Lista obiektów w Układzie Słonecznym ze względu na promień

Lista obiektów w Układzie Słonecznym ze względu na promień, od największego do najmniejszego. Lista nie jest kompletna; zawiera Słońce, planety, wiele naturalnych satelitów i wiele innych ciał wartych odnotowania.

Lista obiektów w Układzie Słonecznym ze względu na masę i ta lista różnią się kolejnością ciał, gdyż niektóre ciała różnią się między sobą gęstością. Na przykład Uran jest większy od Neptuna, ale jest lżejszy, natomiast Ganimedes i Tytan są większe od Merkurego, lecz ich masa jest około dwa razy mniejsza.

Wiele niedawno odkrytych obiektów transneptunowych nie ma dokładnie wyznaczonych rozmiarów, a podane rozmiary są jedynie oszacowaniami[1].

Lista obiektów według długości promienia

Powyżej 400 km

#CiałoZdjęciePromieńObjętośćMasaGęstość
g/cm³
GrawitacjaRodzaj
kmR109 km³V1021 kgMm/s2
1SłońceSun920607.jpg696 342 ±65109,31 414 300 0001 305 7001 988 550 000333 0001,408274,027,94gwiazda
2JowiszJupiter.jpg69 911 ±610,971 431 2801 3211 898 600317,831,32624,792,528planeta (gazowy olbrzym)
3SaturnSaturn-cassini-March-27-2004.jpg58 232 ±69,14827 130764568 46095,1620,68710,4451,065planeta (gazowy olbrzym)
4UranUranus.jpg25 362 ±73,98168 34063,186 83214,5361,278,870,9planeta (gazowy olbrzym)
5NeptunNeptune.jpg24 622 ±193,86562 54057,7102 43017,1471,63811,151,137planeta (gazowy olbrzym)
6ZiemiaThe Earth seen from Apollo 17.jpg6371,0 ±0,0111 083,2115 973,615,5149,806651planeta skalista
7WenusVenus-real.jpg6051,8 ±10,9499928,430,8574 868,50,8155,2438,8720,905planeta skalista
8MarsMars Valles Marineris.jpeg3389,5 ±0,20,532163,180,151641,850,1073,9335 ± 0,00043,70,38planeta skalista
9GanimedesGanymede g1 true.jpg2634,1 ±0,30,413576,300,0704148,20,02481,9361,4280,15księżyc Jowisza
10TytanTitan in natural color Cassini.jpg2576 ±20,404371,520,0660134,50,02251,8798 ± 0,00441,3450,14księżyc Saturna
11MerkuryMercury in color - Prockter07 centered.jpg2439,7 ±10,382960,830,0562330,20,05535,4273,70,38planeta skalista
12KallistoCallisto.jpg2410,3 ±1,50,378358,650,0541107,60,0181,8344 ± 0,00341,236030,126księżyc Jowisza
13IoIo highest resolution true color.jpg1821,6 ± 0,50,285925,320,023489,30,0153,528 ± 0,0061,7970,183księżyc Jowisza
14KsiężycFull moon.jpeg1737,10,272721,9580,020373,50,01233,34641,6250,166satelita Ziemi
15EuropaEuropa-moon.jpg1560,8 ± 0,50,24515,930,0147480,0080353,013 ± 0,0051,3160,134księżyc Jowisza
16TrytonTriton Voyager 2.jpg1353,4 ±0,90,212410,380,009621,50,0035992,0610,7820,0797księżyc Neptuna
17(134340) PlutonNh-pluto-in-true-color 2x JPEG.jpg1186 ±20,1866,950,006413,1050,00221,87 ± 0,020,610,062planeta karłowata, obiekt Pasa Kuipera
18(136199) ErisEris and Dysnomia.png1163 ±60,18256,590,00616,70,00282,52 ± 0,050,6590,0672planeta karłowata, obiekt dysku rozproszonego
19TytaniaPIA00039 Titania.jpg788,4 ±0,60,12372,060,00193,5260,000591,711 ± 0,0050,3780,0385księżyc Urana
20Rea763,8 ±1,00,11991,870,00172,31660,000391,236 ± 0,0050,260,027księżyc Saturna
21OberonVoyager 2 picture of Oberon.jpg761,4 ±2,60,11951,850,00173,0140,00051,63 ± 0,050,3470,035księżyc Urana
22JapetIapetus by Voyager 2 - enhanced.jpg734,5 ±2,80,11531,550,00141,97390,000331,088 ± 0,0130,2230,0227księżyc Saturna
23(136472) MakemakeMakemake and its moon.jpg715 ± 70,1121,70,00162,3 ± 0,9planeta karłowata, obiekt Pasa Kuipera
24(225088) Gonggong2007 OR10 and its moon.png640 ± 1050,10051,09810,00101obiekt Pasa Kuipera
25(136108) HaumeaHaumea Hubble.png620 ± 300,0971,3-1,60,0014,0060,000672,550,440,045planeta karłowata, obiekt Pasa Kuipera
26CharonCharon by New Horizons on 13 July 2015.png606 ±30,09510,870,00081,520,000251,702 ± 0,0210,2790,028księżyc Plutona
27UmbrielUmbriel (moon).jpg584,7 ±2,80,09180,840,00081,20,000201,39 ± 0,160,2340,024księżyc Urana
28ArielAriel (moon).jpg578,9 ±0,60,09090,810,00071,350,0002261,66 ± 0,150,2690,027księżyc Urana
29DioneDione color south.jpg561,4 ±0,40,08810,730,00071,0960,0001831,478 ± 0,0030,2320,0237księżyc Saturna
30(50000) QuaoarQuaoar-weywot hst.jpg555 ±30,08711,4 ± 0,10,00022,2 ± 0,40,1250,0127obiekt Pasa Kuipera
31TetydaPIA18317-SaturnMoon-Tethys-Cassini-20150411.jpg531,1 ±0,60,08340,6240,00060,61730,0001030,984 ± 0,0030,1450,015księżyc Saturna
32(90377) SednaSedna PRC2004-14d.jpg500 ± 800,0785obiekt odłączony
33(1) CeresCeresintruecolor.png4730,07420,4330,00040,9390,0001572,170,290,030planeta karłowata, planetoida pasa głównego
342002 MS4307261-2002ms4 hst.jpg467 ± 240,0733obiekt Pasa Kuipera
35(90482) OrkusOrcus-vanth hst.jpg458 ±130,07192,47obiekt Pasa Kuipera
36(120347) SalaciaSalacia Hubble.png425 ± 230,6670,45 ±?1,16 ± 0,45obiekt Pasa Kuipera

400–200 km

CiałoZdjęciePromień
km
Masa
1018 kg
Gęstość
g/cm³
Rodzaj
2013 FY272013 FY27.png265-550obiekt dysku rozproszonego
2002 AW1972002AW197-Spitzer.jpg384 ± 20obiekt odłączony
2003 AZ842003AZ84 Hubble.png385obiekt Pasa Kuipera
(174567) VardaVarda-ilmare hst.jpg3582,651,25obiekt Pasa Kuipera
Dysnomia342 ± 25księżyc Eris
2004 GV92004-gv9 hst.jpg340 ± 40obiekt Pasa Kuipera
2005 RN432005-rn43 hst.jpg340 ± 400,055obiekt Pasa Kuipera
2002 UX2520131105 2002 UX25 hst.png335 ± 171,250,82obiekt Pasa Kuipera
2007 JJ43335 ± 150obiekt Pasa Kuipera
(20000) Waruna20000-varuna hst.jpg334 ± 503,70,99obiekt Pasa Kuipera
(28978) IksjonIxion planetoid nasa.jpg325 ± 120obiekt Pasa Kuipera
(229762) Gǃkúnǁʼhòmdímà2007 UK126 Hubble.png300 ± 40obiekt dysku rozproszonego
(19521) Chaos300 ± 70obiekt Pasa Kuipera
2010 KZ39~300obiekt Pasa Kuipera
2012 VP13~300obiekt dysku rozproszonego
2010 RF43293obiekt dysku rozproszonego
2005 RM432005rm43-19761117.gif~300obiekt dysku rozproszonego
2001 UR16342301-2001ur163 hst.jpg~300obiekt dysku rozproszonego
2002 TC30284522-2002tc302 hst.jpg290 ± 50obiekt Pasa Kuipera
2002 XV932002xv93-19920928.gif280 ± 10obiekt Pasa Kuipera
2003 UZ4132003uz413-19961014.gif~280obiekt Pasa Kuipera
2008 ST291~318obiekt dysku rozproszonego
2010 RE64~280obiekt dysku rozproszonego
2010 FX86~280obiekt Pasa Kuipera
2006 QH181~280obiekt dysku rozproszonego
2014 UM33~270obiekt Pasa Kuipera
2004 XR190~270obiekt dysku rozproszonego
(4) WestaVesta full mosaic.jpg262,7 ± 0,12,593,46planetoida pasa głównego
2003 VS284922-2003vs2 hst.jpg260 ± 20obiekt Pasa Kuipera
2004 TY364~260obiekt Pasa Kuipera
2010 VK201~260obiekt Pasa Kuipera
(2) PallasPotw1749a Pallas crop.png256 ± 32,11 ± 0,263,0 ± 0,5planetoida pasa głównego
2014 FT71~253obiekt Pasa Kuipera
EnceladusEnceladus from Voyager.jpg252,1 ± 0,21,081,61księżyc Saturna
2005 UQ513250 ± 40obiekt Pasa Kuipera
2003 QX113~250obiekt dysku rozproszonego
2014 FC113~250obiekt Pasa Kuipera
2002 WC19245obiekt Pasa Kuipera
(471143) Dziewanna240 ± 70obiekt dysku rozproszonego
MirandaPIA18185 Miranda's Icy Face.jpg235,8 ± 0,70,661,2księżyc Urana
2005 TB190230 ± 30obiekt odłączony
1999 DE9230 ± 20obiekt Pasa Kuipera
2003 FY128230 ± 10obiekt dysku rozproszonego
(38628) Huya229 ± 5obiekt Pasa Kuipera
2002 VR128220 ± 20obiekt Pasa Kuipera
2010 TJ~220obiekt dysku rozproszonego
2010 VZ98~220obiekt dysku rozproszonego
2011 FW62~220obiekt dysku rozproszonego
(10) HygieaSPHERE image of Hygiea.jpg215 ± 4planetoida pasa głównego
ProteuszProteus (Voyager 2).jpg210 ± 70,44~1,3księżyc Neptuna
2005 QU182210 ± 40obiekt dysku rozproszonego
2004 NT33210 ± 40obiekt Pasa Kuipera
1999 CD158~210obiekt Pasa Kuipera
2004 PF15203 ± 43obiekt Pasa Kuipera
2011 GM27~201obiekt Pasa Kuipera
1998 SN165200 ± 20obiekt Pasa Kuipera
2001 QF298200 ± 20obiekt Pasa Kuipera
2002 YW134~200obiekt dysku rozproszonego
1996 GQ21~200obiekt dysku rozproszonego

Zobacz też

Przypisy

  1. Mike Brown: How many dwarf planets are there in the outer solar system? (ang.). Caltech, 2014-01-18. [dostęp 2014-01-19].

Linki zewnętrzne

Media użyte na tej stronie

Solar System XXX.png
This is a revised version of Solar_System_XXIX.png.
Saturn PIA06077.jpg
Saturn Cassini-Huygens (NASA)

Instrument: Imaging Science Subsystem - Narrow Angle

Saturn's peaceful beauty invites the Cassini spacecraft for a closer look in this natural color view, taken during the spacecraft's approach to the planet. By this point in the approach sequence, Saturn was large enough that two narrow angle camera images were required to capture an end-to-end view of the planet, its delicate rings and several of its icy moons. The composite is made entire from these two images.

Moons visible in this mosaic: Epimetheus (116 kilometers, 72 miles across), Pandora (84 kilometers, 52 miles across) and Mimas (398 kilometers, 247 miles across) at left of Saturn; Prometheus (102 kilometers, 63 miles across), Janus (181 kilometers, 113 miles across) and Enceladus (499 kilometers, 310 miles across) at right of Saturn.

The images were taken on May 7, 2004 from a distance of 28.2 million kilometers (17.6 million miles) from Saturn. The image scale is 169 kilometers (105 miles) per pixel. Moons in the image have been brightened for visibility.

The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Cassini-Huygens mission for NASA's Office of Space Science, Washington, D.C. The Cassini orbiter and its two onboard cameras, were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo.

For more information, about the Cassini-Huygens mission visit, http://saturn.jpl.nasa.gov and the Cassini imaging team home page, http://ciclops.org.
Salacia Hubble.png
Autor: Renerpho, Licencja: CC BY-SA 4.0
Salacia and its moon Actaea, imaged by the Hubble Space Telescope on 21 July 2006.
225088 Gonggong and Xiangliu by Hubble (2010).png
225088 Gonggong (2007 OR10) with its moon. It was the largest unnamed Solar System and Kuiper Belt object before official naming on 5 February 2020.
Makemake and its moon.jpg
(c) ESA/Hubble, CC BY 4.0
This Hubble Space Telescope image reveals the first moon ever discovered around the dwarf planet Makemake. The tiny moon, located just above Makemake in this image, is barely visible because it is almost lost in the glare of the very bright dwarf planet. The moon, nicknamed MK 2, is roughly 160 kilometres wide and orbits about 21,000 kilometres from Makemake. Makemake is 1,300 times brighter than its moon and is also much larger, at 2,200 kilometres across.

The Makemake system is more than 50 times farther than the Earth is from the Sun. The pair resides on the outskirts of our solar system in the Kuiper Belt, a vast region of frozen debris from the construction of our solar system 4.5 billion years ago.

Previous searches for a moon around Makemake turned up empty. The moon may be in an edge-on orbit, so part of the time it gets lost in the bright glare of Makemake.

Hubble's sharp-eyed Wide Field Camera 3 made the observation in April 2015.
Ganymede g1 true.jpg
True color image of Ganymede, obtained by the Galileo spacecraft, with enhanced contrast.

Here is the description from JPL's web entry for PIA00716:

Natural color view of Ganymede from the Galileo spacecraft during its first encounter with the satellite. North is to the top of the picture and the sun illuminates the surface from the right. The dark areas are the older, more heavily cratered regions and the light areas are younger, tectonically deformed regions. The brownish-gray color is due to mixtures of rocky materials and ice. Bright spots are geologically recent impact craters and their ejecta. The finest details that can be discerned in this picture are about 13.4 kilometers across. The images which combine for this color image were taken beginning at Universal Time 8:46:04 UT on June 26, 1996.

The Jet Propulsion Laboratory, Pasadena, CA manages the mission for NASA's Office of Space Science, Washington, DC. This image and other images and data received from Galileo are posted on the World Wide Web, on the Galileo mission home page at URL http://galileo.jpl.nasa.gov. Background information and educational context for the images can be found at http://www.jpl.nasa.gov/galileo/sepo.
2004-gv9 hst.jpg
Hubble Space Telescope image of the cubewano (90568) 2004 GV9, taken on 17 March 2010.
Titan in natural color Cassini.jpg
This natural color composite was taken during the Cassini spacecraft's April 16, 2005, flyby of Titan. It is a combination of images taken through three filters that are sensitive to red, green and violet light. It shows approximately what Titan would look like to the human eye: a hazy orange globe surrounded by a tenuous, bluish haze. The orange color is due to the hydrocarbon particles which make up Titan's atmospheric haze. This obscuring haze was particularly frustrating for planetary scientists following the NASA Voyager mission encounters in 1980-81. Fortunately, Cassini is able to pierce Titan's veil at infrared wavelengths (see PIA06228). North on Titan is up and tilted 30 degrees to the right. The images to create this composite were taken with the Cassini spacecraft wide angle camera on April 16, 2005, at distances ranging from approximately 173,000 to 168,200 kilometers (107,500 to 104,500 miles) from Titan and from a Sun-Titan-spacecraft, or phase, angle of 56 degrees. Resolution in the images is approximately 10 kilometers per pixel. The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington, D.C. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo. For more information about the Cassini-Huygens mission, visit http://saturn.jpl.nasa.gov and the Cassini imaging team home page, http://ciclops.org.
2007 UK126 Hubble.png
Autor: Renerpho, Licencja: CC BY-SA 4.0
Hubble image of (229762) 2007 UK126 and its satellite, taken on 2 January 2018.
From Hubble images idid01m4q, idid01m5q, idid01m6q, idid01m7q, idid01m8q, idid01m9q, idid01maq and idid01mbq (in public domain since 2 July 2018). Credit: NASA.
84522-2002tc302 hst.jpg
Hubble Space Telescope image of the trans-Neptunian object (84522) 2002 TC302, taken on 16 September 2005.
Mars Valles Marineris.jpeg
Global mosaic of 102 Viking 1 Orbiter images of Mars taken on orbit 1,334, 22 February 1980. The images are projected into point perspective, representing what a viewer would see from a spacecraft at an altitude of 2,500 km. At center is Valles Marineris, over 3000 km long and up to 8 km deep. Note the channels running up (north) from the central and eastern portions of Valles Marineris to the area at upper right, Chryse Planitia. At left are the three Tharsis Montes and to the south is ancient, heavily impacted terrain. (Viking 1 Orbiter, MG07S078-334SP)
Some of the features in this mosaic are annotated in Wikimedia Commons.
Triton Voyager 2.jpg
Image of Triton, a moon of Neptune, taken by Voyager 2 at a distance of 4 million kilometers (2.5 million miles) at 4 a.m. EDT on August 22, 1989
Sedna PRC2004-14d.jpg
Image of Sedna, taken by Hubble Space Telescope
Saturn-cassini-March-27-2004.jpg
Saturn Cassini-Huygens (NASA)

Instrument: Imaging Science Subsystem - Narrow Angle

Saturn's peaceful beauty invites the Cassini spacecraft for a closer look in this natural color view, taken during the spacecraft's approach to the planet. By this point in the approach sequence, Saturn was large enough that two narrow angle camera images were required to capture an end-to-end view of the planet, its delicate rings and several of its icy moons. The composite is made entire from these two images.

Moons visible in this mosaic: Epimetheus (116 kilometers, 72 miles across), Pandora (84 kilometers, 52 miles across) and Mimas (398 kilometers, 247 miles across) at left of Saturn; Prometheus (102 kilometers, 63 miles across), Janus (181 kilometers, 113 miles across) and Enceladus (499 kilometers, 310 miles across) at right of Saturn.

The images were taken on May 7, 2004 from a distance of 28.2 million kilometers (17.6 million miles) from Saturn. The image scale is 169 kilometers (105 miles) per pixel. Moons in the image have been brightened for visibility.

The Cassini-Huygens mission is a cooperative project of NASA, the European Space Agency and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the Cassini-Huygens mission for NASA's Office of Space Science, Washington, D.C. The Cassini orbiter and its two onboard cameras, were designed, developed and assembled at JPL. The imaging team is based at the Space Science Institute, Boulder, Colo.

For more information, about the Cassini-Huygens mission visit, http://saturn.jpl.nasa.gov and the Cassini imaging team home page, http://ciclops.org.
Dione color south.jpg
Approximately natural-color view of Dione taken by Cassini on June 7, 2005. Narrow-angle red and blue frames were combined to produce the composite. The distance at the time was about 237 000 km, the phase angle was 39°. Cassini was below the ring plane, so the view principally shows Dione's south pole. Note the huge, degraded impact basin at 5 o'clock position, near Dione's south pole. North is at the 12 o'clock position, but it's on the far side, so not visible here. Wispy terrain on the trailing hemisphere is visible at upper left.
2005rm43-19761117.gif
Autor: Siding Spring Observatory/Digitized Sky Survey/California Institute of Technology, Licencja: CC BY 2.0
60-minute exposure image of 2005 RM43 taken by the Siding Spring Observatory in 17 November 1976. DSS precovery images are from DSS plate archive scans by the California Institute of Technology.
Io highest resolution true color.jpg
Wysokiej rozdzielczości fotografia Io, księżyca Jowisza, wykonana 3 lipca 1999 roku przez sondę Galileo podczas jej najbliższego przelotu koło Io od momentu wejścia sondy na orbitę Jowisza pod koniec 1995 roku.
42301-2001ur163 hst.jpg
Hubble Space Telescope image of the trans-Neptunian object (42301) 2001 UR163, taken on 26 August 2005.
Enceladus from Voyager.jpg
This color Voyager 2 image mosaic shows the water-ice-covered surface of Enceladus, one of Saturn's icy moons. Enceladus' diameter of just 500 km would fit across the state of Arizona, yet despite its small size Enceladus exhibits one of the most interesting surfaces of all the icy satellites. Enceladus reflects about 90% of the incident sunlight (about like fresh-fallen snow), placing it among the most reflective objects in the Solar System. Several geologic terrains have superposed crater densities that span a factor of at least 500, thereby indicating huge differences in the ages of these terrains. It is possible that the high reflectivity of Enceladus' surface results from continuous deposition of icy particles from Saturn's E-ring, which in fact may originate from icy volcanoes on Enceladus' surface. Some terrains are dominated by sinuous mountain ridges from 1 to 2 km high (3300 to 6600 feet), whereas other terrains are scarred by linear cracks, some of which show evidence for possible sideways fault motion such as that of California's infamous San Andreas fault. Some terrains appear to have formed by separation of icy plates along cracks, and other terrains are exceedingly smooth at the resolution of this image. The implication carried by Enceladus' surface is that this tiny ice ball has been geologically active and perhaps partially liquid in its interior for much of its history. The heat engine that powers geologic activity here is thought to be elastic deformation caused by tides induced by Enceladus' orbital motion around Saturn and the motion of another moon, Dione.
PIA18185 Miranda's Icy Face.jpg
Uranus' icy moon Miranda is seen in this image from Voyager 2 on January 24, 1986. The Voyager project is managed for NASA by the Jet Propulsion Laboratory.
Sun920607.jpg
The Sun with some sunspots visible. The two small spots in the middle have about the same diameter as our planet Earth.
2005-rn43 hst.jpg
Hubble Space Telescope image of the cubewano 2005 RN43, taken on 25 April 2010.
84922-2003vs2 hst.jpg
Hubble Space Telescope image of the plutino (84922) 2003 VS2, taken on 13 September 2005.
Callisto.jpg
Bright scars on a darker surface testify to a long history of impacts on Jupiter's moon Callisto in this image of Callisto from NASA's Galileo spacecraft. The picture, taken in May 2001, is the only complete global color image of Callisto obtained by Galileo, which has been orbiting Jupiter since December 1995. Of Jupiter's four largest moons, Callisto orbits farthest from the giant planet. Callisto's surface is uniformly cratered but is not uniform in color or brightness. Scientists believe the brighter areas are mainly ice and the darker areas are highly eroded, ice-poor material.
307261-2002ms4 hst.jpg
Hubble Space Telescope image of the cubewano (307261) 2002 MS4, taken on 9 April 2006.
Full moon.jpeg
A photograph of the full moon, from photojournal.jpl.nasa.gov catalog, specifically jpeg; Original Caption Released with Image: During its flight, the Galileo spacecraft returned images of the Moon. The Galileo spacecraft took these images on December 7, 1992 on its way to explore the Jupiter system in 1995-97. The distinct bright ray crater at the bottom of the image is the Tycho impact basin. The dark areas are lava rock filled impact basins: Oceanus Procellarum (on the left), Mare Imbrium (center left), Mare Serenitatis and Mare Tranquillitatis (center), and Mare Crisium (near the right edge). This picture contains images through the Violet, 756 nm, 968 nm filters. The color is 'enhanced' in the sense that the CCD camera is sensitive to near infrared wavelengths of light beyond human vision. The Galileo project is managed for NASA's Office of Space Science by the Jet Propulsion Laboratory.
Venus-real color.jpg
Venus in real colors, processed from clear and blue filtered Mariner 10 images.

Source images are in the public domain (NASA)

Images processed by Ricardo Nunes, downloaded from http://www.astrosurf.com/nunes/explor/explor_m10.htm
Voyager 2 picture of Oberon.jpg
Original Caption Released with Image: This Voyager 2 picture of Oberon is the best the spacecraft acquired of Uranus' outermost moon. The picture was taken shortly after 3:30 a.m. PST on Jan. 24, 1986, from a distance of 660,000 kilometers (410,000 miles). The color was reconstructed from images taken through the narrow-angle camera's violet, clear and green filters. The picture shows features as small as 12 km (7 mi) on the moon's surface. Clearly visible are several large impact craters in Oberon's icy surface surrounded by bright rays similar to those seen on Jupiter's moon Callisto. Quite prominent near the center of Oberon's disk is a large crater with a bright central peak and a floor partially covered with very dark material. This may be icy, carbon-rich material erupted onto the crater floor sometime after the crater formed. Another striking topographic feature is a large mountain, about 6 km (4 mi) high, peeking out on the lower left limb. The Voyager project is managed for NASA by the Jet Propulsion Laboratory.
The Earth seen from Apollo 17.jpg
"The Blue Marble" is a famous photograph of the Earth taken on December 7, 1972, by the crew of the Apollo 17 spacecraft en route to the Moon at a distance of about 29,000 kilometres (18,000 mi). It shows Africa, Antarctica, and the Arabian Peninsula.
Orcus-vanth hst.jpg
Hubble Space Telescope image of the plutino 90482 Orcus and its satellite Vanth, taken on 3 November 2006.
2003uz413-19961014.gif
Autor: Siding Spring Observatory/Digitized Sky Survey/California Institute of Technology, Licencja: CC BY 2.0
60-minute exposure precovery image of 2003 UZ413 taken by the Siding Spring Observatory on 14 October 1996. DSS precovery images are from DSS plate archive scans by the California Institute of Technology.
Uranus.jpg
This image of Uranus was compiled from images returned Jan. 17, 1986, by the narrow-angle camera of Voyager 2. The spacecraft was 9.1 million kilometers (5.7 million miles) from the planet, several days from closest approach. This picture has been processed to show Uranus as human eyes would see it from the vantage point of the spacecraft. The picture is a composite of images taken through blue, green and orange filters. The darker shadings at the upper right of the disk correspond to the day-night boundary on the planet. Beyond this boundary lies the hidden northern hemisphere of Uranus, which currently remains in total darkness as the planet rotates. The blue-green color results from the absorption of red light by methane gas in Uranus' deep, cold and remarkably clear atmosphere.
Umbriel (moon).jpg
Original Caption Released with Image: The southern hemisphere of Umbriel displays heavy cratering in this Voyager 2 image, taken Jan. 24, 1986, from a distance of 557,000 kilometers (346,000 miles). This frame, taken through the clear-filter of Voyager's narrow-angle camera, is the most detailed image of Umbriel, with a resolution of about 10 km (6 mi). Umbriel is the darkest of Uranus' larger moons and the one that appears to have experienced the lowest level of geological activity. It has a diameter of about 1,200 km (750 mi) and reflects only 16 percent of the light striking its surface; in the latter respect, Umbriel is similar to lunar highland areas. Umbriel is heavily cratered but lacks the numerous bright ray craters seen on the other large Uranian satellites; this results in a relatively uniform surface albedo (reflectivity). The prominent crater on the terminator (upper right) is about 110 km (70 mi) across and has a bright central peak. The strangest feature in this image (at top) is a curious bright ring, the most reflective area seen on Umbriel. The ring is about 140 km (90 miles) in diameter and lies near the satellite's equator. The nature of the ring is not known, although it might be a frost deposit, perhaps associated with an impact crater. Spots against the black background are due to 'noise' in the data. The Voyager project is managed for NASA by the Jet Propulsion Laboratory.
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Dwarf planet Eris and its moon Dysnomia.
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This is the highest-resolution picture of Titania returned by Voyager 2. The picture is a composite of two images taken Jan. 24, 1986, through the clear filter of Voyager's narrow-angle camera. At the time, the spacecraft was 369,000 kilometers (229,000 miles) from the Uranian moon; the resolution was 13 km (8 mi). Titania is the largest satellite of Uranus, with a diameter of a little more than 1,600 km (1,000 mi). Abundant impact craters of many sizes pockmark the ancient surface. The most prominent features are fault valleys that stretch across Titania. They are up to 1,500 km (nearly 1,000 mi) long and as much as 75 km (45 mi) wide. In valleys seen at right-center, the sunward-facing walls are very bright. While this is due partly to the lighting angle, the brightness also indicates the presence of a lighter material, possibly young frost deposits. An impact crater more than 200 km (125 mi) in diameter distinguishes the very bottom of the disk; the crater is cut by a younger fault valley more than 100 km (60 mi) wide. An even larger impact crater, perhaps 300 km (180 mi) across, is visible at top. The Voyager project is managed for NASA by the Jet Propulsion Laboratory.
The original NASA image has been altered by cropping, doubling the linear pixel density, sharpening and enhancing contrast.
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28978 Ixion. Ixion is shown by the yellow arrow in the center of the image. Courtesy of NASA
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Autor: Renerpho, Licencja: CC BY-SA 4.0
2013 FY27 and its satellite, imaged by the Hubble Space Telescope on January 15, 2018
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Autor: ESO/P. Vernazza et al./MISTRAL algorithm (ONERA/CNRS), Licencja: CC BY 4.0
A new SPHERE/VLT image of Hygiea, which could be the Solar System’s smallest dwarf planet yet. As an object in the main asteroid belt, Hygiea satisfies right away three of the four requirements to be classified as a dwarf planet: it orbits around the Sun, it is not a moon and, unlike a planet, it has not cleared the neighbourhood around its orbit. The final requirement is that it have enough mass that its own gravity pulls it into a roughly spherical shape. This is what VLT observations have now revealed about Hygiea. Credit: ESO/P. Vernazza et al./MISTRAL algorithm (ONERA/CNRS)
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Original Caption Released with Image: This processed color image of Jupiter was produced in 1990 by the U.S. Geological Survey from a Voyager image captured in 1979. The colors have been enhanced to bring out detail. Zones of light-colored, ascending clouds alternate with bands of dark, descending clouds. The clouds travel around the planet in alternating eastward and westward belts at speeds of up to 540 kilometers per hour. Tremendous storms as big as Earthly continents surge around the planet. The Great Red Spot (oval shape toward the lower-left) is an enormous anticyclonic storm that drifts along its belt, eventually circling the entire planet.
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Full-color image of Mercury from first MESSENGER flyby.
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Autor: Renerpho, Licencja: CC BY-SA 4.0
2003 AZ84 (center) and its possible satellite
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Ceres in true color taken by Dawn on May 4, 2015. Oxo Crater, Haulani Crater, and Ahuna Mons are visible.
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Charon, taken by New Horizons late on 13 July 2015
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As NASA's Dawn spacecraft takes off for its next destination, this mosaic synthesizes some of the best views the spacecraft had of the giant asteroid Vesta. Dawn studied Vesta from July 2011 to September 2012. The towering mountain at the south pole — more than twice the height of Mount Everest — is visible at the bottom of the image. The set of three craters known as the "snowman" can be seen at the top left.
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Autor: Palomar Observatory/Digitized Sky Survey/California Institute of Technology, Licencja: CC BY 2.0
90-minute exposure precovery image of 2002 XV93 taken by the Palomar Observatory in 28 September 1992. DSS precovery images are from DSS plate archive scans by the California Institute of Technology.
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Proteus is the second largest moon of Neptune behind the mysterious Triton. Proteus was discovered only in 1989 by the Voyager 2 spacecraft. This is unusual since Neptune has a smaller moon - Nereid - which was discovered 33 years earlier from Earth. The reason Proteus was not discovered sooner is that its surface is very dark and it orbits much closer to Neptune. Proteus has an odd box-like shape and were it even slightly more massive, its own gravity would cause it to reform itself into a sphere.

Original NASA caption: This image of Neptune's satellite 1989N1 was obtained on Aug. 25, 1989 from a range of 146,000 kilometers (91,000 miles). The resolution is about 2.7 kilometers (1.7 miles) per line pair.

The satellite, seen here about half illuminated, has an average radius of some 200 kilometers (120 miles). It is dark (albedo 6 percent) and spectrally grey. Hints of crater-like forms and groove-like lineations can be discerned. The apparent graininess of the image is caused by the short exposure necessary to avoid significant smear.
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This image of Rhea was acquired by the Voyager 1 spacecraft on November 11, 1980.
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Neptune
Original Caption Released with Image: During August 16 and 17, 1989, the Voyager 2 narrow-angle camera was used to photograph Neptune almost continuously, recording approximately two and one-half rotations of the planet. These images represent the most complete set of full disk Neptune images that the spacecraft will acquire. This picture from the sequence shows two of the four cloud features which have been tracked by the Voyager cameras during the past two months. The large dark oval near the western limb (the left edge) is at a latitude of 22 degrees south and circuits Neptune every 18.3 hours. The bright clouds immediately to the south and east of this oval are seen to substantially change their appearances in periods as short as four hours. The second dark spot, at 54 degrees south latitude near the terminator (lower right edge), circuits Neptune every 16.1 hours. This image has been processed to enhance the visibility of small features, at some sacrifice of color fidelity. The Voyager Mission is conducted by JPL for NASA's Office of Space Science and Applications.
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Hubble Space Telescope image of (55637) 2002 UX25
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This mosaic of the four highest-resolution images of Ariel represents the most detailed Voyager 2 picture of this satellite of Uranus. The images were taken through the clear filter of Voyager's narrow-angle camera on Jan. 24, 1986, at a distance of about 130,000 kilometers (80,000 miles). Ariel is about 1,200 km (750 mi) in diameter; the resolution here is 2.4 km (1.5 mi). Much of Ariel's surface is densely pitted with craters 5 to 10 km (3 to 6 mi) across. These craters are close to the threshold of detection in this picture. Numerous valleys and fault scarps crisscross the highly pitted terrain. Voyager scientists believe the valleys have formed over down-dropped fault blocks (graben); apparently, extensive faulting has occurred as a result of expansion and stretching of Ariel's crust. The largest fault valleys, near the terminator at right, as well as a smooth region near the center of this image, have been partly filled with deposits that are younger and less heavily cratered than the pitted terrain. Narrow, somewhat sinuous scarps and valleys have been formed, in turn, in these young deposits. It is not yet clear whether these sinuous features have been formed by faulting or by the flow of fluids.
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Hubble Space Telescope image of the cubewano 20000 Varuna, taken on 26 October 2005.
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PIA18317: Tethys the Target

http://photojournal.jpl.nasa.gov/catalog/PIA18317

Like most moons in the Solar System, Tethys is covered by impact craters. Some craters bear witness to incredibly violent events, such as the crater Odysseus (seen here at the right of the image).

While Tethys is 1,062 kilometers (660 miles) across, the crater Odysseus is 450 kilometers (280 miles) across, covering about 18 percent of the moon's surface area. A comparably sized crater on Earth would be as large as Africa!

This view looks toward the anti-Saturn hemisphere of Tethys. North on Tethys is up and rotated 42 degrees to the right. The image was taken in visible light with the Cassini spacecraft narrow-angle camera on April 11, 2015.

The view was acquired at a distance of approximately 190,000 kilometers (118,000 miles) from Tethys. Image scale is 1 kilometer (3,280 feet) per pixel.

The Cassini mission is a cooperative project of NASA, ESA (the European Space Agency) and the Italian Space Agency. The Jet Propulsion Laboratory, a division of the California Institute of Technology in Pasadena, manages the mission for NASA's Science Mission Directorate, Washington. The Cassini orbiter and its two onboard cameras were designed, developed and assembled at JPL. The imaging operations center is based at the Space Science Institute in Boulder, Colorado.

For more information about the Cassini–Huygens mission visit http://saturn.jpl.nasa.gov and http://www.nasa.gov/cassini. The Cassini imaging team homepage is at http://ciclops.org.
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Hubble Space Telescope image of cubewano 50000 Quaoar and its moon Weywot, taken on 14 February 2006.
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This image shows a view of the trailing hemisphere of Jupiter's ice-covered satellite, Europa, in approximate natural color. Long, dark lines are fractures in the crust, some of which are more than 3,000 kilometers (1,850 miles) long. The bright feature containing a central dark spot in the lower third of the image is a young impact crater some 50 kilometers (31 miles) in diameter. This crater has been provisionally named "Pwyll" for the Celtic god of the underworld. Europa is about 3,160 kilometers (1,950 miles) in diameter, or about the size of Earth's moon. This image was taken on September 7, 1996, at a range of 677,000 kilometers (417,900 miles) by the solid state imaging television camera onboard the Galileo spacecraft during its second orbit around Jupiter. The image was processed by Deutsche Forschungsanstalt fuer Luftund Raumfahrt e.V., Berlin, Germany.
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PLUTO - NEW HORIZONS - July 14, 2015

ORIGINAL IMAGE DESCRIPTION:

Four images from New HorizonsLong Range Reconnaissance Imager (LORRI) were combined with color data from the Ralph instrument to create this global view of Pluto. (The lower right edge of Pluto in this view currently lacks high-resolution color coverage.) The images, taken when the spacecraft was 280,000 miles (450,000 kilometers) away, show features as small as 1.4 miles (2.2 kilometers), twice the resolution of the single-image view taken on July 13 [2015].

UPLOADER NOTES:

The north polar region is at top, with bright Tombaugh Regio to the lower right of center and part of the dark Cthulhu Regio at lower left. Part of the dark Krun Regio is also visible at extreme lower right.

The original NASA image has been modified by doubling the linear pixel density and cropping.
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Haumea and its satellites, imaged on June 30, 2015 by the Hubble Space Telescope
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Hubble Space Telescope image of the cubewano 174567 Varda and its satelite Ilmarë, taken on 31 August 2010.
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Autor: Credit: ESO/Vernazza et al., Licencja: CC BY 4.0
VLT's SPHERE spies rocky worlds

From the description at File:Potw1749a.tif:

These images were taken by ESO's SPHERE (Spectro-Polarimetric High-Contrast Exoplanet Research) instrument, installed on the Very Large Telescope at the Paranal Observatory, Chile. These strikingly-detailed views reveal four of the millions of rocky bodies in the main asteroid belt, a ring of asteroids between Mars and Jupiter that separates the rocky inner planets of the Solar System from the gaseous and icy outer planets.

Clockwise from top left, the asteroids shown here are 29 Amphitrite, 324 Bamberga, 2 Pallas, and 89 Julia. Named after the Greek goddess Pallas Athena, 2 Pallas is about 510 kilometres wide. This makes it the third largest asteroid in the main belt and one of the biggest asteroids in the entire Solar System. It contains about 7% of the mass of the entire asteroid belt — so hefty that it was once classified as a planet. A third of the size of 2 Pallas, 89 Julia is thought to be named after St Julia of Corsica. Its stony composition led to its classification as an S-type asteroid. Another S-type asteroid is 29 Amphitrite, which was only discovered in 1854. 324 Bamberga, one of the largest C-type asteroid in the asteroid belt, was discovered even later: Johann Palisa found it in 1892. Today, it is understood that C-type asteroids may actually be bodies from the outer Solar System following the migration of the giant planets. As such, they may contain ice in their interior.

Although the asteroid belt is often portrayed in science fiction as a place of violent collisions, packed full of large rocks too dangerous for even the most skilled of space pilots to navigate, it is actually very sparse. In total, the asteroid belt contains just 4% of the mass of the Moon, with about half of this mass contained in the four largest residents: Ceres, 4 Vesta, 2 Pallas, and 10 Hygiea.