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Plüton, formal adı 134340 Pluto, Güneş Sistemi'nde Eris'ten sonra bilinen en büyük cüce gezegen ve doğrudan Güneş'in etrafında dönen en büyük onuncu cisim. Önceleri gezegen olarak sınıflandırılmıştır; Plüton, birçok cismi barındıran Kuiper kuşağı'nın en belirgin üyelerinden biridir.[note 1]

Plüton, diğer Kuiper kuşağı üyelerine benzer biçimde taş ve buz'dan oluşmaktadır; ancak bu kuşaktaki gezegenlere nispeden oldukça küçüktür. Kütle ve hacim olarak Ay'dan bile daha küçüktür. Plüton, eksenindeki eksantrik (dış merkezli) eğim sayesinde Güneş'e Neptün'den daha yakındır.

Plüton, 1930'da keşfedildikten 2006'ya kadar olan süre içerisinde Güneş Sistemi'nin dokuzuncu gezegeni olarak düşünülmüştür. 70'li yılları takip eden senelerde, Solar Sistemi'n dışında bir cüce gezegen olan 2060 Chiron saptanmıştır. Bu durumdan önce küçük bir gezegen olarak düşünülen Plüton'nun, gezegen olma statüsü tartışılmaya başlanmıştır.[1] 20. yüzyılın sonlarını ve 21. yüzyılın başlarını kapsayan dönemde, Güneş Sistemi'nin dışında Plüton'a benzeyen birçok cisim saptanmıştır, bunların en önemlisi 2005'te saptanan ve Plüton'dan yaklaşık %27 daha büyük olan Eris olmuştur.[2] 24 Ağustos 2006'da, Uluslararası Astronomi Birliği (IAU ya da UAB) Güneş Sistemi'nde bir gezegen olmanın koşullarını tanımlamıştır. Bu tanımlama sonrasında Plüton gezgenlikten çıkartılmış, Eris ve Ceres ile birlikte yeni bir küme olan "cüce gezegenler" sınıfının içerisine dahil edilmiştir.[3] Bunun ardından Plüton yeniden sınıflandırılmış, küçük gezegenler dizinine eklenmiş ve astronomik adı yani numarası 134340 olarak değiştirilmiştir.[4][5] Plüton, bazı araştırmacılar tarafından hala gezegen olarak onaylanmaktadır.[6]

Şaron, ay ve Plüton'dan bile daha büyüktür, bazı bilim insanlarınca ikili uzay sistemi'nde gösterilir, çünkü yörüngesi başka bir ağırlık merkezinin içinde yer almaz.[7] IAU tarafından Plüton cüce gezegen sınıfına alınana dek geçen ürede, Şaron Plüton'un uydusu olarak kabul edildi.[8] Plüton'un bilinen iki küçük uydusu vardır, bunlar Niks ve Hidra'dır. Bu uydular 2005'te saptanmıştır.[

Kaşif Clyde Tombaugh
Keşif Tarihi 18 Şubat 1930
Astronomi'de İsmi B
Kategori [Cüce Gezegen]
Yörüngesel Özellikleri C
Dönem 15846
Dışmerkezlik (e) 0.24880766
Yarı büyük eksen (a) 39.481 686 77 AB
5,906,376,272 km
3,670,060,865 mil
Enberi (q) 29.658 340 67 AB
4,436,824,613 km
2,756,921,611 mil
Enöte (Q) 49.305 032 87 AB
7,375,927,931 km
4,583,200,123 mil
Dolanma Süresi (P) 6.387230 gün
Yörünge Hızı 4.666 km/sn
Yörünge Eğikliği (i) 17.141 75°
Fiziksel Özellikler
Boyutları
Kütle 1.305×10²² kg (0.0021 x Dünya)20
Yoğunluk 2.03 g/cm³
Yerçekimi 0.58 m/sn²
Kurtulma Hızı 1.2 km/s
Dönme Süresi 6.387230 gün
Tayf Sınıfı 54545411 Yeni ismi Plütoin
Kadir 13.65 e kadar
Albedo 0.49-0.66
Ortalama Yüzey Sıcaklığı ~44 K

Saptanma [değiştir]
Ana madde: Planets beyond Neptune
Dosyaluto discovery plates.png
Discovery photographs of Pluto

1840'da, klasik mekaniğin kullanılmasıyla, Urbain Le Verrier tarafından Uranüs'ün yörüngesindeki kuşkular analiz edildi ve henüz saptanmamış bir gezegen olan Neptün'ün konumu tahmin edildi.[10] 19. yüzyıldan sonra yağılan gözlemlerde, Uranüs'ün yörüngeleri üzerindeki kuramlar, Neptün'ün ayrı bir gezegen olarak kabul edilmesi konusunu tartışmaya açtı. 1906'da, varlıklı bir Bostonlu olan Percival Lowell, Lowell Gözlemevi'ni kurdu, 1984'te Flagstaff, Arizona'da başladığı anstronomik arayışlar sonucunda, Neptün'ün gözlenmesi imkanlı hale geldi ve Neptün'e Lowell tarafından "X Gezegeni" adı verildi.[11] 1909'da, Lowell ve William H. Pickering böyle bir gezegen için çeşitli gök koordinatları önerdi.[12] Lowell'in 1916'daki ölümüne dek yapılan çalışmalardan bir sonuç alınamadı. 19 Mart 1915'te, Lowell Gözlemevi'nde Plüton'un iki fotoğrafı çekilmesine rağmen, bu yeni cisim fark edilemedi.[12][13]

Bu ölümün ardından, Constance Lowell'in Percival'le on yıl süren miras hukuku mücadelesi nedeniyle, milyon dolarlık gözlemevi işleyemez duruma geldi. Özetle X Gezegeni 1929'a kadar aranamadı,[14] Vesto Melvin Slipher'in yönetici olmasıyla, summarily handed the job of locating Planet X to Clyde Tombaugh, a 23-year-old Kansas man who had just arrived at the Lowell Observatory after Slipher had been impressed by a sample of his astronomical drawings.[14]

Tombaugh's task was to systematically image the night sky in pairs of photographs taken two weeks apart, then examine each pair and determine whether any objects had shifted position. Using a machine called a blink comparator, he rapidly shifted back and forth between views of each of the plates, to create the illusion of movement of any objects that had changed position or appearance between photographs. On February 18, 1930, after nearly a year of searching, Tombaugh discovered a possible moving object on photographic plates taken on January 23 and January 29 of that year. A lesser-quality photograph taken on January 21 helped confirm the movement.[15] After the observatory obtained further confirmatory photographs, news of the discovery was telegraphed to the Harvard College Observatory on March 13, 1930.[12]
Name [değiştir]
Dosya:Venetia phair.jpg
Venetia Burney

The discovery made headlines across the globe. The Lowell Observatory, who had the right to name the new object, received over 1000 suggestions from all over the world, ranging from Atlas to Zymal.[16] Tombaugh urged Slipher to suggest a name for the new object quickly before someone else did.[16] Constance Lowell proposed Zeus, then Percival and finally Constance – her own first name. These suggestions were disregarded.[17]

The name Pluto was proposed by Venetia Burney (1918–2009), an eleven-year-old schoolgirl in Oxford, England.[18] Venetia was interested in classical mythology as well as astronomy, and considered the name, that of the Roman god of the underworld, appropriate for such a presumably dark and cold world. She suggested it in a conversation with her grandfather Falconer Madan, a former librarian at the University of Oxford's Bodleian Library. Madan passed the name to Professor Herbert Hall Turner, who then cabled it to colleagues in the ****** States.[19]

The object was officially named on March 24, 1930.[20][21] Each member of the Lowell Observatory was allowed to vote on a short-list of three: Minerva (which was already the name for an asteroid), Cronus (which had lost reputation through being proposed by the unpopular astronomer Thomas Jefferson Jackson See), and Pluto. Pluto received every vote.[22] The name was announced on May 1, 1930.[18] Upon the announcement, Madan gave Venetia five pounds as a reward.[18]

It has been noted that the first two letters of Pluto are the initials of Percival Lowell, and Pluto's astronomical symbol () is a monogram constructed from the letters 'PL'.[23] Pluto's astrological symbol resembles that of Neptune (), but has a circle in place of the middle prong of the trident ().

The name was soon embraced by wider culture. In 1930, Walt Disney introduced for Mickey Mouse a canine companion, named Pluto apparently in the object's honour, although Disney animator Ben Sharpsteen could not confirm why the name was given.[24] In 1941, Glenn T. Seaborg named the newly created element plutonium after Pluto, in keeping with the tradition of naming elements after newly discovered planets, such as uranium, which was named after Uranus, and neptunium, which was named after Neptune.[25]

In Chinese, Japanese and Korean the name was translated as underworld king star (冥王&#26143, [26][27] as suggested by Houei Nojiri in 1930.[28] Many other non-European languages use a transliteration of "Pluto" as their name for the object; however, some Indian languages use a form of Yama, the Guardian of Hell in Hindu mythology, such as the Gujarati Yamdev.[26]
Demise of Planet X [değiştir]

Clyde W. Tombaugh, the discoverer of Pluto
Mass estimates for Pluto:Year Mass Notes
1931 1 Earth Nicholson & Mayall [29][30][31]
1948 0.1 (1/10 Earth) Kuiper [32]
1976 0.01 (1/100 Earth) Cruikshank, Pilcher, & Morrison [33]
1978 0.002 (2/1,000 Earth) Christy & Harrington [34]


Once found, Pluto's faintness and lack of a resolvable disc cast doubt on the idea that it was Lowell's Planet X. Estimates of Pluto's mass were revised downward throughout the 20th century. In 1978, the discovery of Pluto's moon Charon allowed the measurement of Pluto's mass for the first time. Its mass, roughly 0.2% that of the Earth, was far too small to account for the discrepancies in the orbit of Uranus. Subsequent searches for an alternate Planet X, notably by Robert Sutton Harrington,[35] failed. In 1992, Myles Standish used data from Voyager 2's 1989 flyby of Neptune, which had revised the planet's total mass downward by 0.5%, to recalculate its gravitational effect on Uranus. With the new figures added in, the discrepancies, and with them the need for a Planet X, vanished.[36] Today, the majority of scientists agree that Planet X, as Lowell defined it, does not exist.[37] Lowell had made a prediction of Planet X's position in 1915 that was fairly close to Pluto's actual position at that time; however, Ernest W. Brown concluded almost immediately that this was a coincidence,[38] a view still held today.[36]
Orbit and rotation [değiştir]

Orbit of Pluto—ecliptic view. This 'side view' of Pluto's orbit (in red) shows its large inclination to Neptune's orbit (in blue). The ecliptic is horizontal

This diagram shows the relative positions of Pluto (red) and Neptune (blue) on selected dates. The size of Neptune and Pluto is depicted as inversely proportional to the distance between them to emphasise the closest approach in 1896.

Pluto's orbital period is 248 Earth years. Its orbital characteristics are substantially different from those of the planets, which follow nearly circular orbits around the Sun close to a flat reference plane called the ecliptic. In contrast, Pluto's orbit is highly inclined relative to the ecliptic (over 17°) and highly eccentric (elliptical). This high eccentricity means a small region of Pluto's orbit lies nearer the Sun than Neptune's. The Pluto–Charon barycentre came to perihelion on September 5, 1989,[39][note 2] and was last closer to the Sun than Neptune between February 7, 1979 and February 11, 1999.[40] Detailed calculations indicate that the previous such occurrence lasted only fourteen years, from July 11, 1735 to September 15, 1749, whereas between April 30, 1483 and July 23, 1503, it had also lasted 20 years. The durations of the relationship varies because of the varying speed of motion of Neptune along its orbit; the relationship between the orbits themselves varies much mure slowly, as Neptune's orbit precesses and otherwise evolves.

Although this repeating pattern may suggest a regular structure, in the long term Pluto's orbit is in fact chaotic. While computer simulations can be used to predict its position for several million years (both forward and backward in time), after intervals longer than the Lyapunov time of 10–20 million years, calculations become speculative: Pluto's tiny size makes it sensitive to unmeasurably small details of the solar system, hard-to-predict factors that will gradually disrupt its orbit.[41][42] Millions of years from now, Pluto may well be at aphelion, at perihelion or anywhere in between, with no way for us to predict which. This does not mean Pluto's orbit itself is unstable, but its position on that orbit is impossible to determine so far ahead. Several resonances and other dynamical effects keep Pluto's orbit stable, safe from planetary collision or scattering.
Relationship with Neptune [değiştir]

Orbit of Pluto—polar view. This 'view from above' shows how Pluto's orbit (in red) is less circular than Neptune's (in blue), and how Pluto is sometimes closer to the Sun than Neptune. The darker halves of both orbits show where they pass below the plane of the ecliptic.

Despite Pluto's orbit appearing to cross that of Neptune when viewed from directly above, the two objects' orbits are aligned so that they can never collide or even approach closely. There are several reasons why.

At the simplest level, one can examine the two orbits and see that they do not intersect. When Pluto is closest to the Sun, and hence closest to Neptune's orbit as viewed from above, it is also the farthest above Neptune's path. Pluto's orbit passes about 8 AU above that of Neptune, preventing a collision.[43][44][45] Pluto's ascending and descending nodes, the points at which its orbit crosses the ecliptic, are currently separated from Neptune's by over 21°.[46]

However, this alone is not enough to protect Pluto; perturbations from the planets (especially Neptune) could alter aspects of Pluto's orbit (such as its orbital precession) over millions of years so that a collision could be possible. Some other mechanism or mechanisms must therefore be at work. The most significant of these is that Pluto lies in the 3:2 mean motion resonance with Neptune: for every three of Neptune's orbits around the Sun, Pluto makes two. The two objects then return to their initial positions and the cycle repeats, each cycle lasting about 500 years. This pattern is configured so that, in each 500-year cycle, the first time Pluto is near perihelion Neptune is over 50° behind Pluto. By Pluto's second perihelion, Neptune will have completed a further one and a half of its own orbits, and so will be a similar distance ahead of Pluto. Pluto and Neptune's minimum separation is over 17 AU. Pluto comes closer to Uranus (11 AU) than it does to Neptune.[45]

The 3:2 resonance between the two bodies is highly stable, and is preserved over millions of years.[47] This prevents their orbits from changing relative to one another; the cycle always repeats in the same way, and so the two bodies can never pass near to each other. Thus, even if Pluto's orbit were not highly inclined the two bodies could never collide.[45]
Other factors [değiştir]

Numerical studies have shown that over periods of millions of years, the general nature of the alignment between Pluto and Neptune's orbits does not change.[43][48] However, there are several other resonances and interactions that govern the details of their relative motion, and enhance Pluto's stability. These arise principally from two additional mechanisms (besides the 3:2 mean motion resonance).

First, Pluto's argument of perihelion, the angle between the point where it crosses the ecliptic and the point where it is closest to the Sun, librates around 90°.[48] This means that when Pluto is nearest the Sun, it is at its farthest above the plane of the Solar System, preventing encounters with Neptune. This is a direct consequence of the Kozai mechanism,[43] which relates the eccentricity of an orbit to its inclination to a larger perturbing body—in this case Neptune. Relative to Neptune, the amplitude of libration is 38°, and so the angular separation of Pluto's perihelion to the orbit of Neptune is always greater than 52° (= 90°–38°). The closest such angular separation occurs every 10,000 years.[47]

Second, the longitudes of ascending nodes of the two bodies—the points where they cross the ecliptic—are in near-resonance with the above libration. When the two longitudes are the same—that is, when one could draw a straight line through both nodes and the Sun—Pluto's perihelion lies exactly at 90°, and it comes closest to the Sun at its peak above Neptune's orbit. In other words, when Pluto most closely intersects the plane of Neptune's orbit, it must be at its farthest beyond it. This is known as the 1:1 superresonance, and is controlled by all the Jovian planets.[43]

To understand the nature of the libration, imagine a polar point of view, looking down on the ecliptic from a distant vantage point where the planets orbit counter-clockwise. After passing the ascending node, Pluto is interior to Neptune's orbit and moving faster, approaching Neptune from behind. The strong gravitational pull between the two causes angular momentum to be transferred to Pluto, at Neptune's expense. This moves Pluto into a slightly larger orbit, where it travels slightly slower, according to Kepler's third law. As its orbit changes, this has the gradual effect of changing the pericentre and longitudes of Pluto (and, to a lesser degree, of Neptune). After many such repetitions, Pluto is sufficiently slowed, and Neptune sufficiently speeded up, that Neptune begins to catch Pluto at the opposite side of its orbit (near the opposing node to where we began). The process is then reversed, and Pluto loses angular momentum to Neptune, until Pluto is sufficiently speeded up that it begins to catch Neptune again at the original node. The whole process takes about 20,000 years to complete.[45][47]
Rotation [değiştir]

Pluto's rotation period, its day, is equal to 6.39 Earth days.[49] Like Uranus, Pluto rotates on its "side" on its orbital plane, with an axial tilt of 120°, and so its seasonal variation is extreme; at its solstices, one hemisphere is in permanent daylight, while the other is in permanent darkness.[50]
Physical characteristics [değiştir]

Hubble map of Pluto's surface, showing great variations in color and albedo

Three views of Pluto from different orientations

Pluto's distance from Earth makes in-depth investigation difficult. Many details about Pluto will remain unknown until 2015, when the New Horizons spacecraft is expected to arrive there.[51]
Appearance and surface [değiştir]

Pluto's visual apparent magnitude averages 15.1, brightening to 13.65 at perihelion.[52] To see it, a telescope is required; around 30 cm (12 in) aperture being desirable.[53] It looks star-like and without a visible disk even in large telescopes, because its angular diameter is only 0.11". Distance, and current limits on telescope technology, make it impossible to directly photograph surface details on Pluto.

The earliest maps of Pluto, made in the late 1980s, were brightness maps created from close observations of eclipses by its largest moon, Charon. Observations were made of the change in the total average brightness of the Pluto-Charon system during the eclipses. For example, eclipsing a bright spot on Pluto makes a bigger total brightness change than eclipsing a dark spot. Computer processing of many such observations can be used to create a brightness map. This method can also track changes in brightness over time.[54][55]

Current maps have been produced from images from the Hubble Space Telescope, which offers the highest resolution currently available, and show considerably more detail,[56] resolving variations several hundred kilometres across, including polar regions and large bright spots.[57] The maps are produced by complex computer processing, which find the best-fit projected maps for the few pixels of the Hubble images.[58] As the two cameras on the HST used for these maps are no longer in service, these will remain the most detailed maps of Pluto until the 2015 flyby of New Horizons.[58]

These maps, together with Pluto's lightcurve and the periodic variations in its infrared spectra, reveal that Pluto's surface is remarkably varied, with large changes in both brightness and colour.[59] Pluto is one of the most contrastive bodies in the Solar System, with as much contrast as Saturn's moon Iapetus.[56] The colour varies between charcoal black, dark orange and white:[60] Buie et al. term it "significantly less red than Mars and much more similar to the hues seen on Io with a slightly more orange cast".[57]

Pluto's surface has changed between 1994 and 2002-3: the northern polar region has brightened and the southern hemisphere darkened.[60] Pluto's overall redness has also increased substantially between 2000 and 2002.[60] These rapid changes are probably related to seasonal variation, which is expected to be complex due to Pluto's extreme axial tilt and high orbital eccentricity.[60]

Spectroscopic analysis of Pluto's surface reveals it to be composed of more than 98 percent nitrogen ice, with traces of methane and carbon monoxide.[61] The face of Pluto oriented toward Charon contains more methane ice, while the opposite face contains more nitrogen and carbon monoxide ice.[62]
Structure [değiştir]

Theoretical structure of Pluto (2006)[63]
1. Frozen nitrogen [61]
2. Water ice
3. Rock

Observations by the Hubble Space Telescope place Pluto's density at between 1.8 and 2.1 g/cm3, suggesting its internal composition consists of roughly 50–70 percent rock and 30–50 percent ice by mass.[64] Because decay of radioactive minerals would eventually heat the ices enough for the rock to separate from them, scientists expect that Pluto's internal structure is differentiated, with the rocky material having settled into a dense core surrounded by a mantle of ice. The diameter of the core should be around 1,700 km, 70% of Pluto's diameter.[63] It is possible that such heating continues today, creating a subsurface ocean layer of liquid water some 100 to 180 km thick at the core–mantle boundary.[63][65] The DLR Institute of Planetary Research calculated that Pluto's density-to-radius ratio lies in a transition zone, along with Neptune's moon Triton, between icy satellites like the mid-sized moons of Uranus and Saturn, and rocky satellites such as Jupiter's Europa.[66]
Mass and size [değiştir]
Dosyaluto, Earth size comparison.jpg
Pluto's volume is about 0.6% that of Earth

Pluto's mass is 1.31×1022 kg, less than 0.24 percent that of the Earth,[67] while its diameter is 2,306 (+/- 20) km, or roughly 66% that of the Moon.[68] Pluto's atmosphere complicates determining its true solid size within a certain margin.[69]

Astronomers, assuming Pluto to be Lowell's Planet X, initially calculated its mass based on its presumed effect on Neptune and Uranus. In 1955 Pluto was calculated to be roughly the mass of the Earth, with further calculations in 1971 bringing the mass down to roughly that of Mars.[70] However, in 1976, Dale Cruikshank, Carl Pilcher and David Morrison of the University of Hawaii calculated Pluto's albedo for the first time, finding that it matched that for methane ice; this meant Pluto had to be exceptionally luminous for its size and therefore could not be more than 1 percent the mass of the Earth.[70] Pluto's albedo is 1.3–2.0 times greater than that of Earth.[52]
Radius estimates for Pluto:Year Radius Notes
1993 1180 km Millis, et al.[71]
(no haze)[72]
1994 1164 km Young & Binzel [73]
2006 1153 km Buie, et al.[68]
2007 1161 km Young, Young, & Buie [69]


The discovery of Pluto's satellite Charon in 1978 enabled a determination of the mass of the Pluto–Charon system by application of Newton's formulation of Kepler's third law. Once Charon's gravitational effect was measured, Pluto's true mass could be determined. Observations of Pluto in occultation with Charon allowed scientists to establish Pluto's diameter more accurately, while the invention of adaptive optics allowed them to determine its shape more accurately.[74]

Among the objects of the Solar System, Pluto is much less massive than the terrestrial planets, and at less than 0.2 lunar masses, it is also less massive than seven moons: Ganymede, Titan, Callisto, Io, Earth's Moon, Europa and Triton.
Diameter [değiştir]

Pluto is more than twice the diameter and a dozen times the mass of the dwarf planet Ceres, the largest object in the asteroid belt. However, it is less massive than the dwarf planet Eris, a trans-Neptunian object discovered in 2005. Given the error bars in the different size estimates, it is currently unknown whether Eris or Pluto has the larger diameter.[72] Both Pluto and Eris are estimated to have solid-body diameters of about 2330 km.[72] Determinations of Pluto's size are complicated by its atmosphere, and possible hydrocarbon haze.[72]
Atmosphere [değiştir]

CRIRES model-based computer-generated impression of the Plutonian surface by ESO—L. Calçada, with atmospheric haze, and Charon and the Sun in the sky.

Pluto's atmosphere consists of a thin envelope of nitrogen, methane, and carbon monoxide gases, which are derived from the ices of these substances on its surface.[75] Its surface pressure ranges from 6.5 to 24 μbar.[76] Pluto's elongated orbit is predicted to have a major effect on its atmosphere: as Pluto moves away from the Sun, its atmosphere should gradually freeze out, and fall to the ground. When Pluto is closer to the Sun, the temperature of Pluto's solid surface increases, causing the ices to sublimate into gas. This creates an anti-greenhouse effect; much as sweat cools the body as it evaporates from the surface of the skin, this sublimation cools the surface of Pluto. Scientists using the Submillimeter Array have recently discovered that Pluto's temperature is about 43 K (−−-230 °C), 10 K colder than would otherwise be expected.[77]

The presence of methane, a powerful greenhouse gas, in Pluto's atmosphere creates a temperature inversion, with average temperatures 36 K warmer 10 km above the surface.[78] The lower atmosphere contains a higher concentration of methane than its upper atmosphere.[78]

The first evidence of Pluto's atmosphere was found by the Kuiper Airborne Observatory in 1985, from observations of the occultation of a star behind Pluto. When an object with no atmosphere moves in front of a star, the star abruptly disappears; in the case of Pluto, the star dimmed out gradually.[79] From the rate of dimming, the atmospheric pressure was determined to be 0.15 pascal, roughly 1/700,000 that of Earth.[80] The conclusion was confirmed and significantly strengthened by extensive observations of another similar occultation in 1988.

In 2002, another occultation of a star by Pluto was observed and analysed by teams led by Bruno Sicardy of the Paris Observatory,[81] James L. Elliot of MIT,[82] and Jay Pasachoff of Williams College.[83] Surprisingly, the atmospheric pressure was estimated to be 0.3 pascal, even though Pluto was farther from the Sun than in 1988 and thus should have been colder and had a more rarefied atmosphere. One explanation for the discrepancy is that in 1987 the south pole of Pluto came out of shadow for the first time in 120 years, causing extra nitrogen to sublimate from the polar cap. It will take decades for the excess nitrogen to condense out of the atmosphere as it freezes onto the north pole's now permanently dark ice cap.[84] Spikes in the data from the same study revealed what may be the first evidence of wind in Pluto's atmosphere.[84] Another stellar occultation was observed by the MIT-Williams College team of James Elliot, Jay Pasachoff, and a Southwest Research Institute team led by Leslie Young on June 12, 2006 from sites in Australia.[85]

In October 2006, Dale Cruikshank of NASA/Ames Research Center (a New Horizons co-investigator) and his colleagues announced the spectroscopic discovery of ethane on Pluto's surface. This ethane is produced from the photolysis or radiolysis (i.e., the chemical conversion driven by sunlight and charged particles) of frozen methane on Pluto's surface and suspended in its atmosphere.[86]
Satellites [değiştir]

Pluto and its three known moons
Ana madde: Moons of Pluto

Pluto has three known natural satellites: Charon, first identified in 1978 by astronomer James Christy; and two smaller moons, Nix and Hydra, both discovered in 2005.[87]

The Plutonian moons are unusually close to Pluto, compared to other observed systems. Moons could potentially orbit Pluto up to 53% (or 69%, if retrograde) of the Hill sphere radius, the stable gravitational zone of Pluto's influence. For example, Psamathe orbits Neptune at 40% of the Hill radius. In the case of Pluto, only the inner 3% of the zone is known to be occupied by satellites. In the discoverers` terms, the Plutonian system appears to be "highly compact and largely empty",[88] although others have pointed out the possibility of additional objects, including a small ring system.[89]
Charon [değiştir]

A 1990 photograph of Pluto and Charon by the Hubble Telescope
Ana madde: Charon (moon)

The Pluto-Charon system is noteworthy for being the largest of the Solar System's few binary systems, defined as those whose barycentre lies above the primary's surface (617 Patroclus is a smaller example).[90] This and the large size of Charon relative to Pluto has led some astronomers to call it a dwarf double planet.[91] The system is also unusual among planetary systems in that each is tidally locked to the other: Charon always presents the same face to Pluto, and Pluto always presents the same face to Charon: from any position on either body, the other is always at the same position in the sky, or always obscured.[92] Because of this, the rotation period of each is equal to the time it takes the entire system to rotate around its common centre of gravity.[49] Just as Pluto revolves on its side relative to the orbital plane, so the Pluto-Charon system does also.[50] In 2007, observations by the Gemini Observatory of patches of ammonia hydrates and water crystals on the surface of Charon suggested the presence of active cryo-geysers.[93]
Nix and Hydra [değiştir]

Pluto and Charon as taken with the ESA/Dornier Faint Object Camera on Hubble Space Telescope in 1994

Diagram of the Plutonian system. P 1 is Hydra, and P 2 is Nix.
Ana maddeler: Nix (moon) ve Hydra (moon)

Two additional moons of Pluto were imaged by astronomers working with the Hubble Space Telescope on May 15, 2005, and received provisional designations of S/2005 P 1 and S/2005 P 2. The International Astronomical Union officially named Pluto's newest moons Nix (or Pluto II, the inner of the two moons, formerly P 2) and Hydra (Pluto III, the outer moon, formerly P 1), on June 21, 2006.[94]

These small moons orbit Pluto at approximately two and three times the distance of Charon: Nix at 48,700 kilometres and Hydra at 64,800 kilometres from the barycenter of the system. They have nearly circular prograde orbits in the same orbital plane as Charon, and are very close to (but not in) 4:1 and 6:1 mean motion orbital resonances with Charon.[95]

Observations of Nix and Hydra to determine individual characteristics are ongoing. Hydra is sometimes brighter than Nix, suggesting either that it is larger or that different parts of its surface may vary in brightness. Sizes are estimated from albedos. The moons' spectral similarity to Charon suggests a 35% albedo similar to Charon's; this value results in diameter estimates of 46 kilometres for Nix and 61 kilometres for the brighter Hydra. Upper limits on their diameters can be estimated by assuming the 4% albedo of the darkest Kuiper Belt objects; these bounds are 137 ± 11 km and 167 ± 10 km, respectively. At the larger end of this range, the inferred masses are less than 0.3% that of Charon, or 0.03% of Pluto's.[96]

The discovery of the two small moons suggests that Pluto may possess a variable ring system. Small body impacts can create debris that can form into planetary rings. Data from a deep optical survey by the Advanced Camera for Surveys on the Hubble Space Telescope suggest that no ring system is present. If such a system exists, it is either tenuous like the rings of Jupiter or is tightly confined to less than 1,000 km in width.[89]

Similar conclusions have been made from occultation studies.[97] In imaging the Plutonian system, observations from Hubble placed limits on any additional moons. With 90% confidence, no additional moons larger than 12 km (or a maximum of 37 km with an albedo of 0.041) exist beyond the glare of Pluto 5 arcseconds from the dwarf planet. This assumes a Charon-like albedo of 0.38; at a 50% confidence level the limit is 8 kilometres.[98]
Pluto's satellites, with Earth's Moon comparison[68]Name

(Pronunciation) Discovery
Year Diameter
(km) Mass
(kg) Orbital radius (km)
(barycentric) Orbital period (d)
Pluto /ˈpluːtoʊ/ 1930 2,306
(66% Moon) 13,050 ×1018
(18% Moon) 2,040
(0.6% Moon)
Charon /ˈʃærən/,
/ˈkɛərən/ 1978 1,205
(35% Moon) 1,520 ×1018
(2% Moon) 17,530
(5% Moon) 6.3872
(25% Moon)
Nix /ˈnɪks/ 2005 91 4 ×1017 48,708 24.856
Hydra /ˈhaɪdrə/ 2005 114 8 ×1017 64,749 38.206


Mass of Nix and Hydra assumes icy/porous density of 1.0 g/cm3
Origins [değiştir]
Ana maddeler: Kuiper belt ve Nice model

Plot of known Kuiper belt objects, set against the four gas giants

Pluto's origin and identity had long puzzled astronomers. One early hypothesis was that Pluto was an escaped moon of Neptune, knocked out of orbit by its largest current moon, Triton. This notion has been heavily criticised because Pluto never comes near Neptune in its orbit.[99]

Pluto's true place in the Solar System began to reveal itself only in 1992, when astronomers found a population of small icy objects beyond Neptune that were similar to Pluto not only in orbit but also in size and composition. This trans-Neptunian population is believed to be the source of many short-period comets. Astronomers now believe Pluto to be the largest[note 1] member of the Kuiper belt, a somewhat stable ring of objects located between 30 and 50 AU from the Sun. Like other Kuiper belt objects (KBOs), Pluto shares features with comets; for example, the solar wind is gradually blowing Pluto's surface into space, in the manner of a comet.[100] If Pluto were placed as near to the Sun as Earth, it would develop a tail, as comets do.[101]

Though Pluto is the largest of the Kuiper belt objects discovered so far, Neptune's moon Triton, which is slightly larger than Pluto, is similar to it both geologically and atmospherically, and is believed to be a captured Kuiper belt object.[102] Eris (see below) is also larger than Pluto but is not strictly considered a member of the Kuiper belt population. Rather, it is considered a member of a linked population called the scattered disc.

A large number of Kuiper belt objects, like Pluto, possess a 3:2 orbital resonance with Neptune. KBOs with this orbital resonance are called "plutinos", after Pluto.[103]

Like other members of the Kuiper belt, Pluto is thought to be a residual planetesimal; a component of the original protoplanetary disc around the Sun that failed to fully coalesce into a full-fledged planet. Most astronomers agree that Pluto owes its current position to a sudden migration undergone by Neptune early in the Solar System's formation. As Neptune migrated outward, it approached the objects in the proto-Kuiper belt, setting one in orbit around itself, which became its moon Triton, locking others into resonances and knocking others into chaotic orbits. The objects in the scattered disc, a dynamically unstable region beyond the Kuiper belt, are believed to have been placed in their current positions by interactions with Neptune's migrating resonances.[104] A 2004 computer model by Alessandro Morbidelli of the Observatoire de la Côte d'Azur in Nice suggested that the migration of Neptune into the Kuiper belt may have been triggered by the formation of a 1:2 resonance between Jupiter and Saturn, which created a gravitational push that propelled both Uranus and Neptune into higher orbits and caused them to switch places, ultimately doubling Neptune's distance from the Sun. The resultant expulsion of objects from the proto-Kuiper belt could also explain the Late Heavy Bombardment 600 million years after the Solar System's formation and the origin of Jupiter's trojan asteroids.[105] It is possible that Pluto had a near-circular orbit about 33 AU from the Sun before Neptune's migration perturbed it into a resonant capture.[106] The Nice model requires that there were about a thousand Pluto-sized bodies in the original planetesimal disk; these may have included the bodies which became Triton and Eris.[105]
Exploration [değiştir]
Ana madde: New Horizons
Dosya:New Horizons Jan19 06.jpg
New Horizons, launched on January 19, 2006

Pluto presents significant challenges for spacecraft because of its small mass and great distance from Earth. Voyager 1 could have visited Pluto, but controllers opted instead for a close flyby of Saturn's moon Titan, resulting in a trajectory incompatible with a Pluto flyby. Voyager 2 never had a plausible trajectory for reaching Pluto.[107] No serious attempt to explore Pluto by spacecraft occurred until the last decade of the 20th century. In August 1992, JPL scientist Robert Staehle telephoned Pluto's discoverer, Clyde Tombaugh, requesting permission to visit his planet. "I told him he was welcome to it," Tombaugh later remembered, "though he's got to go one long, cold trip."[108] Despite this early momentum, in 2000, NASA cancelled the Pluto Kuiper Express mission, citing increasing costs and launch vehicle delays.[109]

First Pluto sighting from New Horizons

After an intense political battle, a revised mission to Pluto, dubbed New Horizons, was granted funding from the US government in 2003.[110] New Horizons was launched successfully on January 19, 2006. The mission leader, S. Alan Stern, confirmed that some of the ashes of Clyde Tombaugh, who died in 1997, had been placed aboard the spacecraft.[111]

In early 2007 the craft made use of a gravity assist from Jupiter. Its closest approach to Pluto will be on July 14, 2015; scientific observations of Pluto will begin 5 months before closest approach and will continue for at least a month after the encounter. New Horizons captured its first (distant) images of Pluto in late September 2006, during a test of the Long Range Reconnaissance Imager (LORRI).[112] The images, taken from a distance of approximately 4.2 billion kilometres, confirm the spacecraft's ability to track distant targets, critical for maneuvering toward Pluto and other Kuiper Belt objects.

New Horizons will use a remote sensing package that includes imaging instruments and a radio science investigation tool, as well as spectroscopic and other experiments, to characterise the global geology and morphology of Pluto and its moon Charon, map their surface composition and analyse Pluto's neutral atmosphere and its escape rate. New Horizons will also photograph the surfaces of Pluto and Charon.

Discovery of moons Nix and Hydra may present unforeseen challenges for the probe. Debris from collisions between Kuiper belt objects and the smaller moons, with their relatively low escape velocities, may produce a tenuous dusty ring. Were New Horizons to fly through such a ring system, there would be an increased potential for Şablonp damage that could disable the probe.[89]

 

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