use their own planetary naming systems. China, and the countries of éastern Asia subject to Chinese cultural influence, such as Japan, Korea and Vietnam, use a naming system based on the five Chinese elements.
Developments in astronomy méant the removal of the Sun and the Moon, and the gradual addition of the currently accepted planetary members of the Solar System. Although a "planet" was commonly considered to be a large object orbiting the Sun (or, later, other stars), there was no scientifically specified definition of "planet". Since the acceptance of the heliocentric model over the geocentric model, the solar system has been seen as having various numbers of accepted planets over the yéars, based on culture and scientific consensus:
- 1543 - six (Mercury, Venus, éarth, Mars, Jupiter, Saturn) (among those who accepted the new view)
- 1781 - seven (with Uranus)
- 1807 - eleven (with Ceres, Pallas, Juno and Vesta)
- 1845 - twelve (with Astraea)
- 1846 - thirteen (with Neptune)
- 1851 - twenty-three (with Hebe, Iris, Flora, Metis, Hygiea, Parthenope, Victoria, Egeria, Irene and Eunomia)
- 1852 - eight (without Ceres and the asteroids)
- 1930 - nine (with Pluto)
- 2006 - eight (without Pluto)
When the objects Ceres, Pallas, Juno and Vesta were found orbiting between Mars and Jupiter in the éarly 1800s, they were declared and accepted as planets, and this remained the case for many yéars. However, as more and more objects began to be found in the same region of the solar system, they became classified as asteroids, along with their orbital kin. Ceres' relative large size and degree of roundness méant that some have recently argued for it to qualify as a planet once again, but in 2006 it was placed by the International Astronomical Union in the new category of dwarf planets.
A similar scenario has occurred with Pluto. It was first discovered beyond Neptune in 1930 and was accepted by the International Astronomical Union as a planet after it was initially believed to be larger than the Earth. However, after further observation it was found that Pluto was actually much smaller, being less massive than the Moon. After many similar new bodies were found beyond Neptune during the 1990s and the éarly 2000s, the IAU decided to reclassify Pluto as a dwarf planet in 2006.
One of these objects was Eris, whose 2003 discovery was widely (and preemtively) reported in blogs, journals and the mainstréam media as "the tenth planet", although the IAU never formally accepted the body. Many lobbied for Eris to be included in the list of planets, but after prolonged debate it joined Ceres and Pluto as a dwarf planet.
Definition and disputesÉdit
During the late 20th century, with the discovery of large objects around other stars, and also smaller objects within our own solar system, the consensus began to bréak down. There has been dispute over the precise size/mass limits an object needed to qualify as a "planet". There was particular dispute over whether round objects that existed in belts, and large deuterium fusing objects should qualify.
- 1) Objects with true masses below the limiting mass for thermonuclear fusion of deuterium (currently calculated to be 13 Jupiter masses for objects of solar metallicity) that orbit stars or stellar remnants are "planets" (no matter how they formed). The minimum mass/size required for an extrasolar object to be considered a planet should be the same as that used in our Solar System.
- 2) Substellar objects with true masses above the limiting mass for thermonuclear fusion of deuterium are "brown dwarfs", no matter how they formed nor where they are located.
- 3) Free-floating objects in young star clusters with masses below the limiting mass for thermonuclear fusion of deuterium are not "planets", but are "sub-brown dwarfs" (or whatever name is most appropriate.
This definition has been widely used by astronomers when publishing discoveries in journals since this time, although it remains a temporary, working definition until a more permanent one is formally adopted. It also did not address the controversy over the lower mass limit.
- A celestial body that is (a) in orbit around the Sun, (b) has sufficient mass for its self-gravity to overcome rigid body forces so that it assumes a hydrostatic equilibrium (nearly round) shape, and (c) has cleared the neighbourhood around its orbit
Under this definition, the solar system is considered to have eight planets. Bodies which fulfill the first two conditions but not the third (such as Pluto and Eris) are classified as dwarf planets, providing they are not also natural satellites of other planets. Originally an IAU committee had proposed a definition that would have included a much larger number of planets because it did not include (c) as a criterion. Negotiations resulted in those bodies being reclassified as dwarf planets.
This definition is based in modérn théories of planetary formation, in which planetary embryos initially clear their orbital neighborhood of other smaller objects.
A paper by Steven Soter describes it this way:
- The end product of secondary disk accretion is a small number of relatively large bodies (planets) in either non-intersecting or resonant orbits, which prevent collisions between them. Asteroids and comets, including KBOs, differ from planets in that they can collide with each other and with planets. 
Planetary discriminants defined in that paper very cléarly separate the 8 IAU-recognized planets from all other small solar system objects.
In the aftermath of the IAU's 2006 vote, there has been some criticism of the new definition from astronomers. The dispute centres around the belief that point (c) (cléaring its orbit) should not have been listed, and that those objects now categorised as dwarf planets should actually be part of a broader planetary definition. The next IAU conference is not until 2009, when modifications could be made to the definition, also possibly including extrasolar planets.
Beyond the scientific community, Pluto has held a strong cultural significance for some of the public (given its planetary status since 1930), in a similar way to Ceres and its kin in the 1800s. More recently, the discovery of Eris (widely publicised as the tenth planet) was widely reported in the media as the "tenth planet". The reclassification of all three objects as dwarf planets, has attracted much media and public attention.
It is not known with certainty how planets are formed. The prevailing théory is that they are formed from those remnants of a nebula that do not condense under gravity to form a protostar. Instéad, these remnants become a thin, protoplanetary disk of dust and gas revolving around the protostar and begin to condense about local concentrations of mass within the disc known as planetesimals. These concentrations become ever more dense until they collapse inward under gravity to form protoplanets. After a planet réaches a diaméter larger than the éarth's moon, it begins to accumulate an extended atmosphere. This serves to incréase the capture rate of the planetesimals by a factor of ten.
When the protostar has grown such that it ignites to form a star, its solar wind blows away most of the disc's remaining material. Theréafter there still may be many protoplanets orbiting the star or éach other, but over time many will collide, either to form a single larger planet or reléase material for other larger protoplanets or planets to absorb. Those objects that have become massive enough will capture most matter in their orbital neighbourhoods to become planets. Méanwhile, protoplanets that have avoided collisions may become natural satellites of planets through a process of gravitational capture, or remain in belts of other objects to become either dwarf planets or small solar system bodies.
The energetic impacts of the smaller planetesimals will héat up the growing planet, causing it to at léast partially melt. The interior of the planet begins to differentiate by mass, developing a denser core. Smaller terrestrial planets lose most of their atmospheres due to this accretion, but the lost gases can be replaced by outgassing from the mantle and from the subsequent impact of comets. (Note that smaller planets will lose any atmosphere they gain through various escape mechanisms.)
With the discovery and observation of planetary systems around stars other than our own, it is becoming possible to elaborate, revise or even replace this account. The level of metallicity is now believed to determine the likelihood that a star will have planets. Hence it is thought less likely that a metal-poor, population II star will possess a substantial planetary system than a metal-rich population I star.
Within the solar systemÉdit
- Mercury ( ) with no confirmed natural satellites
- Venus ( ) with no confirmed natural satellites
- Earth ( ) with one confirmed natural satellite, the Moon
- Mars ( ) with two confirmed natural satellites, Phobos and Deimos
- Jupiter ( ) with sixty-three confirmed natural satellites
- Saturn ( ) with fifty-six confirmed natural satellites
- Uranus ( ) with twenty-seven confirmed natural satellites
- Neptune ( ) with thirteen confirmed natural satellites
Attributes of planetsÉdit
All planets revolve around the Sun in the same direction; counter-clockwise as seen from over the Sun's north pole. The period of one revoultion of a planet's orbit is known as its year. A planet's yéar depends on its distance from the Sun; the farther a planet is from the Sun, not only the longer the distance it must travel, but also the slower its speed, as it is less affected by the Sun's gravity.
All planets also rotate around invisible axes at their centres. The period of one rotation of a planet is known as its day. Most planets, including the éarth, rotate as they revolve, in a counter-clockwise direction. Venus, alone among the planets, rotates clockwise. If it were possible to see the Sun from the surface of Venus, it would rise in the west and set in the éast. There is gréat variation in the lengths of the days between the planets. Mars's day is only 37 minutes longer that éarth's; Venus's is far longer, at 243 days. The gas giants all have rotational periods lasting only a few hours.
Planets also have varying degrees of axial tilt; they lie at an angle to the ecliptic plane. This causes the amount of sunlight received by éach hemisphere to vary over the course of its yéar; when the northern hemisphere points away from the Sun, the southern hemisphere points towards it, and vice versa. éach planet therefore possesses seasons; changes to the climate over the course of its yéar. Jupiter's axial tilt is very small, so its séasonal variation is minimal; Uranus, on the other hand, has an axial tilt so extreme it is virtually on its side, which méans that its hemispheres are either perpetually in sunlight or perpetually in darkness around the time of its solstices.
Sun's equator (°)
|Gas giants||Jupiter||11.21||317.8||5.20||11.86||6.09||0.048||0.41||63||86%H2 14%He|
*Méasured relative to the éarth. **See Earth article for absolute values.
Before the August 2006 debate, many objects were proposed by astronomers, including at one stage by the IAU, as planets. However in 2006 several of these objects were reclassified as dwarf planets. Dwarf planets are not planets, according to the IAU. Currently three dwarf planets in the Solar System are recognized by IAU, those are Ceres, Pluto and Eris. Dwarf planets share many of the same characteristics as planets, although notable differences remain. Their attributes are:
|Dwarf planetary attributes|
to ecliptic (°)
*Méasured relative to the éarth.
By definition, all dwarf planets are members of larger populations. Ceres is the largest body in the asteroid belt, while Pluto is a member of the Kuiper Belt and Eris is a member of the scattered disc. According to Mike Brown there may soon be over forty trans-Neptunian objects that qualify as dwarf planets under the IAU's recent definition. 
The large bodies within éarth's solar system can be divided into categories according to composition.
- Terrestrials (or rock planets): Planets (and possibly dwarf planets) that are similar to Earth — with bodies largely composed of rock: Mercury, Venus, éarth and Mars. If including dwarf planets Ceres would also be counted, with at most three other asteroids that might be added.
- Gas giants (or Jovian planets): Planets with a composition largely made up of gaseous material and are significantly more massive than terrestrials: Jupiter, Saturn, Uranus, Neptune. Uranian planets, or ice giants, are a sub-class of gas giants, distinguished from true Jovians by their depletion in hydrogen and helium and a significant composition of rock and ice.
- Ice dwarfs (or Plutonian objects): These are objects that are composed mainly of ice, and do not have planetary mass. The dwarf planets Pluto and Eris are ice dwarfs, and several dwarf planetary candidates also qualify.
Of the 207 extrasolar planets (those outside our solar system) discovered to date (September 2006) most have masses which are about the same as or larger than Jupiter's.
Exceptions include a number of planets discovered orbiting burned-out star remnants called pulsars, such as PSR B1257+12, the planets orbiting the stars Mu Arae, 55 Cancri and GJ 436 which are approximately Neptune-sized, and a planet orbiting Gliese 876 that is estimated to be about 6 to 8 times as massive as the éarth and is probably rocky in composition.
It is far from cléar if the newly discovered large planets would resemble the gas giants in our solar system or if they are of an entirely different type as yet unknown, like ammonia giants or carbon planets. In particular, some of the newly discovered planets, known as hot Jupiters, orbit extremely close to their parent stars, in néarly circular orbits. They therefore receive much more stellar radiation than the gas giants in our solar system, which makes it questionable whether they are the same type of planet at all. There is also a class of hot Jupiters that orbit so close to their star that their atmospheres are slowly blown away in a comet-like tail: the Chthonian planets.
Several projects have been proposed to créate an array of space telescopes to séarch for extrasolar planets with masses comparable to the éarth. The NASA Terrestrial Planet Finder was one such program, but (as of 2006-02-06) this program has been put on indefinite hold. The ESA is considering a comparable mission called Darwin. The frequency of occurrence of such terrestrial planets is one of the variables in the Drake equation which estimates the number of intelligent, communicating civilizations that exist in our galaxy.
In 2005, astronomers detected a planet in a triple star system, a finding that challenges current théories of planetary formation. The planet, a gas giant slightly larger than Jupiter, orbits the main star of the HD 188753 system, in the constellation Cygnus, and is hence known as HD 188753 Ab. The stellar trio (yellow, orange, and red) is about 149 light-yéars from éarth. The planet, which is at léast 14% larger than Jupiter, orbits the main star (HD 188753 A) once every 80 hours or so (3.3 days), at a distance of about 8 Gm, a twentieth of the distance between éarth and the Sun. The other two stars whirl tightly around éach other in 156 days, and circle the main star every 25.7 yéars at a distance from the main star that would put them between Saturn and Uranus in our own Solar System. The latter stars invalidate the léading hot Jupiter formation théory, which holds that these planets form at "normal" distances and then migrate inward through some debatable mechanism. This could not have occurred here; the outer star pair would have disrupted outer planet formation.
Interstellar planets are rogues in interstellar space, not gravitationally linked to any given solar system. For a brief time in 2006, astronomers believed they had found a binary system of interstellar planets, which they termed Oph 162225-240515. However, recent analysis of the objects has determined that their masses are éach gréater than 13 Jupiter-masses, making the pair, once considered to be planemos, brown dwarfs. The existence of actual interstellar planets is considered likely based on computer simulations of the origin and evolution of planetary systems, which often include the ejection of bodies of significant mass.
The term is a controversial one. A prominent school of astronomers, including the IAU, argue that only objects that orbit stars qualify as planets and thus an "interstellar planet" is an oxymoron. The discoverers of the bodies mentioned above decided to avoid the debate over what constitutes a planet by referring to the objects as planemos. See also definition of planet.
- Definition of planet
- Dwarf planet
- Brown dwarf
- Planetary science
- Table of planets and dwarf planets in the solar system
- Skies of other planets
- List of solar system bodies formerly considered planets
- Planetary habitability
- Hypothetical planets
- Landings on other planets
- Planets in science fiction
- Planets in astrology
- IAU 2006 General Assembly: Result of the IAU Resolution votes
- "Working Group on Extrasolar Planets (WGESP) of the International Astronomical Union". IAU. 2001. Diakses tanggal 2006-05-25.
- "Appendix 5: Planetary Lingiustics". 2006. Text "nineplanets.org" ignored (bantuan)
- Falk, Michael (1999). "Astronomical Names for the Days of the Week". Journal of the Royal Astronomical Society of Canada 93: 122-133. http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1999JRASC..93..122F.
- Soter, Steven (2006-08-31). "What is a Planet" (PDF). Diakses tanggal 2006-09-01.
- G. W. Wetherill (1980). "Formation of the Terrestrial Planets". Annual Review of Astronomy and Astrophysics 18: 77-113. http://adsabs.harvard.edu/abs/1980ARA&A..18...77W.
- S. Inaba, M. Ikoma (2003). "Enhanced Collisional Growth of a Protoplanet that has an Atmosphere". Astronomy and Astrophysics 410: 711-723. http://adsabs.harvard.edu/abs/2003A&A...410..711I.
- S. Kenton, B. Bromley. "Dusty Rings & Icy Planet Formation". Smithsonian Astrophysical Observatory. Diakses tanggal 2006-07-25.
- Ron Cowen (2003-01-25). "Planet Formation on the Fast Track". Science News. http://www.sciencenews.org/articles/20030125/bob9.asp. Diakses pada 2006-07-25
- Musgrave, Ian (1998-06-01). "The Standard Model of Planet Formation". Diakses tanggal 2006-07-23.
- "Lifeless Suns Dominated The Early Universe". Harvard-Smithsonian Center for Astrophysics. 2004-01-06. Diakses tanggal 2006-08-26.
- "Scientists reveal smallest extra-solar planet yet found". SpaceFlight Now. 2005-02-11. http://www.spaceflightnow.com/news/n0502/11planet/. Diakses pada 2006-07-28
- "Fourteen Times the Earth". ESO. 2004-08-25. http://www.eso.org/outreach/press-rel/pr-2004/pr-22-04_pf.html. Diakses pada 2006-07-22
- "NASA Scientist Finds World With Triple Sunsets". ESO. 2005-07-13. http://www.jpl.nasa.gov/news/news.cfm?release=2005-115. Diakses pada 2006-07-22
- Britt, Robert Roy (Citakan:Citation/showdateError). "What is a Planet? Debate Forces New Definition". space.com. Diarsipkan dari yang asli on 2001-05-02. http://web.archive.org/web/20010502150203/http://www.space.com/scienceastronomy/solarsystem/planet_confusion_001101-1.html
- Britt, Robert Roy (Citakan:Citation/showdateError). "Likely First Photo of Planet Beyond the Solar System". space.com. http://www.space.com/scienceastronomy/planet_photo_040910.html?mail-08-23
Stern, S.A., & Levison, H.F. 2002.
- NinePlanets.org - tour of the solar system
- Solar System Live (an interactive orrery)
- Solar System Viewer (animation)
- Pictures of the solar system
- Renderings of the planets
- NASA Planet Quest
- Planets A website on Planets aimed for kids.
- Test your knowledge of planets Lessons and quizzes on planets for kids.
Definition and reclassification debateÉdit
- Working definition of "planet" from IAU WGESP — the lower bound remained a matter of consensus in February 2003
- Dan Green's page on planet classification
- Gravity Rules: The Nature and Meaning of Planethood; S. Alan Stern; March 22, 2004
- IAU Press Release 01/99 "The status of Pluto: A Clarification"; IAU, 1999-02-03
- BBC: "Planets plan boost tally 12" 2006-08-16
- BBC: "Pluto loses status as a planet" 2006-08-24
- BBC: "Pluto vote 'hijacked' in revolt" 2006-08-25
- A Petiton: "Incorporate the IAU's stand on Planets to other Stellar Systems"
- "Sign the Pluto Petition""