Lista obiektów w Układzie Słonecznym ze względu na masę

Lista obiektów w Układzie Słonecznym ze względu na masę, w porządku malejącym. Lista jest niekompletna, gdyż masa wielu planetoid jest obecnie nieznana.

Kolejność obiektów jest podobna, jak na liście obiektów w Układzie Słonecznym ze względu na promień. Niektóre tylko ciała są mniejsze, ale za to cięższe od innych, większych. Dla przykładu Neptun jest masywniejszy od Urana, ale mniejszy od niego. Podobnie Merkury jest cięższy od Ganimedesa i Tytana, aczkolwiek mniejszy.

Nota: satelity zostały oznaczone gwiazdką.

Zakres jottagrama

Następująca lista zawiera obiekty Układu Słonecznego o masie ponad 1021 kilogramów (1 jottagram [Yg]). Nawet najlżejsze obiekty z tej listy są w przybliżeniu sferyczne[1].

PozycjaNazwaZdjęcieMasa w YgMasa w kgMas ZiemiRodzaj obiektu
1Słońce
Sun920607.jpg
1 989 100 0001,9891×1030[2]332837gwiazda
2Jowisz
Jupiter.jpg
1 899 0001,899×1027318,7215-ta planeta
3Saturn
Saturn-cassini-March-27-2004.jpg
568 4605,6846×102695,1526-ta planeta
4Neptun
Neptune.jpg
102 4301,0243×102617,1458-ma planeta
5Uran
Uranus.jpg
86 8328,6832×102514,5347-ma planeta
6Ziemia
The Earth seen from Apollo 17.jpg
5974,25,9742×102413-cia planeta
7Wenus
Venus-real.jpg
4868,54,8685×10240,814922-ga planeta
8Mars
Mars Valles Marineris.jpeg
641,856,4185×10230,1074-ta planeta
9Merkury
Mercury in color - Prockter07 centered.jpg
330,23,302×10230,05531-sza planeta
10* Ganimedes
Ganymede g1 true.jpg
148,21,482×10230,0248księżyc Jowisza
11* Tytan
Titan in natural color Cassini.jpg
134,51,345×10230,0225księżyc Saturna
12* Callisto
Callisto.jpg
107,61,076×10230,018księżyc Jowisza
13* Io
Io highest resolution true color.jpg
89,38,9319×10220,015księżyc Jowisza
14* Księżyc
Moon merged small.jpg
73,57,3477×10220,0123księżyc Ziemi
15* Europa
Europa-moon.jpg
48,04,80×10220,00803księżyc Jowisza
16* Tryton
Triton moon mosaic Voyager 2 (large).jpg
21,52,147×10220,00359księżyc Neptuna
17(136199) Eris
Eris and Dysnomia.png
16,61,67×1022~0,0027planeta karłowata
18(134340) Pluton
Nh-pluto-in-true-color 2x JPEG.jpg
13,11,305 ± 0.007×1022~0,0022planeta karłowata
19(136108) Haumea
Haumea Hubble.png
4,24,2 ± 0,1 × 1021~0,00069planeta karłowata
20(136472) Makemake
Makemake and its moon.jpg
~4~4 × 1021~0,00067planeta karłowata
21* Tytania
3,53,526×1021~0,00059księżyc Urana
22* Oberon
Voyager 2 picture of Oberon.jpg
3,03,014×1021~0,00050księżyc Urana
23(90377) Sedna
Sedna PRC2004-14d.jpg
~3~3×1021~0,00050obiekt transneptunowy
24* Rea
2,32,3166×1021~0,00039księżyc Saturna
25(50000) Quaoar
Quaoar-weywot hst.jpg
~2~2×1021~0,00033obiekt transneptunowy
26* Iapetus
Iapetus by Voyager 2 - enhanced.jpg
2,01,9739×1021~0,00033księżyc Saturna
27* Charon
Charon by New Horizons on 13 July 2015.png
1,51,52 ± 0,06×1021~0,00025księżyc Plutona
28* Ariel
Ariel (moon).jpg
1,41,35×1021~0,00022księżyc Urana
29* Umbriel
Umbriel (moon).jpg
1,21,2×1021~0,00020księżyc Urana
30* Dione
Dione.jpg
1,11,096×1021~0,00018księżyc Saturna
Znak gwiazdki (* ) oznacza satelitę.

Zakres zettagrama

Obiekty o masie od 1018 do 1021 kg (od 1 do 1000 zettagramów [Zg]). Największe obiekty w tym przedziale, takie jak Tetyda, (1) Ceres, czy Mimas, są spłaszczonymi elipsoidami obrotowymi – dzięki ich grawitacji, podczas gdy mniej masywne ciała (na przykład Amaltea, czy Janus), są tylko w przybliżeniu sferyczne. W tabeli opisano ich kształt jako "nieregularny".

Wszystkie elipsoidalne ciała mają lekkie spłaszczenie biegunowe zależne od szybkości ich rotacji, ale charakterystyczną cechą ciał "nieregularnych" jest wyraźna różnica długości średnic równikowych mierzona w różnych kierunkach.

Zostało zasugerowane by obiektów transneptunowych o masie poniżej 1020 kg nie umieszczać na tej liście z powodu mało dokładnych danych o ich masie.
NazwaZdjęcieMasa w kgRodzaj obiektuKształt
(1) Ceres
Ceresintruecolor.png
9,5×1020planeta karłowataspłaszczona elipsoida obrotowa
(90482) Orkus
Orcus-vanth hst.jpg
~6,2×1020obiekt transneptunowynieznany
* Tetyda
Tethys cassini.jpg
6,173×1020księżyc Saturnawydłużona elipsoida obrotowa
(28978) Iksjon
Ixion planetoid nasa.jpg
6×1020obiekt transneptunowynieznany
(20000) Waruna~5,9×1020obiekt transneptunowynieznany
(4) Westa
Vesta 4.jpg
2,7×1020planetoidaspłaszczona elipsoida obrotowa
(15874) 1996 TL66~2,6×1020obiekt dysku rozproszonegonieznany
(2) Pallas
Potw1749a Pallas crop.png
2,2×1020planetoidanieregularny
* Enceladus
Enceladus from Voyager.jpg
1,08×1020księżyc Saturnawydłużona elipsoida obrotowa
(10) Hygiea
SPHERE image of Hygiea.jpg
9×1019planetoidanieregularny
(511) Davida
511 Davida dettaglio.png
~6,6×1019planetoidanieregularny
* Miranda
PIA18185 Miranda's Icy Face.jpg
6,59×1019księżyc Uranawydłużona elipsoida obrotowa
(704) Interamnia
Interamnia medie.gif
6×1019planetoidanieregularny
* Proteusz
Proteus (Voyager 2).jpg
5×1019księżyc Neptunanieregularny
(52) Europa
52Eur-LB1-richfield.jpg
~5×1019planetoidanieregularny
* Mimas
Mimas moon.jpg
3,752×1019księżyc Saturnawydłużona elipsoida obrotowa
(15) Eunomia3,3×1019planetoidanieregularny
* Nereida
Nereid-Voyager2.jpg
3,1×1019 kgksiężyc Neptunanieregularny
(3) Juno
Juno from Hooker telescope.jpg
3,0×1019planetoidanieregularny
(16) Psyche~1,7×1019planetoidanieregularny
(31) Euphrosyne~1,69×1019planetoidanieregularny
(87) Sylvia1,478×1019planetoidanieregularny
(6) Hebe~1,4×1019planetoidanieregularny
(624) Hektor
624Hektor-LB1-mag15.jpg
~1,4×1019planetoidanieregularny
(130) Elektra1,28×1019planetoidanieregularny
(65) Cybele~1,15×1019planetoidanieregularny
(107) Camilla1,09×1019planetoidanieregularny
(7) Iris
7Iris-LB1-richfield-mag10.jpg
1,0×1019planetoidanieregularny
(324) Bamberga
Potw1749a Bamberga crop.png
1,0×1019planetoidanieznany
(9) Metis~9×1018planetoidanieregularny
* Febe
Phoebe cassini.jpg
8,3×1018księżyc Saturnanieregularny
* Amaltea
Amalthea Mond.jpg
7,43×1018księżyc Jowiszanieregularny
* Himalia6,74×1018księżyc Jowiszanieregularny
(22) Kalliope
InsetKalliopeKVLT.jpg
6,3×1018planetoidanieregularny
(45) Eugenia5,8×1018planetoidanieregularny
* Hyperion
Hyperion PIA07740.jpg
5,58×1018księżyc Saturnanieregularny
(121) Hermione5,4×1018planetoidanieregularny
(20) Massalia5,2×1018planetoidanieregularny
* Larissa
Larissa 1.jpg
~4×1018księżyc Neptunanieregularny
(8) Flora~3,6×1018planetoidanieregularny
(85) Io~3,4×1018planetoidanieregularny
* Puk
Puck.png
~2,9×1018księżyc Urananieregularny
(2060) Chiron~2,7×1018centaurnieregularny
(5) Astraea~2,4×1018planetoidanieregularny
* Sykoraks~2,3×1018księżyc Urananieregularny
* Galatea
Galatea moon.jpg
2,12×1018księżyc Neptunanieregularny
* Despoina
Despina.jpg
~2,1×1018księżyc Neptunanieregularny
* Janus
Janus - Voyager 2.jpg
1,912×1018księżyc Saturnanieregularny
* Porcja~1,7×1018księżyc Urananieregularny
(141) Lumen~1,6×1018planetoida
* Tebe
Thebe.jpg
1,5×1018księżyc Jowiszanieregularny
(140) Siwa~1,5×1018planetoidanieregularny
(159) Aemilia~1,4×1018planetoida
(21) Lutetia
Rosetta triumphs at asteroid Lutetia.jpg
~1,3×1018planetoidanieregularny
(100) Hekate~1,0×1018planetoida

Zakres eksagrama

Obiekty o masie od 1015 do 1018 kg (od 1 do 1000 eksagramów [Eg]). Te obiekty nie są sferyczne.

Tylko niebywale warte uwagi planetoidy (na przykład odwiedzone przez sondę kosmiczną, o precyzyjnie znanej masie, bardzo specyficzne) są zamieszczone w tej sekcji.
NameImageMass in kgRodzaj obiektu
* Elara8,7×1017księżyc Jowisza
* Julia
Potw1749a Julia crop.png
~5,6×1017księżyc Urana
* Epimeteusz
Epimetheus.jpg
5,30×1017księżyc Saturna
(90) Antiope4,1×1017planetoida (większy składnik systemu podwójnego Antiope)
S/2000 (90) 14,1×1017planetoida (mniejszy składnik systemu podwójnego Antiope)
* Belinda~3,6×1017księżyc Urana
* Talassa~3,5×1017księżyc Neptuna
* Kresyda~3,4×1017księżyc Urana
* Pazyfae3,0×1017księżyc Jowisza
* Rozalinda~2,5×1017księżyc Urana
* Kaliban~2,5×1017księżyc Urana
* Najada
Naiad Voyager.png
~1,9×1017księżyc Neptuna
* Desdemona~1,8×1017księżyc Urana
* Prometeusz
1,57×1017księżyc Saturna
* Pandora
Pandora PIA07632.jpg
1,36×1017księżyc Saturna
* Karme1,3×1017księżyc Jowisza
(253) Mathilde
(253) mathilde.jpg
1,033×1017planetoida
* Metis
Metis.jpg
9,5467×1016księżyc Jowisza
* Bianka~9,2×1016księżyc Urana
* Prospero~8,5×1016księżyc Urana
* Sinope7,6×1016księżyc Jowisza
* Setebos~7,5×1016księżyc Urana
* Hydra
Hydra imaged by LORRI from 231 000 kilometres.jpg
~7×1016księżyc Plutona
* Nix
Nix (moon) in color.jpg
~7×1016księżyc Plutona
* Lizytea6,3×1016księżyc Jowisza
* Linus~6×1016satelita (22) Kalliope
* Ofelia~5,4×1016księżyc Urana
* Kordelia~4,4×1016księżyc Urana
(243) Ida
243 ida.jpg
4,2×1016planetoida
* Ananke3,82×1016księżyc Jowisza
* Adrastea
Adrastea.jpg
1,8894×1016księżyc Jowisza
* Psamathe~1,5×1016księżyc Neptuna
(1036) Ganymed3,3×1016planetoida bliska Ziemi
* Stefano~2,2×1016księżyc Urana
* Perdyta~1,3×1016księżyc Urana
* Leda1,09×1016księżyc Jowisza
* Fobos
Phobos colour 2008.jpg
1,08×1016księżyc Marsa
* Mab~1,0×1016księżyc Urana
(2685) Masursky0,5–1,1×1016planetoida
(433) Eros
433eros.jpg
7,2×1015planetoida
* Francisco~7,2×1016księżyc Urana
* Atlas
Atlas Rev09.2x.jpg
6,6×1015księżyc Saturna
* Ferdynand~5,4×1015księżyc Urana
* Margaret~5,4×1015księżyc Urana
* Pan
Pan Rev09.2x.jpg
4,9×1015księżyc Saturna
* Romulus~4×1015satelita (87) Sylvia
* Trinkulo~3,9×1015księżyc Urana
* Kupid~3,8×1015księżyc Urana
(951) Gaspra
951 Gaspra.jpg
2–3×1015planetoida
* Deimos
Deimos-MRO.jpg
2,2×1015księżyc Marsa
* S/2002 (121) 1~1,6×1015satelita (121) Hermione
* S/2001 (107) 1~1,5×1015satelita (107) Camilla
* Mały Książę~1,2×1015satelita (45) Eugenia

Zakres petagrama

Obiekty o masie od 1012 do 1015 kg (od 1 do 1000 petagramów [Pg]). Lista obejmuje kilka mniejszych, nieregularnych satelitów gazowych olbrzymów, a także największe planetoidy bliskie Ziemi. Inne obiekty bliskie Ziemi, nie będące planetoidami (na przykład komety krótkookresowe Układu Słonecznego), mają prawie zawsze masę mniejszą od 1 Pg.

NazwaMasa w kgRodzaj obiektu
* Temisto~6,89×1014księżyc Jowisza
* Karpo~4,5×1014księżyc Jowisza
* S/2003 (130) 1~4×1014księżyc planetoidy (130) Elektra
* Remus~2×1014księżyc planetoidy (87) Sylvia
(4179) Toutatis~5,0×1013NEA, Grupa Apolla, planetoida przecinająca orbitę Marsa
* Pallene~4,35×1013księżyc Saturna
* Polydeuces~3×1013księżyc Saturna
* Methone~1,85×1013księżyc Saturna
* Euporie~1,5×1013księżyc Jowisza
(1862) Apollo~5,1×1012NEA, Grupa Apolla, planetoida przecinająca orbitę Marsa
(1620) Geographos~4,0×1012[3]NEA, planetoida przecinająca orbitę Marsa
(1566) Ikar~2,9×1012NEA, planetoida przecinająca orbitę Merkurego, orbitę Wenus i orbitę Marsa
2007 CA19~1,2×1012NEA

Zakres teragrama

Obiekty o masie od 109 do 1012 kg (od 1 do 1000 teragramów [Tg]). Obecnie wszystkie te obiekty są planetoidami bliskimi Ziemi.

NazwaMasa w kg
(2062) Aten~7,6×1011
(4769) Castalia~5,0×1011
2004 VD17~3×1011[4]
2009 WM1~2,8×1010[5]
(99942) Apophis~2,7×1010[6]
1994 WR12~2 × 109[4]

Zakres gigagrama

Obiekty o masie od 106 do 109 kg (od 1 do 1000 gigagramów [Gg]). Obecnie wszystkie te obiekty są planetoidami bliskimi Ziemi.

NazwaMasa w kg
2000 SG344~7×107[4]
2006 QV89~4×107[4]
2004 FH~2,8×107[4]

Zobacz też

Uwagi

Wiele z podanych wartości zostało wziętych wprost z właściwych artykułów na Wikipedii. Niektóre zostały podane na podstawie Planetary Fact Sheets (ang.). Masa (20000) Waruna została oszacowana bazując na danych z [1] dotyczących jej gęstości i średnicy. Masa kilku większych obiektów nie jest jeszcze dokładnie znana. (24) Themis nie jest wymieniona z powodu kontrowersji na temat jego gęstości. (136199) Eris została dodana po odkryciu i wyznaczeniu orbity jej księżyca, Dysnomii.

Przypisy

  1. Ciała astronomiczne formują kuliste kształty (spłaszczona elipsoida obrotowa), gdy grawitacja jego własnej masy jest wystarczająca do przezwyciężenie sił spójności warunkujących sztywność jego wewnętrznej materii. Nazywane jest to zapadaniem grawitacyjnym.
  2. Sun Fact Sheet (ang.)
  3. Asteroid Fact Sheet (ang.)
  4. a b c d e Bazując na przeciętnej gęstości 2,6 g/cm³ danej przez the NASA NEO impact risk page https://www.webcitation.org/5wRY4rqQf?url=http://neo.jpl.nasa.gov/risk/index.html
  5. 2009 WM1 Earth Impact Risk (ang.). NASA/JPL. [dostęp 2009-12-03]. [zarchiwizowane z tego adresu (2009-11-27)].
  6. (99942) Apophis (2004 MN4) Earth Impact Risk (ang.). NASA/JPL. [dostęp 2009-12-03]. [zarchiwizowane z tego adresu (2013-05-12)].

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.
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.
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.
Potw1749a Julia crop.png
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.
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.
Thebe.jpg
This image of Thebe was taken by NASA's Galileo spacecraft on January 4, 2000, at a range of 193,000 kilometers.
Deimos-MRO.jpg
Color-enhanced image of Deimos, a moon of Mars, captured by the HiRISE instrument on the Mars Reconnaissance Orbiter on 21 Feb 2009. Cropped from source image.
Naiad Voyager.png
Naiad as seen by en:Voyager 2. The image is smeared due to the combination of long exposure needed at this distance from the Sun, and the rapid relative motion of the moon and Voyager. Hence, the moon appears more elongated than in reality. Subsequently the brightness was processed and the image cropped somewhat
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.
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.
Metis.jpg
Jovian satellite Metis, imaged by the Galileo spacecraft
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.
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.
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.
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a Photo of Asteroid (253) Mathilde taken by the space probe NEAR Shoemaker on 27 June 1997 from a distance of 2400 km. It is lit up by the sun from the top right. The part of the Asteroid visible in the picture has Dimensions of 59 km x 47 km, whereas the picture resolution is 380px. On the surface, numerous large craters are visible, like the Large Crater in the Center, named Karoo [1], which is more than 30 km wide. Most of it is shaded in the picture.
52Eur-LB1-richfield.jpg
(c) I, Kevin Heider, CC BY-SA 3.0
2 minute exposure of asteroid 52 Europa (bright star to lower left of E) with a 24" telescope. Europa is apparent magnitude 11.7 in this image taken at 2009-09-22 11:15 UT. (Astronomical twilight would be at 11:45 UT with sunrise at 13:15 UT.) To the lower right of Europa is HD 39395 at apmag 8.3 and to the lower left of Europa is HD 248796 at apmag 8.8. Both of these stars are over exposed resulting in the white streaks. To the upper right of Europa and HD 39395 is TYC 1312-2824-1 at apmag 11.3 (comparable to the brightness of Europa.)
Nix (moon) in color.jpg
The most high-definition picture of Nix released so far, cropped from the 'family portrait' of Pluto's moons. This color photograph made using Adobe Photoshop CS5.
Triton moon mosaic Voyager 2 (large).jpg
Global Color Mosaic of Triton, taken by Voyager 2 in 1989
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.
Despina.jpg
Despina as seen by Voyager 2. There is significant horizontal smearing due to the combination of long exposure needed at this distance from the Sun, and the rapid relative motion of the moon and Voyager.
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.
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.
Adrastea.jpg
Adrastea—the moon of Jupiter by Galileo
Ixion planetoid nasa.jpg
28978 Ixion. Ixion is shown by the yellow arrow in the center of the image. Courtesy of NASA
Nereid-Voyager2.jpg
衛星ネレイド、ボイジャー2号の撮影
Rosetta triumphs at asteroid Lutetia.jpg
Autor: ESA 2010 MPS for OSIRIS Team MPS/UPD/LAM/IAA/RSSD/INTA/UPM/DASP/IDA, Licencja: CC BY-SA 2.0
Asteroid 21 Lutetia has been revealed as a battered world of many craters. ESA's Rosetta mission has returned the first close-up images of the asteroid showing it is most probably a primitive survivor from the violent birth of the Solar System.
433eros.jpg
This picture of Eros, taken on February 14, 2001, shows the view looking from one end of the asteroid across the gouge on its underside and toward the opposite end. In this mosaic, constructed from two images taken after the NEAR spacecraft was inserted into orbit, features as small as 120 feet (35 meters) across can be seen. House-sized boulders are present in several places; one lies on the edge of the giant crater separating the two ends of the asteroid. A bright patch is visible on the asteroid in the top left-hand part of this image, and shallow troughs can be see just below this patch. The troughs run parallel to the asteroid's long dimension. (Mosaic of images 0125971425, 0125971487)
SPHERE image of Hygiea.jpg
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)
Jupiter.jpg
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.
Mercury in color - Prockter07 centered.jpg
Full-color image of Mercury from first MESSENGER flyby.
243 ida.jpg
This color picture is made from images taken by the imaging system on the Galileo spacecraft about 14 minutes before its closest approach to asteroid 243 Ida on August 28, 1993, at a distance of about 10,500 kilometers (6,500 miles). The images used are from the sequence in which Ida's moon was originally discovered; the moon is visible to the right of the asteroid. This picture is made from images through the 4100-ångström (violet), 7560 Å (infrared) and 9680 Å (infrared) filters. The color is 'enhanced' in the sense that the CCD camera is sensitive to near-infrared wavelengths of light beyond human vision; a 'natural' color picture of this asteroid would appear mostly gray. Shadings in the image indicate changes in illumination angle on the many steep slopes of this irregular body as well as subtle color variations due to differences in the physical state and composition of the soil (regolith). There are brighter areas, appearing bluish in the picture, around craters on the upper left end of Ida, around the small bright crater near the center of the asteroid, and near the upper right-hand edge (the limb). This is a combination of more reflected blue light and greater absorption of near infrared light, suggesting a difference in the abundance or composition of iron-bearing minerals in these areas. Ida's moon also has a deeper near-infrared absorption and a different color in the violet than any area on this side of Ida. The moon is not identical in spectral properties to any area of Ida in view here, though its overall similarity in reflectance and general spectral type suggests that it is made of the same rock types basically. These data, combined with study of further imaging data and more detailed spectra from the Near Infrared Mapping Spectrometer, may allow scientists to determine whether the larger parent body of which Ida, its moon, and some other asteroids are fragments was a heated, differentiated object or made of relatively unaltered primitive chondritic material.
Janus - Voyager 2.jpg
This is a colorized version of the high-resolution Voyager 2 spacecraft image of Janus that was taken on 25 August 1981. Janus was discovered by Audouin Dollfus in 1966 and was named after the god of gates and doorways. It is depicted with two faces looking in opposite directions. Janus has an irregular shape with a size of 196x192x150 kilometers (122x119x93 miles) in diameter. It is heavily cratered with several craters 30 kilometers (19 miles) in diameter. The pervasive cratering indicates that its surface must be several billion years old. Janus and Epimetheus share the same orbit of 151,472 kilometers (94,125 miles) from Saturn's center or 91,000 kilometers (56,547 miles) above the cloud tops. They are only separated by about 50 kilometers (31 miles). As these two satellites approach each other they exchange a little momentum and trade orbits; the inner satellite becomes the outer and the outer moves to the inner position. This exchange happens about once every four years. Janus and Epimetheus may have formed from a disruption of a single parent to form co-orbital satellites. If this is the case, the disruption must have happened early in the history of the satellite system.
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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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L'asteroide 511 Davida fotografato dal Keck Observatory, dicembre 2002.

Credit: W.M. Keck Observatory

http://www2.keck.hawaii.edu/news/science/asteroid/asteroid.html

http://solarsystem.nasa.gov/multimedia/display.cfm?IM_ID=142
Charon by New Horizons on 13 July 2015.png
Charon, taken by New Horizons late on 13 July 2015
Moon merged small.jpg
Autor: unknown, Licencja: CC-BY-SA-3.0
Proteus (Voyager 2).jpg
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.
Prometheus moon.jpg
Saturn's satellite Prometheus, acquired by the Voyager 2 spacecraft on August 25, 1981.
Hyperion PIA07740.jpg
original description: This stunning false-color view of Saturn's moon Hyperion reveals crisp details across the strange, tumbling moon's surface. Differences in color could represent differences in the composition of surface materials. The view was obtained during Cassini's close flyby on Sept. 26, 2005. Hyperion has a notably reddish tint when viewed in natural color. The red color was toned down in this false-color view, and the other hues were enhanced, in order to make more subtle color variations across Hyperion's surface more apparent. Images taken using infrared, green and ultraviolet spectral filters were combined to create this view. The images were taken with the Cassini spacecraft's narrow-angle camera at a distance of approximately 62,000 kilometers (38,500 miles) from Hyperion and at a Sun-Hyperion-spacecraft, or phase, angle of 52 degrees. The image scale is 362 meters (1,200 feet) 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 operations center is based at the Space Science Institute in Boulder, Colo.
Juno from Hooker telescope.jpg
The asteroid Juno was photographed in 2003 with a special optics system on the Hooker telescope at the Mount Wilson Observatory. The researchers at the Harvard-Smithsonian Center for Astrophysics who took the picture used varying wavelengths of light as measured in nanometers, starting with cyan and going into the infrared.
Titania (moon) color cropped.jpg
Original caption: This high-resolution color composite of Titania was made from Voyager 2 images taken Jan. 24, 1986, as the spacecraft neared its closest approach to Uranus. Voyager's narrow-angle camera acquired this image of Titania, one of the large moons of Uranus, through the violet and clear filters. The spacecraft was about 500,000 kilometers (300,000 miles) away; the picture shows details about 9 km (6 mi) in size. Titania has a diameter of about 1,600 km (1,000 mi). In addition to many scars due to impacts, Titania displays evidence of other geologic activity at some point in its history. The large, trenchlike feature near the terminator (day-night boundary) at middle right suggests at least one episode of tectonic activity. Another, basinlike structure near the upper right is evidence of an ancient period of heavy impact activity. The neutral gray color of Titania is characteristic of the Uranian satellites as a whole. The Voyager project is managed for NASA by the Jet Propulsion Laboratory.
Rhea (moon) thumb.jpg
This image of Rhea was acquired by the Voyager 1 spacecraft on November 11, 1980.
Amalthea Mond.jpg
Amalthea Moon
7Iris-LB1-richfield-mag10.jpg
(c) I, Kevin Heider, CC BY-SA 3.0
2 minute exposure of asteroid 7 Iris (blooming star to the lower left of I) with a 24" telescope. Iris is apparent magnitude 10.1 in this image taken at 2009-10-01 02:30 UT. (The moon was 90% full and 53 degrees away. Astronomical twilight ended at 02:15 UT and sunset was at 01:00 UT.) The star just to the upper left of Iris is TYC 6275-527-1 at magnitude 11.2. The star blooming to the far lower left of Iris is TYC 6275-164-1 at magnitude 10.0.
Larissa 1.jpg

Image:Larissa.jpg cropped and cut down to show only one image.

The photojournal caption for the original image:

These Voyager 2 images of satellite 1989N2 at a resolution of 4.2 kilometers (2.6 miles) per pixel reveal it to be and irregularly shaped, dark object. The satellite appears to have several craters 30 to 50 kilometers (18.5 to 31 miles) across. The irregular outline suggests that this moon has remained cold and rigid throughout much of its history. It is about 210 by 190 kilometers (130 by 118 miles), about half the size of 1989N1. It has a low albedo surface reflecting about 5 percent of the incident light. The Voyager Mission is conducted by JPL for NASA's Office of Space Science and Applications.
Neptune.jpg
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.
Hydra imaged by LORRI from 231 000 kilometres.jpg
Hydra imaged by the LORRI instrument aboard the New Horizons spacecraft on 14 July.
951 Gaspra.jpg
Asteroid en:951 Gaspra.

Calvin J. Hamilton's website View of the Solar System describes this image as follows:

"This picture Gaspra is a combination of the highest-resolution images and color information obtained by the Galileo spacecraft. The Sun is shining from the right. The subtle color variations on Gaspra's surface have been exaggerated. en:Albedo and color variations are associated with surface en:topography. The bluish areas are regions of slightly higher albedo and tend to be associated with some of the crisper craters and with ridges. The slightly reddish areas, apparently concentrated in low areas, represent regions of somewhat lower albedo. In general, such patterns can be explained in terms of greater exposure of fresher rock in the brighter bluish areas and the accumulation of some en:regolith materials in the darker reddish areas. (Courtesy USGS/NASA/JPL)" [1]
Vesta 4.jpg
Vesta 4 as imaged by the Dawn spacecraft on July 18 (distance about 10,500 km)
Galatea moon.jpg
Galatea as seen by Voyager 2. The image is smeared due to the combination of long exposure needed at this distance from the Sun, and the rapid relative motion of Galatea and Voyager. Hence, Galatea appears more elongated than in reality.
InsetKalliopeKVLT.jpg
Autor: F. Marchis/University of Berkeley, Licencja: CC BY-SA 4.0
VLT/NACO-8m observation of Kalliope and Linus
Ariel (moon).jpg
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.
Pandora PIA07632.jpg
NASA description:
Cassini acquired infrared, green and ultraviolet images on Sept. 5, 2005, which were combined to create this false-color view. The image was taken with the Cassini spacecraft narrow-angle camera at a distance of approximately 52,000 kilometers (32,000 miles) from Pandora and at a Sun-Pandora-spacecraft, or phase, angle of 54 degrees. Resolution in the original image was about 300 meters (1,000 feet) per pixel. The image has been magnified by a factor of two to aid visibility.
Phobos colour 2008.jpg
Kolorowa fotografia Fobosa, księżyca Marsa, wykonana przez sondę Mars Reconnaissance Orbiter w dniu 23 marca 2008 roku.
Quaoar-weywot hst.jpg
Hubble Space Telescope image of cubewano 50000 Quaoar and its moon Weywot, taken on 14 February 2006.
Mimas moon.jpg
Image of Mimas, moon of Saturn taken by the Cassini probe on August 1, 2005 at approximately 189,410 kilometres away.
Puck.png
translated from French: Image taken from Voyager 2 on 24 January 1986 of the Uranian moon Puck (at a distance of 493 Mm (thousand kilometers))
Europa-moon.jpg
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.
Nh-pluto-in-true-color 2x.jpg
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.
Phoebe cassini.jpg
Phoebe, as imaged by the Cassini probe.
Haumea Hubble.png
Haumea and its satellites, imaged on June 30, 2015 by the Hubble Space Telescope
Potw1749a Pallas crop.png
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.
Interamnia medie.gif
Autor: Cantiell, Licencja: CC BY-SA 3.0
Observation of the asteroid 704 Interamnia carried out at the Observatory of Teramo (Italy) in occasion of the 101-st anniversary from the discovery of the asteroid
Dione.jpg
This picture of Dione was take by Voyager 1 from a range of 162,000 kilometers on November 12, 1980. Many impact craters -- the record of the collision of cosmic debris -- are shown, the largest crater is less than 100 kilometers (62 miles) in diameter and shows a well-developed central peak. Bright rays represent material ejected from other impact craters. Sinuous valleys probably formed by faults break the moon's icy crust.
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(c) I, Kevin Heider, CC BY-SA 3.0
8 minute exposure of Jupiter Trojan 624 Hektor with a 24" telescope. Hektor is apparent magnitude 15.0 in this image taken at 2009-09-29 10:00 UT. The bright star blooming above asteroid Hektor is TYC 2351-444-1 at magnitude 9.9 (about the limit of typical 50mm binoculars). The star on the right of the bloom that is comparable to Hektor is magnitude 14.8. The star to the far lower left of Hektor (showing very mild blooming) is magnitude 12.7.
Potw1749a Bamberga crop.png
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.