Chronologiczny wykaz odkryć planet, planet karłowatych i ich księżyców w Układzie Słonecznym
Chronologiczny wykaz odkryć planet, planet karłowatych i ich księżyców w Układzie Słonecznym przedstawia w postaci tabelarycznej chronologiczny przegląd odkryć głównych obiektów w Układzie Słonecznym, takich jak: planety, planety karłowate i ich księżyce.
W dawnych czasach nadawanie nazw naturalnym satelitom nie zawsze miało miejsce w tym samym czasie, co ich odkrycie.
W poniższych tabelach nazwy księżyców są pogrubione, a nazwy planet i planet karłowatych – pochylone. Dane w tabelach są uszeregowane według dat pierwszych publikacji o odkryciu. Daty są przypisane literami:
- f: data pierwszego uwiecznienia w postaci graficznej (na fotografii, rysunku itp.)
- o: data pierwszej obserwacji przez człowieka za pomocą teleskopu lub płyty fotograficznej
- p: data pierwszej publikacji o odkryciu
Tabela kolorów
Planety, planety karłowate oraz ich naturalne satelity (księżyce) są opisane pod danymi kolorami:
| Planety | Planety karłowate | |
| Merkury | Jowisz i jego księżyce | Ceres |
| Wenus | Saturn i jego księżyce | Pluton i jego księżyce |
| Ziemia i jej Księżyc | Uran i jego księżyce | Haumea i jej księżyce |
| Mars i jego księżyce | Neptun i jego księżyce | Makemake i jego księżyc |
| Eris i jej księżyc | ||
Przed wiekiem XVII
| Przed wiekiem XVII | |||||
|---|---|---|---|---|---|
| data odkrycia | nazwa | zdjęcie | inna nazwa | uwagi | |
| Nieznana | Merkury |  | pierwsza planeta | Teoria geocentryczna zakładała, że nieruchoma Ziemia znajduje się w centrum wszechświata, a wokół niej krążą pozostałe ciała niebieskie: Księżyc, Merkury, Wenus, Słońce, Mars, Jowisz i Saturn (w kolejności od Ziemi). Teoria heliocentryczna Kopernika (ogłoszona w 1543 w De revolutionibus orbium coelestium) mówiła, że Ziemia wraz z innymi planetami krąży wokół Słońca (w kolejności od Słońca): Merkury, Wenus, Ziemia, Mars, Jowisz i Saturn. Położone w centrum Słońce nie było już uważane za planetę. | |
| Wenus |  | druga planeta | |||
| Ziemia |  | trzecia planeta | |||
| Mars |  | czwarta planeta, czerwona planeta | |||
| Jowisz |  | piąta planeta, Jupiter | |||
| Saturn |  | szósta planeta | |||
| Nieznana | Księżyc |  | Ziemia I | W teorii Kopernika Księżyc nie był już uważany za planetę, ale za naturalnego satelitę Ziemi. | |
Wiek XVII
| XVII wiek | ||||
|---|---|---|---|---|
| data odkrycia | nazwa | zdjęcie | inna nazwa | odkrywcy |
| 1610 | ||||
| o: 7 stycznia 1610 p: 13 marca 1610 | Kallisto |  | Jowisz IV | Galileusz[1] (Galileuszowe księżyce Jowisza)[a] |
| Io |  | Jowisz I | ||
| Europa |  | Jowisz II | ||
| o: 11 stycznia 1610 p: 13 marca 1610 | Ganimedes |  | Jowisz III | |
| 1650–1659 | ||||
| o: 25 marca 1655 p: 5 marca 1656 | Tytan |  | Saturn VI | Huygens[b][2] |
| 1670–1679 | ||||
| o: 25 października 1671 p: 1673 | Japet |  | Saturn VIII | Cassini[c] |
| o: 23 grudnia 1672 p: 1673 | Rea | Saturn V | ||
| 1680–1689 | ||||
| o: 21 marca 1684 p: 22 kwietnia 1686 | Tetyda |  | Saturn III | Cassini[d] |
| Dione |  | Saturn IV | ||
| data odkrycia | nazwa | zdjęcie | inna nazwa | odkrywcy |
Wiek XVIII
| XVIII wiek | ||||
|---|---|---|---|---|
| data odkrycia | nazwa | zdjęcie | inna nazwa | odkrywcy |
| 1780–1789 | ||||
| o: 13 marca 1781 p: 26 kwietnia 1781 | Uran |  | siódma planeta | Herschel[e][3] |
| o: 11 stycznia 1787 p: 15 lutego 1787 | Tytania |  | Uran III | Herschel[4] |
| Oberon |  | Uran IV | ||
| o: 28 sierpnia 1789[5] p: 12 listopada 1789 | Enceladus |  | Saturn II | Herschel[6] |
| o: 17 września 1789 p: 12 listopada 1789 | Mimas |  | Saturn I | |
| data odkrycia | nazwa | zdjęcie | inna nazwa | odkrywcy |
Wiek XIX
| XIX wiek | ||||
|---|---|---|---|---|
| data odkrycia | nazwa | zdjęcie | inna nazwa | odkrywcy |
| 1801 | ||||
| o: 1 stycznia 1801 p: 1801 | Ceres |  | ósma planeta (1801) asteroida (1851) planeta karłowata (2006) | Giuseppe Piazzi[f] |
| 1840–1849 | ||||
| o: 23 września 1846 p: 13 listopada 1846 | Neptun |  | trzynasta planeta (1846) ósma planeta (1851) | Galle i Le Verrier[7][8] |
| o: 10 października 1846 p: 13 listopada 1846 | Tryton | .jpg) | Neptun I | Lassell[9] |
| o: 16 września 1848 p: październik 1848 | Hyperion |  | Saturn VII | Bond, Bond, Lassell[10][11][12] |
| 1851 | ||||
| o: 24 października 1851 | Ariel | .jpg) | Uran I | Lassell[13] |
| Umbriel | .jpg) | Uran II | ||
| 1877 | ||||
| o: 12 sierpnia 1877 | Deimos |  | Mars II | Hall[14][15][16] |
| o: 18 sierpnia 1877 | Fobos |  | Mars I | |
| 1890–1899 | ||||
| o: 9 września 1892 p: 4 października 1892 | Amaltea |  | Jowisz V | Barnard[17] |
| f: 16 sierpnia 1898 o: 17 marca 1899 | Febe |  | Saturn IX | Pickering[18] |
| data odkrycia | nazwa | zdjęcie | inna nazwa | odkrywcy |
Wiek XX
| XX wiek | |||||
|---|---|---|---|---|---|
| data odkrycia | nazwa | zdjęcie | inna nazwa | odkrywcy | |
| 1901–1909 | |||||
| f: 3 grudnia 1904 p: 6 stycznia 1905 | Himalia[g] |  | Jowisz VI | Perrine[19][20][21] | |
| f: 2 stycznia 1905 p: 27 lutego 1905 | Elara[h] |  | Jowisz VII | Perrine[22][23][21] | |
| f: 27 stycznia 1908 o: 28 lutego 1908 p: 1–6 marca 1908 | Pazyfae[i] |  | Jowisz VIII | Melotte[24][25] | |
| 1910–1919 | |||||
| f: 21 lipca 1914 | Sinope[j] |  | Jowisz IX | Nicholson[26] | |
| 1930–1939 | |||||
| f: 23 stycznia 1930 o: 18 lutego 1930 p: 13 marca 1930 | Pluton |  | dziewiąta planeta (1930) planeta karłowata (2006) | Tombaugh[27] | |
| f: 6 lipca 1938 p: sierpień 1938 | Lizytea[k] |  | Jowisz X | Nicholson[28] | |
| f: 30 lipca 1938 p: sierpień 1938 | Karme[l] |  | Jowisz XI | Nicholson[28] | |
| 1940–1949 | |||||
| f: 16 lutego 1948 p: czerwiec 1949 | Miranda |  | Uran V | Kuiper[29] | |
| f: 1 maja 1949 p: sierpień 1949 | Nereida |  | Neptun II | Kuiper[30][31] | |
| 1950–1959 | |||||
| f: 28 września 1951 p: grudzień 1951 | Ananke[m] | Jowisz XII | Nicholson[32] | ||
| 1960–1969 | |||||
| f: 15 grudnia 1966 | Janus[n] | S/1966 S 2 |  | Saturn X | Dollfus[o][33][34][35][36][37][38] |
| f: 18 grudnia 1966 | Epimeteusz[p] | S/1980 S 3 |  | Saturn XI | Walker[39] |
| 1970–1979 | |||||
| f: 11 września 1974 p: 20 września 1974 | Leda | Jowisz XIII | Kowal[40][41][42][43] | ||
| f: 30 września 1975 p: 3 października 1975 | Temisto[q] | S/1975 J 1 | Jowisz XVIII | Kowal[44][45][46] | |
| f: 13 kwietnia 1978 o: 22 czerwca 1978 | Charon | S/1978 P 1 |  | Pluton I | Christy[47][48] |
| f: 8 lipca 1979 p: 23 listopada 1979 | Adrastea | S/1979 J 1 |  | Jowisz XV | Jewitt, Danielson / Voyager 2[49][50][51][52][53] |
| 1980–1989 | |||||
| f: 19 lutego 1980 | Janus | S/1980 S 1 | | Saturn X | Voyager 1[36][54][55][38][56] |
| f: 26 lutego 1980 | Epimeteusz | S/1980 S 3 | | Saturn XI | Voyager 1[57][54][55][38][56] |
| f: 1 marca 1980 | Helena | S/1980 S 6 |  | Saturn XII | Laques, Lecacheux[57][54][55][56] |
| f: 13 marca 1980 | Kalipso | S/1980 S 25 |  | Saturn XIV | Pascu, Seidelmann, Baum, Currie[55][56] |
| f: 8 kwietnia 1980 | Telesto | S/1980 S 13 |  | Saturn XIII | Smith, Reitsema, Larson, Fountain, Voyager 1[58][56] |
| f: 5 marca 1979 p: 28 kwietnia 1980 | Tebe | S/1979 J 2 |  | Jowisz XIV | Synnott, Voyager 1[59][60] |
| f: 4 marca 1979 p: 26 sierpnia 1980 | Metis | S/1979 J 3 |  | Jowisz XVI | Synnott, Voyager 1[60] |
| o: październik 1980 | Atlas | S/1980 S 28 |  | Saturn XV | Terrile, Voyager 1[61] |
| o: październik 1980 p: 31 października 1980 | Prometeusz | S/1980 S 27 |  | Saturn XVI | Collins, Voyager 1[62] |
| Pandora | S/1980 S 26 |  | Saturn XVII | Collins, Voyager 1[62] | |
| f: 24 maja 1981 p: 29 maja 1981 | Larissa[q] | S/1981 N 1 = S/1989 N 2 |  | Neptun VII | Reitsema, Hubbard, Lebofsky, Tholen, Voyager 2[63][64] |
| f: 30 grudnia 1985 | Puk | S/1985 U 1 |  | Uran XV | Synnott, Voyager 2[65] |
| f: 3 stycznia 1986 | Julia | S/1986 U 2 |  | Uran XI | Synnott, Voyager 2[66][67] |
| Porcja | S/1986 U 1 |  | Uran XII | ||
| f: 9 stycznia 1986 | Kresyda | S/1986 U 3 | | Uran IX | |
| f: 13 stycznia 1986 | Desdemona | S/1986 U 6 |  | Uran X | |
| Rozalinda | S/1986 U 4 |  | Uran XIII | ||
| Belinda | S/1986 U 5 |  | Uran XIV | ||
| f: 20 stycznia 1986 | Kordelia | S/1986 U 7 |  | Uran VI | Terrile, Voyager 2[68] |
| Ofelia | S/1986 U 8 | | Uran VII | ||
| f: 23 stycznia 1986 | Bianka | S/1986 U 9 |  | Uran VIII | Smith, Voyager 2[68] |
| f: 16 czerwca 1989 p: 7 lipca 1989 | Proteusz | S/1989 N 1 | .jpg) | Neptun VIII | Synnott, Voyager 2[69] |
| f: 28 lipca 1989 p: 2 sierpnia 1989 | Despoina | S/1989 N 3 |  | Neptun V | Synnott, Voyager 2[64] |
| Galatea | S/1989 N 4 |  | Neptun VI | ||
| f: 18 września 1989 p: 29 września 1989 | Talassa | S/1989 N 5 |  | Neptun IV | Terrile, Voyager 2[70] |
| Najada | S/1989 N 6 |  | Neptun III | ||
| 1990–1999 | |||||
| data odkrycia | nazwa | tymcz. oznaczenie | zdjęcie | inna nazwa | odkrywcy |
| f: 22 sierpnia 1981 p: 16 lipca 1990 | Pan[r] | S/1981 S 13 |  | Saturn XVIII | Showalter, Voyager 2[71] |
| f: 23 sierpnia 1981 p: 14 kwietnia 1995 | Pallene[s] | S/1981 S 14 | Gordon, Murray i Beurle[72][73] | ||
| f: 6 września 1997 p: 31 października 1997 | Kaliban | S/1997 U 1 |  | Uran XVI | Gladman, Nicholson, Burns, Kavelaars[74] |
| Sykoraks | S/1997 U 2 |  | Uran XVII | Gladman, Nicholson, Burns, Kavelaars[74] | |
| f: 18 stycznia 1986 p: 18 maja 1999 | Perdyta[t] | S/1986 U 10 |  | Uran XXV | Karkoschka, Voyager 2[75] |
| f: 18 lipca 1999 | Setebos | S/1999 U 1 | Uran XIX | Kavelaars, Gladman, Holman, Petit, Scholl[76] | |
| Stefano | S/1999 U 2 | Uran XX | Gladman, Holman, Kavelaars, Petit, Scholl[76] | ||
| Prospero | S/1999 U 3 | Uran XVIII | Holman, Kavelaars, Gladman, Petit, Scholl[77] | ||
| 2000 | |||||
| data odkrycia | nazwa | tymcz. oznaczenie | zdjęcie | inna nazwa | odkrywcy |
| f: 6 października 1999 p: 20 lipca 2000 | Callirrhoe | S/1999 J 1 |  | Jowisz XVII | Scotti, Spahr, McMillan, Larsen, Montani, Gleason, Gehrels[78][79] |
| f: 7 sierpnia 2000 | Imir | S/2000 S 1 | Saturn XIX | Gladman[80][81] | |
| Paaliaq | S/2000 S 2 | Saturn XX | |||
| Kiviuq | S/2000 S 5 | Saturn XXIV | Gladman[82][83] | ||
| f: 23 września 2000 | Siarnaq | S/2000 S 3 | Saturn XXIX | Gladman, Kavelaars[84][83] | |
| Tarvos | S/2000 S 4 | Saturn XXI | Kavelaars, Gladman[84][83] | ||
| Ijiraq | S/2000 S 6 | Saturn XXII | Kavelaars, Gladman[82][83] | ||
| Thrymr | S/2000 S 7 | Saturn XXX | Gladman, Kavelaars[85][81] | ||
| Skadi | S/2000 S 8 | Saturn XXVII | Kavelaars, Gladman[85][81] | ||
| Mundilfari | S/2000 S 9 | Saturn XXV | Gladman, Kavelaars[85][81] | ||
| Erriapus | S/2000 S 10 | Saturn XXVIII | Kavelaars, Gladman[86][83] | ||
| Suttungr | S/2000 S 12 | Saturn XXIII | Gladman, Kavelaars[87][88] | ||
| f: 9 listopada 2000 p: 19 grudnia 2000 | Albioriks | S/2000 S 11 | Saturn XXVI | Holman, Spahr[89][90] | |
| f: 21 listopada 2000 p: 25 listopada 2000 | Temisto[q] | S/2000 J 1 |  | Jowisz XVIII | Sheppard, Jewitt, Fernández, Magnier[91][92] |
| data odkrycia | nazwa | tymcz. oznaczenie | zdjęcie | inna nazwa | odkrywcy |
Wiek XXI
| XXI wiek | |||||
|---|---|---|---|---|---|
| 2001–2009 | |||||
| data odkrycia | nazwa | tymcz. oznaczenie | zdjęcie | inna nazwa | odkrywcy |
f: 23 listopada 2000 | Kalyke | S/2000 J 2 | Jowisz XXIII | Sheppard, Jewitt, Fernández, Magnier, Dahm, Evans[93][94] | |
| Jokasta | S/2000 J 3 | Jowisz XXIV | |||
| Erinome | S/2000 J 4 | Jowisz XXV | |||
| Harpalyke | S/2000 J 5 | Jowisz XXII | |||
| Isonoe | S/2000 J 6 | Jowisz XXVI | |||
| Praxidike | S/2000 J 7 | Jowisz XXVII | Sheppard, Jewitt, Fernández, Magnier, Dahm, Evans[93][95] | ||
| f: 25 listopada 2000 p: 5 stycznia 2001 | Megaclite | S/2000 J 8 | Jowisz XIX | ||
| Taygete | S/2000 J 9 | Jowisz XX | |||
| f: 26 listopada 2000 p: 5 stycznia 2001 | Chaldene | S/2000 J 10 | Jowisz XXI | ||
| f: 5 grudnia 2000 p: 5 stycznia 2001 | Dia | S/2000 J11 | Jowisz LIII | ||
| f: 9 grudnia 2001 p: 16 maja 2002 | Hermippe | S/2001 J 3 |  | Jowisz XXX | Sheppard, Jewitt, Kleyna[96] |
| Eurydome | S/2001 J 4 | Jowisz XXXII | |||
| Sponde | S/2001 J 5 | Jowisz XXXVI | |||
| Kale | S/2001 J 8 | Jowisz XXXVII | |||
| f: 10 grudnia 2001 p: 16 maja 2002 | Autonoe | S/2001 J 1 | Jowisz XXVIII | ||
| f: 11 grudnia 2001 p: 16 maja 2002 | Thyone | S/2001 J 2 | Jowisz XXIX | ||
| Pasithee | S/2001 J 6 | Jowisz XXXVIII | |||
| Euanthe | S/2001 J 7 | Jowisz XXXIII | |||
| Orthosie | S/2001 J 9 | Jowisz XXXV | |||
| Euporie | S/2001 J 10 | Jowisz XXXIV | |||
| Aitne | S/2001 J 11 | Jowisz XXXI | |||
| f: 13 sierpnia 2001 p: 30 września 2002 | Trinkulo | S/2001 U 1 | Uran XXI | Holman, Kavelaars, Milisavljevic[97][98] | |
| f: 31 października 2002 p: 18 grudnia 2002 | Arche | S/2002 J 1 | Jowisz XLIII | Sheppard, Meech, Hsieh, Tholen, Tonry[99][100] | |
| f: 23 lipca 2002 p: 13 stycznia 2003 | Sao | S/2002 N 2 | Neptun XI | Holman, Kavelaars, Grav, Fraser, Milisavljevic[101][102] | |
| f: 10 sierpnia 2002 p: 13 stycznia 2003 | Halimede | S/2002 N 1 | Neptun IX | ||
| f: 11 sierpnia 2002 p: 13 stycznia 2003 | Laomedea | S/2002 N 3 | Neptun XII | ||
| f: 5 lutego 2003 p: 4 marca 2003 | Eukelade | S/2003 J 1 | Jowisz XLVII | Sheppard, Jewitt, Kleyna, Fernández, Hsieh[103][104] | |
| S/2003 J 2 | |||||
| S/2003 J 3 | Jowisz LX | ||||
| S/2003 J 4 | |||||
| f: 6 lutego 2003 p: 4 marca 2003 | S/2003 J 5 | Jowisz LVII | |||
| Helike | S/2003 J 6 | Jowisz XLV | |||
| f: 8 lutego 2003 p: 4 marca 2003 | Aoede | S/2003 J 7 | Jowisz XLI | ||
| f: 8 lutego 2003 p: 6 marca 2003 | Hegemone | S/2003 J 8 | Jowisz XXXIX | Sheppard, Jewitt, Kleyna, Fernández[105][106] | |
| f: 6 lutego 2003 p: 7 marca 2003 | S/2003 J 9 | Sheppard, Jewitt, Kleyna, Fernández[107][108] | |||
| S/2003 J 10 | |||||
| Kallichore | S/2003 J 11 | Jowisz XLIV | |||
| f: 8 lutego 2003 p: 7 marca 2003 | S/2003 J 12 | ||||
| f: 5 lutego 2003 p: 11 kwietnia 2003 | Narvi | S/2003 S 1 | Saturn XXXI | Sheppard, Jewitt, Kleyna[109] | |
| f: 9 lutego 2003 p: 11 kwietnia 2003 | Cyllene | S/2003 J 13 | Jowisz XLVIII | Sheppard, Jewitt, Kleyna[109] | |
| f: 8 lutego 2003 p: 11 kwietnia 2003 | Kore | S/2003 J 14 | Jowisz XLIX | ||
| f: 6 lutego 2003 p: 11 kwietnia 2003 | S/2003 J 15 | Jowisz LVIII | Sheppard, Jewitt, Kleyna, Fernández[109] | ||
| S/2003 J 16 | Gladman, Sheppard, Jewitt, Kleyna, Kavelaars, Petit, Allen[109] | ||||
| f: 8 lutego 2003 p: 11 kwietnia 2003 | Herse | S/2003 J 17 | Jowisz L | ||
| f: 6 lutego 2003 p: 11 kwietnia 2003 | S/2003 J 18 | Jowisz LV | Gladman, Kavelaars, Petit, Allen, Sheppard, Jewitt, Kleyna[109] | ||
| f: 6 lutego 2003 p: 30 kwietnia 2003 | S/2003 J 19 | Jowisz LXI | Gladman, Sheppard, Jewitt, Kleyna, Kavelaars, Petit, Allen[110][111] | ||
| f: 9 lutego 2003 p: 30 kwietnia 2003 | Karpo | S/2003 J 20 | Jowisz XLVI | Sheppard, Gladman, Kavelaars, Petit, Allen, Jewitt, Kleyna[110][112] | |
| f: 6 lutego 2003 p: 30 maja 2003 | Mneme | S/2003 J 21 | Jowisz XL | Sheppard, Jewitt, Kleyna, Gladman, Kavelaars, Petit, Allen[113][114] | |
| f: 18 stycznia 1986 p: 25 sierpnia 2003 | Perdyta | S/1986 U 10 | Uran XXV | Karkoschka[115] | |
| f: 13 sierpnia 2001 p: 29 sierpnia 2003 | Ferdynand[u] | S/2001 U 2 | Uran XXIV | 2001: Holman, Kavelaars, Milisavljevic; 2003: Sheppard, Jewitt[116][117] | |
| f: 14 sierpnia 2002 p: 29 sierpnia 2003 | Neso[v] | S/2002 N 4 | Neptun XIII | Holman, Kavelaars, Grav, Fraser, Milisavljevic[116][118] | |
| f: 29 sierpnia 2003 p: 3 września 2003 | Psamathe | S/2003 N 1 | Neptun X | Jewitt, Kleyna, Sheppard, Holman, Kavelaars[119][120] | |
| f: 25 sierpnia 2003 p: 25 września 2003 | Mab | S/2003 U 1 | Uran XXVI | Showalter, Lissauer[121] | |
| Kupid | S/2003 U 2 | Uran XXVII | |||
| f: 13 sierpnia 2001 p: 8 października 2003 | Francisco[w] | S/2001 U 3 |  | Uran XXII | Holman, Kavelaars, Milisavljevic, Gladman[122] |
| f: 29 sierpnia 2003 p: 9 października 2003 | Margaret | S/2003 U 3 | Uran XXIII | Sheppard, Jewitt[123][124] | |
| f: 9 lutego 2003 p: 25 stycznia 2004 | Thelxinoe[x] | S/2003 J 22 | Jowisz XLII | Sheppard, Jewitt, Kleyna, Gladman, Kavelaars, Petit, Allen[125][126] | |
| f: 6 lutego 2003 p: 4 lutego 2004 | S/2003 J 23[x] | Sheppard, Jewitt, Kleyna, Fernández[127][128] | |||
| f: 1 czerwca 2004 p: 16 sierpnia 2004 | Methone | S/2004 S 1 |  | Saturn XXXII | Porco, Charnoz, Brahic, Dones / Cassini-Huygens[129][130] |
| Pallene | S/2004 S 2 =S/1981 S 14 |  | Saturn XXXIII | ||
| f: 21 czerwca 2004 p: 9 września 2004 | S/2004 S 3?[y] |  | Murray, Porco i inni / Cassini-Huygens[131][132] | ||
| f: 21 czerwca 2004 p: 9 września 2004 | S/2004 S 4?[y] | Spitale, Porco i inni / Cassini-Huygens[131][132] | |||
| f: 21 października 2004 o: 24 października 2004 p: 8 listopada 2004 | Polideukes | S/2004 S 5 |  | Saturn XXXIV | Porco i inni / Cassini-Huygens[133] |
| f: 28 października 2004 p: 8 listopada 2004 | S/2004 S 6?[y] |  | |||
| f: 12 grudnia 2004 p: 4 maja 2005 | S/2004 S 7 | Sheppard, Jewitt, Kleyna, Marsden[134][135][136][137] | |||
| Fornjot | S/2004 S 8 | Saturn XLII | |||
| Farbauti | S/2004 S 9 | Saturn XL | |||
| Aegir | S/2004 S 10 | Saturn XXXVI | |||
| Bebhionn | S/2004 S 11 | Saturn XXXVII | |||
| S/2004 S 12 | |||||
| S/2004 S 13 | |||||
| Hati | S/2004 S 14 | Saturn XLIII | |||
| Bergelmir | S/2004 S 15 | Saturn XXXVIII | |||
| f: 13 grudnia 2004 p: 4 maja 2005 | Fenrir | S/2004 S 16 | Saturn XLI | Sheppard, Jewitt, Kleyna, Marsden[134][135][136][137] | |
| S/2004 S 17 | |||||
| Bestla | S/2004 S 18 | Saturn XXXIX | |||
| f: 1 maja 2005 p: 6 maja 2005 | Daphnis | S/2005 S 1 |  | Saturn XXXV | Porco i inni / Cassini-Huygens[138] |
| f: 6 maja 2004 o: 28 grudnia 2004 p: 29 lipca 2005 | Haumea | 2003 EL61 | planeta karłowata | Ortiz, Aceituno i Santos-Sanz lub Brown, Trujillo i Rabinowitz | |
| o: 26 stycznia 2005 p: 29 lipca 2005 | Hiʻiaka | S/2005 (2003 EL61) 1 | Haumea I | Brown, Trujillo i Rabinowitz | |
| o: 30 czerwca 2005 p: 29 lipca 2005 | Namaka | S/2005 (2003 EL61) 2 | Haumea II | Brown, Trujillo i Rabinowitz | |
| f: 31 marca 2005 p: 29 lipca 2005 | Makemake | 2005 FY9 |  | planeta karłowata | Brown, Trujillo i Rabinowitz |
| f: 21 października 2003 o: 5 stycznia 2005 p: 29 lipca 2005 | Eris | 2003 UB313 |  | planeta karłowata | Brown, Trujillo i Rabinowitz |
| f: 10 września 2005 p: 3 października 2005 | Dysnomia | S/2005 (2003 UB313) 1 | Eris I | Brown, van Dam, Bouchez, Le Mignant, Campbell, Chin, Conrad, Hartman, Johansson, Lafon, Rabinowitz, Stomski, Summers, Trujillo i Wizinowich[139] | |
| f: 15 maja 2005 o: 15 czerwca 2005 p: 31 października 2005 | Nix | S/2005 P 2 |  | Pluton II | Weaver, Stern, Mutchler, Steffl, Buie, Merline, Spencer, Young, Young[140] |
| Hydra | S/2005 P 1 |  | Pluton III | ||
| f: 12 grudnia 2004 o: 6 marca 2006(?) p: 26 czerwca 2006 | Hyrrokkin | S/2004 S 19 | Saturn XLIV | Sheppard, Jewitt, Kleyna[141][142] | |
| f: 4 stycznia 2006 o: 6 marca 2006(?) p: 26 czerwca 2006 | S/2006 S 1 | Sheppard, Jewitt, Kleyna[143][142] | |||
| Kari | S/2006 S 2 | Saturn XLV | |||
| f: 5 stycznia 2006 o: 6 marca 2006 (?) p: 26 czerwca 2006 | S/2006 S 3 | ||||
| Greip | S/2006 S 4 | Saturn LI | |||
| Loge | S/2006 S 5 | Saturn XLVI | |||
| Jarnsaksa | S/2006 S 6 | Saturn L | |||
| Surtur | S/2006 S 7 | Saturn XLVIII | |||
| Skoll | S/2006 S 8 | Saturn XLVII | |||
| f: 5 stycznia 2006 o: 16 stycznia 2007 (?) p: 13 kwietnia 2007 | Tarkek | S/2007 S 1 | Saturn LII | Sheppard, Jewitt, Kleyna[144] | |
| f: 18 stycznia 2007 p: 1 maja 2007 | S/2007 S 2 | Sheppard, Jewitt, Kleyna[145] | |||
| S/2007 S 3 | |||||
| f: 30 maja 2007 p: 18 czerwca 2007 | Anthe | S/2007 S 4 |  | Saturn XLIX | Porco i inni / Cassini-Huygens[146] |
| f: 15 sierpnia 2008 p: 3 marca 2009 | Aegaeon | S/2008 S 1 | .jpg){kind=small} | Saturn LIII | Cassini-Huygens[147] |
| f: 26 lipca 2009 p: 2 listopada 2009 | S/2009 S 1 |  | Cassini-Huygens[148] | ||
| 2010–2019 | |||||
| data odkrycia | nazwa | tymcz. oznaczenie | zdjęcie | inna nazwa | odkrywcy |
| o: 7 września 2010 p: 1 czerwca 2011 | S/2010 J 1 | Jowisz LI | Robert Jacobson, Marina Brozovic, Brett Gladman i M. Alexandersen[149] | ||
| o: 8 września 2010 p: 1 czerwca 2011 | S/2010 J 2 | Jowisz LII | Christian Veillet[149] | ||
| f: 28 czerwca 2011 o: 18 lipca 2011 | Kerberos | S/2011 (134340) 1 | .jpg) | Pluton IV | teleskop Hubble’a[150] |
| o: 27 września 2011 p: 29 stycznia 2012 | S/2011 J 1 | Jowisz LXXII | Sheppard[151] | ||
| S/2011 J 2 | Jowisz LVI | ||||
| f: 26 czerwca 2012 o: 11 lipca 2012 | Styx | S/2012 (134340) 1 | .jpg) | Pluton V | teleskop Hubble’a[152] |
| f: 2004 o: 1 lipca 2013 p: 15 lipca 2013 | Hippokamp | S/2004 N 1 |  | Neptun XIV | M. Showalter, I. de Pater, J.J. Lissauer, R.S. French[153] (teleskop Hubble’a)[154] |
| f: kwiecień 2015 p: 26 kwietnia 2016 | S/2015 (136472) 1 | .jpg) | (teleskop Hubble’a)[155] | ||
| f: 8 marca 2016 p: 2 czerwca 2017 | S/2016 J 1 | Jowisz LIV | Sheppard i inni[156][157][158][159][160][161][162][163][164][165][166][167] | ||
| f: 27 marca 2017 p: 2 czerwca 2017 | S/2017 J 1 | Jowisz LIX | |||
| f: 9 marca 2016 p: 17 lipca 2018 | Valetudo | S/2016 J 2 | bgcolor=black | Jowisz LXII | |
| f: 5 lutego 2016 o: 23 marca 2017 p: 17 lipca 2018 | S/2017 J 2 | Jowisz LXIII | |||
| S/2017 J 3 | Jowisz LXIV | ||||
| f: 23 marca 2017 p: 17 lipca 2018 | S/2017 J 4 | Jowisz LXV | |||
| S/2017 J 5 | Jowisz LXVI | ||||
| f: 24 lutego 2017 o: 23 marca 2017 p: 17 lipca 2018 | S/2017 J 6 | Jowisz LXVII | |||
| S/2017 J 7 | Jowisz LXVIII | ||||
| f: 23 marca 2017 p: 17 lipca 2018 | S/2017 J 8 | Jowisz LXIX | |||
| f: 24 lutego 2017 o: 23 marca 2017 p: 17 lipca 2018 | S/2017 J 9 | Jowisz LXX | |||
| f: 25 marca 2017 o: 11 maja 2018 p: 17 lipca 2018 | S/2018 J 1 | Jowisz LXXI | |||
| data odkrycia | nazwa | tymcz. oznaczenie | zdjęcie | inna nazwa | odkrywcy |
Uwagi
- ↑ Jeden z tych księżyców mógł zaobserwować chiński astronom Gan De w 364 p.n.e. Księżyce galileuszowe były pierwszymi poznanymi obiektami, krążącymi po orbicie wokół innej planety niż Ziemia.
- ↑ Huygens po raz pierwszy opublikował swoje odkrycie jako anagram, wysłany 13 czerwca 1655; później opublikował je w formie broszurki De Saturni luna Observatio Nova i w pełnej wersji: Systema Saturnium (lipiec 1659).
- ↑ Cassini opublikował te dwa odkrycia w Cassini, Giovanni Domenico: Découverte de deux nouvelles planetes autour de Saturne. Paryż: Sébastien Mabre-Cramoisy, 1673..
- ↑ Cassini opublikował te dwa odkrycia 22 kwietnia 1686. Razem z jego dwoma poprzednimi odkryciami nazwał on je Sidera Lodoicea. W swojej pracy Kosmotheôros (wydanej po jego śmierci w 1698), Christiaan Huygens pisze: „Jupiter you see has his four, and Saturn his five Moons about him, all plac’d in their Orbits.” (Jowisz widzisz ma swoje cztery, Saturn ma pięć księżyców, wszystkie ułożone na ich orbitach) (Huygens, Christiaan: Kosmotheôros. s. 113.).
- ↑ Herschel pierwszy oświadczył o odkryciu Saturna 26 kwietnia 1781, myśląc, że był on kometą: Account of a Comet. By Mr. Herschel, F. R. S.; communicated by Dr. Watson, Jun. of Bath, F. R. S.
- ↑ Po raz pierwszy oświadczył o odkryciu 24 stycznia 1801 w listach do znajomych astronomów. Pierwsza formalna publikacja odbyła się we wrześniowym wydaniu Monatliche Correspondenz w 1801 roku.
- ↑ Dawniej znana jako Hestia.
- ↑ Dawniej znana jako Hera, Heracles i Danaë.
- ↑ Dawniej znany jako Poseidon, Proserpine i Helena.
- ↑ Dawniej znany jako Hades, Cerberus i Ida.
- ↑ Dawniej znana jako Demeter, Prometeusz i Latona.
- ↑ Dawniej znany jako Pan, Daedalus i Leda.
- ↑ Dawniej znany jako Adrastea, Hephaestus i Semele.
- ↑ Został odkryty przez A. Dollfusa, ale pewność co do jego istnienia potwierdziła dopiero sonda Voyager 1.
- ↑ Dollfus zobaczył Janusa lub Epimeteusza.
- ↑ Odkryty na zdjęciach przesłanych przez sondę Voyager 1, właściwej interpretacji tychże zdjęć dokonał także Walker.
- ↑ a b c Odkryty, zgubiony i ponownie odkryty.
- ↑ Odkryty na podstawie analizy zdjęć pochodzących z sond Voyager.
- ↑ Odkryty na zdjęciach przesłanych przez sondę Cassini latem 2004 roku.
- ↑ Pierwsze fotografie zrobione przez sondę Voyager 2 w 1986 r., lecz nie rozpoznany na zdjęciach aż do 1999 r. przez Karkoschkę, potem zgubiony, a w 2003 odnaleziony ponownie przez teleskop Hubble’a.
- ↑ Został odkryty przez Matthew Holmana, Johna J. Kavelaarsa, Dana Milisavljevica i Bretta J. Gladmana 13 sierpnia 2001 roku. Potem został zgubiony i ostatecznie odnaleziony w 2003 r.
- ↑ Odkryty w 2003 r. ze zdjęć zrobionych w 2002 r.
- ↑ Odkryty ze zdjęć zrobionych w 2001 roku.
- ↑ a b Odkryty ze zdjęć zrobionych w 2003 roku.
- ↑ a b c Istnienie tego księżyca nie zostało potwierdzone, gdyż nie był obserwowany od tamtej pory.
Przypisy
- ↑ Satellite and Ring Systems. W: Jon K. Wooley: Voyages Through Space and Time. Wadsworth Pub., 1995, s. 201. ISBN 978-0-534-25002-7. (ang.)
- ↑ De Saturni luna observatio nova. Universiteit Utrecht. [dostęp 2007-05-27]. [zarchiwizowane z tego adresu (2011-11-29)].
- ↑ Herschel, W., and Watson, Dr. Account of a Comet. By Mr. Herschel, F. R. S.; Communicated by Dr. Watson, Jun. of Bath, F. R. S.. „Philosophical Transactions of the Royal Society of London”. 71, s. 492–501, 1781. Bibcode: 1781RSPT...71..492H.
- ↑ Herschel, William. An Account of the Discovery of Two Satellites revolving round the Georgian Planet. „Philosophical Transactions of the Royal Society of London”. 77, s. 125–129, 1787.
- ↑ Imago Mundi – La découverte des satellites de Saturne.
- ↑ Herschel, William. Account of the Discovery of a Sixth and Seventh Satellite of the Planet Saturn; With Remarks on the Construction of Its Ring, Its Atmosphere, Its Rotation on an Axis, and Its Spheroidical Figure. „Philosophical Transactions of the Royal Society of London”. 80, s. 1–20, 1790.
- ↑ Airy, G.B. Account of some circumstances historically connected with the discovery of the planet exterior to Uranus. „Monthly Notices of the Royal Astronomical Society”. 7, s. 121–144, 1846. Bibcode: 1846MNRAS...7..121A.
- ↑ Galle, J.G. Account of the discovery of Le Verrier’s planet Neptune. „Monthly Notices of the Royal Astronomical Society”. 7, s. 153, 1846. Bibcode: 1846MNRAS...7..153G.
- ↑ Lassell, W. Discovery of new satellite of Saturn. „Monthly Notices of the Royal Astronomical Society”. 7, s. 157, 1846. Bibcode: 1846MNRAS...7..157L.
- ↑ Lassell, W. Discovery of new satellite of Saturn. „Monthly Notices of the Royal Astronomical Society”. 8, s. 195, 1848. DOI: 10.1093/mnras/8.9.195. Bibcode: 1848MNRAS...8..195L.
- ↑ Notices respecting bequest of Dr. Pearson. „Monthly Notices of the Royal Astronomical Society”. 8, s. 163–166, 1848. Bibcode: 1848MNRAS...8R.163.
- ↑ Bond, W.C. Discovery of new satellite of Saturn. „Monthly Notices of the Royal Astronomical Society”. 9, s. 1, 1848. DOI: 10.1093/mnras/9.1.1. Bibcode: 1848MNRAS...9....1B.
- ↑ Lassell, W. Letter to the editor [discovery of two satellites of Uranus]. „Astronomical Journal”. 2 (33), s. 195, 1851. Bibcode: 1851AJ......2...70L.
- ↑ Notes. „The Observatory”. 1, s. 181–185, 1848. Bibcode: 1877Obs.....1..181..
- ↑ Hall, A. Discovery of satellites of Mars. „Monthly Notices of the Royal Astronomical Society”. 38, s. 205–209, 1877. Bibcode: 1878MNRAS..38..205H.
- ↑ Hall, A. Observations of the Satellites of Mars. „Astronomische Nachrichten”. 9 (1), s. 11–16, 1877. Bibcode: 1877AN.....91...11H.
- ↑ Barnard, E.E. Discovery and observations of a fifth satellite to Jupiter. „Astronomical Journal”. 12 (275), s. 81–85, 1892. Bibcode: 1892AJ.....12...81B.
- ↑ Pickering, E.C. Phoebe, ninth Satellite of Saturn discovered by W. W. Pickering. „Harvard College Observatory Bulletin”. 49, s. 1, 1898. Bibcode: 1899BHarO..49....1P.
- ↑ Perrine, C.D. Sixth Satellite of Jupiter (Himalia). „Harvard College Observatory Bulletin”. 173, s. 1, 1905. Bibcode: 1905BHarO.173....1P.
- ↑ Discovery of a Sixth Satellite of Jupiter. „Astronomical Journal”. 24, s. 161, 1905. Bibcode: 1905AJ.....24..160P.
- ↑ a b Perrine, C.D. Orbits of the sixth and seventh satellites of Jupiter. „Astronomische Nachrichten”. 169, s. 43, 1877. Bibcode: 1905AN....169...43P.
- ↑ Perrine, C.D. Seventh Satellite of Jupiter (Elara). „Harvard College Observatory Bulletin”. 178, s. 1, 1905. Bibcode: 1905BHarO.178....1P.
- ↑ Perrine, C.D. Seventh Satellite of Jupiter (Elara). „Publications of the Astronomical Society of the Pacific”. 17 (101), s. 62, 1905. Bibcode: 1905PASP...17...56..
- ↑ Melotte, J. Recent Observations of the Moving Object near Jupiter, discovered at Greenwich by Mr. J. Melotte. „Publications of the Astronomical Society of the Pacific”. 20 (120), s. 184–185, 1908. Bibcode: 1908PASP...20..184P.
- ↑ Note on the discovery of a moving object near Jupiter (1908 CJ), Greenwich, Royal Observatory. „Monthly Notices of the Royal Astronomical Society”. 68, s. 373, 1908. Bibcode: 1908MNRAS..68..373..
- ↑ Nicholson, S.B. Discovery of the Ninth Satellite of Jupiter. „Publications of the Astronomical Society of the Pacific”. 26 (155), s. 197–198, 1908. Bibcode: 1914PASP...26..197N.
- ↑ Tombaugh, C.W. The Search for the Ninth Planet, Pluto. „Astronomical Society of the Pacific Leaflets”. 5 (209), s. 73–80, 1946. Bibcode: 5...73T 1946ASPL 5...73T.
- ↑ a b Nicholson, S.B. Two New Satellites of Jupiter. „Publications of the Astronomical Society of the Pacific”. 50 (279), s. 292–293, 1938. Bibcode: 1938PASP...50..292N.
- ↑ Kuiper, G.P. The Fifth Satellite of Uranus. „Publications of the Astronomical Society of the Pacific”. 61 (360), s. 129, 1949. Bibcode: 1949PASP...61..129K.
- ↑ Kuiper, G.P. The Second Satellite of Neptune. „Publications of the Astronomical Society of the Pacific”. 61 (361), s. 175–176, 1949. Bibcode: 1949PASP...61..175K.
- ↑ IAUC 1212: OBJECT NEAR NEPTUNE (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ Nicholson, S.B. An Unidentified Object Near Jupiter, Probably a New Satellite. „Publications of the Astronomical Society of the Pacific”. 63 (375), s. 297–299, 1951. Bibcode: 1951PASP...63..297N.
- ↑ IAUC 1987: PROBABLE NEW SATELLITE OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 1995: SATURN X (JANUS) (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 3417: NEW RING AND Satellites OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ a b IAUC 2702: PROBABLE NEW SATELLITE OF JUPITER (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 3456: 1980 S 2 (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ a b c IAUC 3497: SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 1991: Possible NEW Sat OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ Kowal, C.T., Aksnes, K., Marsden, B.G., & Roemer, E. Thirteenth satellite of Jupiter. „Astronomical Journal”. 80, s. 460–464, 1975. Bibcode: 1975AJ.....80..460K.
- ↑ IAUC 2702: Probable NEW Satellite OF JUPITER (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 2703: Probable NEW Satellite OF JUPITER (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 2711: JUPITER XIII (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 2845: Probable NEW Satellite OF JUPITER (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 2855: Probable NEW Satellite OF JUPITER (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 2899: Probable NEW Satellite OF JUPITER (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 3241: 1978 P 1 (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ Christy, J.W.; Harrington, R.S. The satellite of Pluto. „Astronomical Journal”. 83, s. 1005, 1007, 1008, 1978. DOI: 10.1086/112284. Bibcode: 1978AJ.....83.1005C.
- ↑ Jewitt, D.C.; Danielson, G.E.; Synnott, S.P. Discovery of a new Jupiter satellite. „Science”. 206, s. 951, 1979. DOI: 10.1126/science.206.4421.951. Bibcode: 1979Sci...206..951J.
- ↑ IAUC 3454: SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 3470: Satellites OF JUPITER; Satellites OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 3507: Satellites OF JUPITER; SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ Discovery Image of Adrastea.
- ↑ a b c IAUC 3483: Satellites OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ a b c d IAUC 3496: Satellites OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ a b c d e IAUC 3534: Satellites OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ a b IAUC 3457: SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 3466: Satellites OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 3470: Satellites OF JUPITER; Satellites OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ a b IAUC 3507: Satellites OF JUPITER; SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 3539: 1980 S 28 (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ a b IAUC 3532: Satellites OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 3608: 1981 N 1 (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ a b IAUC 4824: Satellites OF NEPTUNE (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 4159: Satellites OF URANUS AND NEPTUNE (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 4164: Satellites OF URANUS (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 4165: Satellites OF URANUS (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ a b AUC 4168: Satellites AND RINGS OF URANUS (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 4806: 1989 N 1 (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 4867: NEPTUNE; JUPITER (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 5052: 1990i; SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ IAUC 6162: Possible Satellites OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ Gordon, Mitchell K.; Murray, Carl D.; Beurle, Kevin. Further evidence for the existence of additional small satellites of Saturn. „Icarus”. 121 (1), s. 114–125, 1996. DOI: 10.1006/icar.1996.0074.
- ↑ a b Brian G. Marsden: IAUC 6764: Satellites OF URANUS (ang.). W: Minor Planet Electronic Circular [on-line]. 1997-10-31.
- ↑ Daniel W.E. Green: IAUC 7171: S/1986 U 10; C/1999 J2 (ang.). W: Minor Planet Electronic Circular [on-line]. 1999-05-18.
- ↑ a b Brian G. Marsden: IAUC 7230: Probable NEW Satellites OF URANUS (ang.). W: Minor Planet Electronic Circular [on-line]. 1999-07-27.
- ↑ Brian G. Marsden: IAUC 7248: Probable NEW Satellites OF URANUS (ang.). W: Minor Planet Electronic Circular [on-line]. 1999-09-04.
- ↑ Brian G. Marsden: IAUC 7460: S/1999 J 1 (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-07-20.
- ↑ PRESS INFORMATION SHEET: NEW OUTER SATELLITE OF JUPITER DISCOVERED (ang.).
- ↑ Brian G. Marsden: IAUC 7512: S/2000 S 1, S/2000 S 2 (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-10-25.
- ↑ a b c d MPEC 2000-Y15 : S/2000 S 1, S/2000 S 2, S/2000 S 7, S/2000 S 8, S/2000 S 9 (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-12-19.
- ↑ a b IAUC 7521: S/2000 S 5, S/2000 S 6 (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-11-18.
- ↑ a b c d e Brian G. Marsden: MPEC 2000-Y14 : S/2000 S 3, S/2000 S 4, S/2000 S 5, S/2000 S 6, S/2000 S 10 (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-12-19.
- ↑ a b Brian G. Marsden: IAUC 7513: S/2000 S 3, S/2000 S 4 (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-10-25.
- ↑ a b c Brian G. Marsden: IAUC 7538: S/2000 S 7, S/2000 S 8, S/2000 S 9 (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-12-07.
- ↑ Brian G. Marsden: IAUC 7539: S/2000 S 10; OUTER Satellites OF THE GIANT PLANETS (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-12-07.
- ↑ Daniel W.E. Green: IAUC 7548: S/2000 S 12 (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-12-23.
- ↑ Brian G. Marsden: MPEC 2000-Y33 : S/2000 S 12 (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-12-22.
- ↑ Daniel W.E. Green: IAUC 7545: 2000fm; 2000fe; S/2000 S 11 (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-12-19.
- ↑ Brian G. Marsden: MPEC 2000-Y13 : S/2000 S 11 (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-12-19.
- ↑ Brian G. Marsden: IAUC 7525: S/1975 J 1 = S/2000 J 1 (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-11-25.
- ↑ Brian G. Marsden: MPEC 2000-Y16 : S/1975 J 1 = S/2000 J 1, S/1999 J 1 (ang.). W: Minor Planet Electronic Circular [on-line]. 2000-12-19.
- ↑ a b Daniel W.E. Green: IAUC 7555: Satellites OF JUPITER (ang.). W: Minor Planet Electronic Circular [on-line]. 2001-01-05.
- ↑ Marsden, Brian G: S/2000 J 2, S/2000 J 3, S/2000 J 4, S/2000 J 5, S/2000 J 6, MPEC 2001-A28 (5 January 2001) (ang.).
- ↑ Marsden, Brian G: S/2000 J 7, S/2000 J 8, S/2000 J 9, S/2000 J 10, S/2000 J 11, MPEC 2001-A29 (5 January 2001) (ang.).
- ↑ Marsden, Brian G: MPEC 2002-J54 : ELEVEN NEW SATELLITES OF JUPITER (ang.). 2002-05-15.
- ↑ Daniel W.E. Green: IAUC 7980: S/2001 U 1; S/2002 (121) 1 (ang.). W: Minor Planet Electronic Circular [on-line]. 2002-09-30.
- ↑ Marsden, Brian G: MPEC 2002-S64 : S/2001 U 1 (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ Daniel W.E. Green: IAUC 8035: S/2002 J 1 (ang.). W: Minor Planet Electronic Circular [on-line]. 2002-12-18.
- ↑ Marsden, Brian G: MPEC 2002-Y22 : S/2002 J 1 (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ Daniel W.E. Green: IAUC 8047: Satellites OF NEPTUNE (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-01-13.
- ↑ Marsden, Brian G: MPEC 2003-A75 : S/2002 N 1, 2002 N 2, 2002 N3 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-01-13.
- ↑ Daniel W.E. Green: IAUC 8087: Satellites OF JUPITER (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-03-04.
- ↑ Marsden, Brian G: MPEC 2003-E11 : S/2003 J 1, 2003 J 2, 2003 J 3, 2003 J 4, 2003 J 5, 2003 J 6, 2003 J 7 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-03-04.
- ↑ Daniel W.E. Green: IAUC 8088: S/2003 J 8 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-03-06.
- ↑ Brian G. Marsden: MPEC 2003-E15 : S/2003 J 8 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-03-06.
- ↑ Daniel W.E. Green: IAUC 8089: Satellites OF JUPITER (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-03-07.
- ↑ Brian G. Marsden: MPEC 2003-E29 : S/2003 J 9, 2003 J 10, 2003 J 11, 2003 J 12; S/2003 J 1, 2003 J 6 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-03-07.
- ↑ a b c d e Daniel W.E. Green: IAUC 8116: Satellites OF JUPITER and SATURN (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-04-11.
- ↑ a b Daniel W.E. Green: IAUC 8125: S/2003 J 19, S/2003 J 20 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-04-30.
- ↑ Brian G. Marsden: MPEC 2003-G64 : S/2003 J 19 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-04-30.
- ↑ Brian G. Marsden: MPEC 2003-G67 : S/2003 J 20 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-04-14.
- ↑ Daniel W.E. Green: IAUC 8138: S/2003 J 21 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-05-30.
- ↑ Brian G. Marsden: MPEC 2003-K45 : S/2003 J 21 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-05-29.
- ↑ Daniel W.E. Green: IAUC 8194: Satellites OF URANUS (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-09-03.
- ↑ a b Daniel W.E. Green: IAUC 8213: S/2001 U 2 and S/2002 N 4 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-10-01.
- ↑ Brian G. Marsden: MPEC 2003-S105: S/2001 U 2 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-09-30.
- ↑ Brian G. Marsden: MPEC 2003-S107: S/2002 N 4 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-09-30.
- ↑ Daniel W.E. Green: IAUC 8193: Satellites OF NEPTUNE (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-09-03.
- ↑ Brian G. Marsden: MPEC 2003-R19 : S/2003 N 1 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-09-03.
- ↑ Daniel W.E. Green: IAUC 8209: S/2003 U 1 and S/2003 U 2 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-09-25.
- ↑ Daniel W.E. Green: IAUC 8216: S/2001 U 3 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-10-07.
- ↑ Daniel W.E. Green: IAUC 8217: S/2003 U 3 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-10-09.
- ↑ Brian G. Marsden: MPEC 2003-T58 : S/2003 U 3 (ang.). W: Minor Planet Electronic Circular [on-line]. 2003-10-09.
- ↑ Daniel W.E. Green: IAUC 8276: S/2003 J 22 (ang.). W: Minor Planet Electronic Circular [on-line]. 2004-01-25.
- ↑ Brian G. Marsden: MPEC 2004-B41 : S/2003 J 22 (ang.). W: Minor Planet Electronic Circular [on-line]. 2004-01-24.
- ↑ Daniel W.E. Green: IAUC 8281: S/2003 J 23 (ang.). W: Minor Planet Electronic Circular [on-line]. 2004-02-04.
- ↑ Brian G. Marsden: MPEC 2004-B81 : S/2003 J 23 (ang.). W: Minor Planet Electronic Circular [on-line]. 2004-01-31.
- ↑ NASA/JPL/Space Science Institute: PIA06105: Cassini Uncovers New Moon. 2004-08-16.
- ↑ Daniel W.E. Green: IAUC 8389: S/2004 S 1, S/2004 S 2 (ang.). W: Minor Planet Electronic Circular [on-line]. 2004-08-16.
- ↑ a b Cassini Discovers Ring and One, Possibly Two, Objects at Saturn. NASA – Jet Propulsion Laboratory, 2004-09-09. [dostęp 2019-02-28].
- ↑ a b Daniel W.E. Green: IAUC 8401: S/2004 S 3, S/2004 S 4 and R/2004 S 1 (ang.). W: Minor Planet Electronic Circular [on-line]. 2004-09-09.
- ↑ Daniel W.E. Green: IAUC 8432: Satellites and RINGS OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line]. 2004-11-08.
- ↑ a b Twelve New Moons for Saturn. The Planetary Society. [dostęp 2007-05-29]. [zarchiwizowane z tego adresu (2006-08-31)].
- ↑ a b Jewitt, D: TWELVE NEW MOONS FOR SATURN. 2005-05-03.
- ↑ a b Daniel W.E. Green: IAUC 8523: NEW Satellites OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line]. 2005-05-04.
- ↑ a b Brian G. Marsden: MPEC 2005-J13 : TWELVE NEW SATELLITES OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line].
- ↑ Daniel W.E. Green: IAUC 8524: S/2005 S 1 (ang.). W: Minor Planet Electronic Circular [on-line]. 2005-05-06.
- ↑ Brown, Michael: Dysnomia, the moon of Eris (ang.). 2005. [dostęp 2019-02-28]. [zarchiwizowane z tego adresu (2013-12-26)].
- ↑ Daniel W.E. Green: IAUC 8625: S/2005 P 1, S/2005 P 2 (ang.). W: Minor Planet Electronic Circular [on-line]. 2005-10-31.
- ↑ Brian G. Marsden: MPEC 2006-M44 : S/2004 S 19 (ang.). W: Minor Planet Electronic Circular [on-line]. 2006-06-26.
- ↑ a b Daniel W.E. Green: IAUC 8727: Satellites OF Saturn (ang.). W: Minor Planet Electronic Circular [on-line]. 2006-06-30.
- ↑ Brian G. Marsden: MPEC 2006-M45 : EIGHT NEW SATELLITES OF SATURN (ang.). W: Minor Planet Electronic Circular [on-line]. 2006-06-26.
- ↑ Brian G. Marsden: MPEC 2007-G38 : S/2007 S 1 (ang.). W: Minor Planet Electronic Circular [on-line]. 2007-04-13.
- ↑ MPEC 2007-J09 : S/2007 S 2, S/2007 S 3 (ang.). W: Minor Planet Electronic Circular [on-line]. 2007-05-01.
- ↑ Green, Daniel W.E: IAUC 8857: S/2007 S 4 (ang.). 2007-07-18.
- ↑ Green, Daniel W.E: IAUC 9023: S/2008 S 1 (ang.). 2009-03-03.
- ↑ Green, Daniel W.E: IAUC 9091: S/2009 S 1 (ang.). 2009-11-02.
- ↑ a b Marsden, Brian G: MPEC 2011-L06 : S/2010 J 1 AND S/2010 J 2 (ang.). W: Minor Planet Electronic Circular [on-line]. 2011-06-01.
- ↑ NASA’s Hubble Discovers Another Moon Around Pluto (ang.). NASA.
- ↑ Williams, Gareth V: S/2011 J 1 and S/2011 J 2, MPEC 2012-B97 (ang.). 2012-01-29.
- ↑ Hubble Discovers a Fifth Moon Orbiting Pluto (ang.). HubbleSite News Center, 2012-07-11. [dostęp 2019-02-28].
- ↑ Planetary Satellite Discovery Circumstances (ang.). [dostęp 2013-07-16].
- ↑ Hubble Finds New Neptune Moon (ang.). Space Telescope Science Institute, 2013-07-15. [dostęp 2019-02-28].
- ↑ Hubble Discovers Moon Orbiting the Dwarf Planet Makemake (ang.). Space Telescope Science Institute, 2016-04-26. [dostęp 2019-02-28].
- ↑ Williams, Gareth V: S/2016 J 1, MPEC 2017-L08 (ang.). 2017-06-02.
- ↑ Williams, Gareth V: S/2017 J 1, MPEC 2017-L47 (ang.). 2017-06-05.
- ↑ Williams, Gareth V: S/2016 J 2, MPEC 2018-O09 (ang.). 2018-07-17.
- ↑ Williams, Gareth V: S/2016 J 2, MPEC 2018-O10 (ang.). 2018-07-17.
- ↑ Williams, Gareth V: S/2017 J 3, MPEC 2018-O11 (ang.). 2018-07-17.
- ↑ Williams, Gareth V: S/2017 J 4, MPEC 2018-O12 (ang.). 2018-07-17.
- ↑ Williams, Gareth V: S/2017 J 5, MPEC 2018-O13 (ang.). 2018-07-17.
- ↑ Williams, Gareth V: S/2017 J 6, MPEC 2018-O14 (ang.). 2018-07-17.
- ↑ Williams, Gareth V: S/2017 J 7, MPEC 2018-O15 (ang.). 2018-07-17.
- ↑ Williams, Gareth V: S/2017 J 8, MPEC 2018-O16 (ang.). 2018-07-17.
- ↑ Williams, Gareth V: S/2017 J 9, MPEC 2018-O17 (ang.). 2018-07-17.
- ↑ Williams, Gareth V: S/2018 J 1, MPEC 2018-O18 (ang.). 2018-07-17.
Linki zewnętrzne
- Gazetteer of Planetary Nomenclature (ang.)
- Scott Sheppard’s Giant Planet Satellite Page (ang.)
- Planetary Satellite Discovery Circumstances (ang.)
- James L. Hilton: When did the asteroids become minor planets? (ang.). [dostęp 2019-02-28]. [zarchiwizowane z tego adresu (2019-04-06)].
- Moons (ang.). W: Solar System Exploration [on-line]. NASA.
| Planety (☾ ∅) | |||||||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Planety karłowate | |||||||||||||||||
| Małe ciała Układu Słonecznego |
| ||||||||||||||||
- Zobacz też
- powstanie i ewolucja Układu Słonecznego
- ciała niebieskie
- lista obiektów w Układzie Słonecznym ze względu na
- Portal: Astronomia
- ciała niebieskie
Media użyte na tej stronie
Solar System XXX.png
This is a revised version of Solar_System_XXIX.png.
This is a revised version of Solar_System_XXIX.png.
Saturn PIA06077.jpg
Saturn Cassini-Huygens (NASA)
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.
Lysithea2.jpg
Lysithea in a 2MASS photograph.
Lysithea in a 2MASS photograph.
Makemake hubble.png
Photograph of Makemake taken by the Hubble Space Telescope
Photograph of Makemake taken by the Hubble Space Telescope
Anthe ring arc PIA11101.jpg
Original Caption Released with Image: Cassini images reveal the existence of a faint arc of material orbiting with Saturn's small moon Anthe.
Original Caption Released with Image: Cassini images reveal the existence of a faint arc of material orbiting with Saturn's small moon Anthe.
The moon is moving downward and to the right in this perspective. In this image, most of the visible material in the arc lies ahead of Anthe (2 kilometers, or 1 mile across) in its orbit. However, over time the moon drifts slowly back and forth with respect to the arc. The arc extends over about 20 degrees in longitude (about 5.5 percent of Anthe's orbit) and appears to be associated with a gravitational resonance caused by the moon Mimas. Micrometeoroid impacts on Anthe are the likely source of the arc material. The orbit of Anthe lies between the larger moons Mimas and Enceladus. Anthe shares this region with two other small moons, Pallene (4 kilometers, or 3 miles across) and Methone (3 kilometers, or 2 miles across). Methone also possesses an arc (see PIA11102), while Pallene is known to orbit within a faint, complete ring of its own (see PIA08328).
Cassini imaging scientists believe the process that maintains the Anthe and Methone arcs is similar to that which maintains the arc in the G ring (see PIA08327). The general brightness of the image (along with the faint horizontal banding pattern) results from the long exposure time of 32 seconds required to capture the extremely faint ring arc and the processing needed to enhance its visibility (which also enhances the digital background noise in the image). The image was digitally processed to remove most of the background noise. The long exposure also produced star trails in the background. This view looks toward the un-illuminated side of the rings from about 3 degrees above the ringplane.
The image was taken in visible light with the Cassini spacecraft narrow-angle camera on July 3, 2008. The view was obtained at a distance of approximately 1.2 million kilometers (739,000 miles) from Anthe and at a sun-Anthe-spacecraft, or phase, angle of 12 degrees. Image scale is 7 kilometers (4 miles) per pixel.
Ganymede g1 true.jpg
True color image of Ganymede, obtained by the Galileo spacecraft, with enhanced contrast.
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.
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.
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.
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.
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.
PIA11665 moonlet in B Ring.jpg
The Cassini spacecraft captured this image of a small object in the outer portion of Saturn's B ring casting a shadow on the rings as Saturn approaches its August 2009 equinox.
The Cassini spacecraft captured this image of a small object in the outer portion of Saturn's B ring casting a shadow on the rings as Saturn approaches its August 2009 equinox.
S1986U10 zoom.png
Portion de l'image S1986U10.jpg avec quatre lunes uraniennes identifiées, dont fr:S/1986 U 10
Portion de l'image S1986U10.jpg avec quatre lunes uraniennes identifiées, dont fr:S/1986 U 10
Image de la lune uranienne S/1986 U 10 saise par le télescope spatial Hubble le 25 août 2003
Source : NASA
http://www.solarviews.com/cap/uranus/1986u10.htm
Kerberos (moon).jpg
Four combined images of Kerberos taken by the Long Range Reconnaissance Imager (LORRI) instrument on 14 July, approximately 7 hours before New Horizons’ closest approach to Pluto and at a distance of 396 100 km from Kerberos.
Four combined images of Kerberos taken by the Long Range Reconnaissance Imager (LORRI) instrument on 14 July, approximately 7 hours before New Horizons’ closest approach to Pluto and at a distance of 396 100 km from Kerberos.
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.
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.
Saturn-cassini-March-27-2004.jpg
Saturn Cassini-Huygens (NASA)
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.
Prometheus 12-26-09b.jpg
This raw, unprocessed image of Prometheus was taken by Cassini on Dec. 26, 2009.
The image was taken in visible light with the Cassini spacecraft narrow-angle camera on Dec. 26, 2009 at a distance of approximately 79,000 kilometers (49,000 miles) from Prometheus and at a Sun-Prometheus-spacecraft, or phase, angle of 18 degrees. Image scale is 474 meters (1,556 feet) per pixel.
The Cassini Equinox Mission is a joint United States and European endeavor. 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 was designed, developed and assembled at JPL. The imaging team consists of scientists from the US, England, France, and Germany. The imaging operations center and team lead (Dr. C. Porco) are based at the Space Science Institute in Boulder, Colo.
For more information about the Cassini Equinox Mission visit http://ciclops.org, http://www.nasa.gov/cassini and http://saturn.jpl.nasa.gov.
The original NASA image has been modified by cropping and doubling the linear pixel density.
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.
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.
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.
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.
Rsz 800px-aegaeon (2008 s1).jpg
Autor: own work, Licencja: CC BY 3.0
croped from File:Aegaeon (2008 S1).jpg, which is the original
Autor: own work, Licencja: CC BY 3.0
croped from File:Aegaeon (2008 S1).jpg, which is the original
Inset-ura bianca-large.gif
Bianca - moon of Uranus
Bianca - moon of Uranus
Caliban feat.png
Caliban, moon of Uranus
Caliban, moon of Uranus
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.
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.
Pan by Cassini, March 2017.jpg
View of the ring shepherd Saturnian moon of Pan, taken from above its northern hemisphere on 7 March 2017 by the Cassini spacecraft. This is a crop of an image by the CL1 and CL2 filters of the Narrow-Angle Imaging Science Subsystem camera, N00277980, that was received on Earth on 8 March.
View of the ring shepherd Saturnian moon of Pan, taken from above its northern hemisphere on 7 March 2017 by the Cassini spacecraft. This is a crop of an image by the CL1 and CL2 filters of the Narrow-Angle Imaging Science Subsystem camera, N00277980, that was received on Earth on 8 March.
N00163156.jpg
N00163156.jpg was taken on September 13, 2010 and received on Earth September 15, 2010. The camera was pointing toward PALLENE, and the image was taken using the CL1 and CL2 filters. This image has not been validated or calibrated. A validated/calibrated image will be archived with the NASA Planetary Data System in 2011
N00163156.jpg was taken on September 13, 2010 and received on Earth September 15, 2010. The camera was pointing toward PALLENE, and the image was taken using the CL1 and CL2 filters. This image has not been validated or calibrated. A validated/calibrated image will be archived with the NASA Planetary Data System in 2011
Cassini Helene N00086698 CL.jpg
Raw Narrow Angle Camera image of Helene. Taken by Cassini-Huygens on July 20, 2007 from 40,211 km with clear filters. Adapted from source image (cropped and contrast adjusted).
Raw Narrow Angle Camera image of Helene. Taken by Cassini-Huygens on July 20, 2007 from 40,211 km with clear filters. Adapted from source image (cropped and contrast adjusted).
Triton moon mosaic Voyager 2 (large).jpg
Global Color Mosaic of Triton, taken by Voyager 2 in 1989
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.
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.
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.
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.
Sycorax.jpg
This shows the discovery image of brighter of the two new moons of Uranus. It is designated as Sycorax (S/1997 U 2) and later names Sycorax. Notice the motion of the moon (circled) with respect to the background stars. The images were taken roughly one hour apart on September 7, 1997. A faint asteroid in the main belt (not circled) may also be observed and identified by its much faster rate of motion.
This shows the discovery image of brighter of the two new moons of Uranus. It is designated as Sycorax (S/1997 U 2) and later names Sycorax. Notice the motion of the moon (circled) with respect to the background stars. The images were taken roughly one hour apart on September 7, 1997. A faint asteroid in the main belt (not circled) may also be observed and identified by its much faster rate of motion.
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.
"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.
Amalthea PIA02532.png
Amalthea, as photographed by the Galileo spacecraft. The left photograph is from August 12, 1999 at a range of 446,000 kilometers. The right photo is from November 26, 1999 at a range of 374,000.
Amalthea, as photographed by the Galileo spacecraft. The left photograph is from August 12, 1999 at a range of 446,000 kilometers. The right photo is from November 26, 1999 at a range of 374,000.
S-2004 N1 Hubble montage.jpg
This composite Hubble Space Telescope picture shows the location of a newly discovered moon, designated S/2004 N 1, orbiting the giant planet Neptune. The moon is so small (no more than 12 miles across) and dim, it was missed by NASA's Voyager 2 spacecraft cameras when the probe flew by Neptune in 1989. Several other moons that were discovered by Voyager appear in this 2009 image, along with a circumplanetary structure known as ring arcs.
Mark Showalter of the SETI Institute discovered S/2004 N 1 in July 2013. He analyzed over 150 archival Neptune photographs taken by Hubble from 2004 to 2009. The same white dot appeared over and over again. He then plotted a circular orbit for the moon, which completes one revolution around Neptune every 23 hours. The black-and-white image was taken in 2009 with Hubble's Wide Field Camera 3 in visible light. Hubble took the color inset of Neptune on August 19, 2009.
This composite Hubble Space Telescope picture shows the location of a newly discovered moon, designated S/2004 N 1, orbiting the giant planet Neptune. The moon is so small (no more than 12 miles across) and dim, it was missed by NASA's Voyager 2 spacecraft cameras when the probe flew by Neptune in 1989. Several other moons that were discovered by Voyager appear in this 2009 image, along with a circumplanetary structure known as ring arcs.
Mark Showalter of the SETI Institute discovered S/2004 N 1 in July 2013. He analyzed over 150 archival Neptune photographs taken by Hubble from 2004 to 2009. The same white dot appeared over and over again. He then plotted a circular orbit for the moon, which completes one revolution around Neptune every 23 hours. The black-and-white image was taken in 2009 with Hubble's Wide Field Camera 3 in visible light. Hubble took the color inset of Neptune on August 19, 2009.
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.
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.
S 2000 J 1.jpg
Autor: IMCCE (Institut de mécanique céleste et de calcul des éphémérides) / University of Hawaii, Licencja: CC BY-SA 2.0 fr
Montage of the rediscovery images of S/2000 J 1 (Themisto, Jupiter XVIII), taken on 21 November 2000 with the 2.2 m U. of Hawaii telescope. The field is 70 arc-seconds wide. The three images, taken 40 minutes apart, are superposed. S/2000 J 1 (arrows) moves from right to left during that time.
Autor: IMCCE (Institut de mécanique céleste et de calcul des éphémérides) / University of Hawaii, Licencja: CC BY-SA 2.0 fr
Montage of the rediscovery images of S/2000 J 1 (Themisto, Jupiter XVIII), taken on 21 November 2000 with the 2.2 m U. of Hawaii telescope. The field is 70 arc-seconds wide. The three images, taken 40 minutes apart, are superposed. S/2000 J 1 (arrows) moves from right to left during that time.
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.
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.
Adrastea.jpg
Adrastea—the moon of Jupiter by Galileo
Adrastea—the moon of Jupiter by Galileo
Nereid-Voyager2.jpg
衛星ネレイド、ボイジャー2号の撮影
衛星ネレイド、ボイジャー2号の撮影
Uranus moon 021002 02.jpg
Three images showing the Uranian satellite S/2001 U2 (Ferdinand). The full CTIO observation set are sub-divided into three batches that were shifted at the rate and direction of the motion of Uranus and then recombined. The satellite is indicated by the circle in each image and can be seen moving from left to right. The elongated features in the images are stars that have been smeared out by the shifting process.
Three images showing the Uranian satellite S/2001 U2 (Ferdinand). The full CTIO observation set are sub-divided into three batches that were shifted at the rate and direction of the motion of Uranus and then recombined. The satellite is indicated by the circle in each image and can be seen moving from left to right. The elongated features in the images are stars that have been smeared out by the shifting process.
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.
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.
Daphnis raw 2010 cropped.jpg
This image was taken on July 05, 2010 and received on Earth July 06, 2010. The camera was pointing toward DAPHNIS, and the image was taken using the CL1 and CL2 filters. This image has not been validated or calibrated. A validated/calibrated image will be archived with the NASA Planetary Data System in 2011.
This image was taken on July 05, 2010 and received on Earth July 06, 2010. The camera was pointing toward DAPHNIS, and the image was taken using the CL1 and CL2 filters. This image has not been validated or calibrated. A validated/calibrated image will be archived with the NASA Planetary Data System in 2011.
Ceresintruecolor.png
Ceres in true color taken by Dawn on May 4, 2015. Oxo Crater, Haulani Crater, and Ahuna Mons are visible.
Ceres in true color taken by Dawn on May 4, 2015. Oxo Crater, Haulani Crater, and Ahuna Mons are visible.
Carmé.jpg
Autor: OHP (Observatoire de Haute-Provence) / CNRS (Centre national de la recherche scientifique) / IMCCE (Institut de mécanique céleste et de calcul des éphémérides), Licencja: CC BY-SA 2.0 fr
Carme (Jupiter XI) photographed by the OHP (Observatoire de Haute-Provence) on 16 December 1998 at 18h32 UTC. Jupiter's glare comes from the lower right.
Autor: OHP (Observatoire de Haute-Provence) / CNRS (Centre national de la recherche scientifique) / IMCCE (Institut de mécanique céleste et de calcul des éphémérides), Licencja: CC BY-SA 2.0 fr
Carme (Jupiter XI) photographed by the OHP (Observatoire de Haute-Provence) on 16 December 1998 at 18h32 UTC. Jupiter's glare comes from the lower right.
Elara2-LB1-mag17.jpg
(c) I, Kevin Heider, CC BY-SA 3.0
2 minute exposure of Jupiter's moon Elara with a 24" telescope. Elara is apparent magnitude 16.8 in this image taken at 2009-10-21 03:00 UT. The glow at the bottom of the image is from Jupiter (which is not in the photo).
(c) I, Kevin Heider, CC BY-SA 3.0
2 minute exposure of Jupiter's moon Elara with a 24" telescope. Elara is apparent magnitude 16.8 in this image taken at 2009-10-21 03:00 UT. The glow at the bottom of the image is from Jupiter (which is not in the photo).
Polydeuces.jpg
Polydeuces, moon of Saturn
Polydeuces, moon of Saturn
Uranus' moon puck.gif
Autor: NASA, Licencja: CC-BY-SA-3.0
Heavily processed version of image taken by the Voyager 2 spacecraft on January 24th, 1986, from a distance of 493,000 km. The satellite is about 130 km across in this image and the rotation axis is vertical.
Autor: NASA, Licencja: CC-BY-SA-3.0
Heavily processed version of image taken by the Voyager 2 spacecraft on January 24th, 1986, from a distance of 493,000 km. The satellite is about 130 km across in this image and the rotation axis is vertical.
Larissa.jpg
These Voyager 2 images of satellite Larissa 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 Proteus. 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.
These Voyager 2 images of satellite Larissa 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 Proteus. 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.
Makemake moon Hubble image with legend (cropped).jpg
Dwarf planet Makemake and its moon S/2015 (136472) 1.
Dwarf planet Makemake and its moon S/2015 (136472) 1.
Charon by New Horizons on 13 July 2015.png
Charon, taken by New Horizons late on 13 July 2015
Charon, taken by New Horizons late on 13 July 2015
Proteus Voyager 2 (big).jpg
This image of Neptune's satellite 1989N1 was obtained on Aug. 25, 1989 from a range of 146,000 kilometers (91,000 miles) by Voyager 2. 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. The Voyager Mission is conducted by JPL for NASA's Office of Space
Science and Applications.
Styx (moon).jpg
Image(s) of Styx taken by the Long Range Reconnaissance Imager (LORRI) on 13 July, approximately 12.5 hours before New Horizons’ closest approach to Pluto.
Image(s) of Styx taken by the Long Range Reconnaissance Imager (LORRI) on 13 July, approximately 12.5 hours before New Horizons’ closest approach to Pluto.
_from_Voyager_1.jpg)
Rhea (moon) thumb.jpg
This image of Rhea was acquired by the Voyager 1 spacecraft on November 11, 1980.
This image of Rhea was acquired by the Voyager 1 spacecraft on November 11, 1980.
N00151485 Calypso crop.jpg
Cassini narrow-angle camera raw image N00151485.jpg was taken on February 13, 2010 and received on Earth February 14, 2010. The camera was pointing toward CALYPSO, and the image was taken using the CL1 and GRN filters. This image has not been validated or calibrated. A validated/calibrated image will be archived with the NASA Planetary Data System in 2011.
The original NASA image has been modified by cropping, doubling the linear pixel density and sharpening.
Cassini narrow-angle camera raw image N00151485.jpg was taken on February 13, 2010 and received on Earth February 14, 2010. The camera was pointing toward CALYPSO, and the image was taken using the CL1 and GRN filters. This image has not been validated or calibrated. A validated/calibrated image will be archived with the NASA Planetary Data System in 2011.
The original NASA image has been modified by cropping, doubling the linear pixel density and sharpening.
Cassini Atlas N00084634 CL.png
Narrow Angle Camera image of Atlas. Adapted from source images. Imaged from 181,000 km with clear filters, about 1km per pixel.
Narrow Angle Camera image of Atlas. Adapted from source images. Imaged from 181,000 km with clear filters, about 1km per pixel.
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.
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.
Hydra imaged by the LORRI instrument aboard the New Horizons spacecraft on 14 July.
Hyperion true.jpg
Approximately true-color mosaic of Saturn's moon Hyperion. Composed of several narrow-angle frames and processed to match Hyperion's natural color. Taken during Cassini's flyby of this lumpy moon on 26th September 2005.
Approximately true-color mosaic of Saturn's moon Hyperion. Composed of several narrow-angle frames and processed to match Hyperion's natural color. Taken during Cassini's flyby of this lumpy moon on 26th September 2005.
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.
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.
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.
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.
Neptune Trio.jpg
A Voyager 2 image of Thalassa (1989 N5), Naiad (1989 N6) and Despina (1989 N3) taken in 1989 at a range of 5.9 million km (3.6 million miles). The high orbital speed of the moons caused faint streaks in this exposure.
A Voyager 2 image of Thalassa (1989 N5), Naiad (1989 N6) and Despina (1989 N3) taken in 1989 at a range of 5.9 million km (3.6 million miles). The high orbital speed of the moons caused faint streaks in this exposure.
Ερμίππη.gif
Discovery images of the Jupiter satellite S/2001 J3, later named Hermippe. It was discovered by Scott S. Sheppard and David Jewitt in 2001.
Discovery images of the Jupiter satellite S/2001 J3, later named Hermippe. It was discovered by Scott S. Sheppard and David Jewitt in 2001.
Phobos colour 2008.jpg
Kolorowa fotografia Fobosa, księżyca Marsa, wykonana przez sondę Mars Reconnaissance Orbiter w dniu 23 marca 2008 roku.
Kolorowa fotografia Fobosa, księżyca Marsa, wykonana przez sondę Mars Reconnaissance Orbiter w dniu 23 marca 2008 roku.
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.
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
PLUTO - NEW HORIZONS - July 14, 2015
ORIGINAL IMAGE DESCRIPTION:
Four images from New Horizons’ Long 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.
Belinda.gif
벨린다.
벨린다.
Propozycja LnM-2.svg
Autor:
Propozycja 1 dla Listy na Medal na PL.WIKI
Autor:
- Propozycja LnM.svg od M.Komorniczak
- derivative work: Michał Komorniczak (dyskusja)
Propozycja 1 dla Listy na Medal na PL.WIKI
Phoebe cassini.jpg
Phoebe, as imaged by the Cassini probe.
Phoebe, as imaged by the Cassini probe.
Methone - Best Image From Cassini.jpg
N00189072.jpg was taken on May 20, 2012 and received on Earth May 21, 2012. The camera was pointing toward METHONE, and the image was taken using the CL1 and CL2 filters. This image has not been validated or calibrated. A validated/calibrated image will be archived with the NASA Planetary Data System in 2013. Image rotated so that north is up. Original image had a pixel scale of 26.72 meters per pixel, but this has been enlarged by 2x to improve feature visibility.
N00189072.jpg was taken on May 20, 2012 and received on Earth May 21, 2012. The camera was pointing toward METHONE, and the image was taken using the CL1 and CL2 filters. This image has not been validated or calibrated. A validated/calibrated image will be archived with the NASA Planetary Data System in 2013. Image rotated so that north is up. Original image had a pixel scale of 26.72 meters per pixel, but this has been enlarged by 2x to improve feature visibility.
Sinopé.jpg
Autor: OHP (Observatoire de Haute-Provence) / CNRS (Centre national de la recherche scientifique) / IMCCE (Institut de mécanique céleste et de calcul des éphémérides), Licencja: CC BY-SA 2.0 fr
Sinope (Jupiter IX) photographed by the OHP (Observatoire de Haute-Provence) on 14 August 1998 at 22h45 UTC. Jupiter is off frame.
Autor: OHP (Observatoire de Haute-Provence) / CNRS (Centre national de la recherche scientifique) / IMCCE (Institut de mécanique céleste et de calcul des éphémérides), Licencja: CC BY-SA 2.0 fr
Sinope (Jupiter IX) photographed by the OHP (Observatoire de Haute-Provence) on 14 August 1998 at 22h45 UTC. Jupiter is off frame.
Nix in Color Released September 11 2015.png
Pluto's moon Nix, with color processing from the Ralph MVIC.
Pluto's moon Nix, with color processing from the Ralph MVIC.
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.
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.
S1999j1.jpg
Autor: Spacewatch/University of Arizona, Licencja: CC BY-SA 4.0
Callirrhoe (S/1999 J1) was discovered by the Spacewatch project and the Minor Planet Center in 2000 from images taken in 1999.
Autor: Spacewatch/University of Arizona, Licencja: CC BY-SA 4.0
Callirrhoe (S/1999 J1) was discovered by the Spacewatch project and the Minor Planet Center in 2000 from images taken in 1999.
Pasiphaé.jpg
Autor: OHP (Observatoire de Haute-Provence) / CNRS (Centre national de la recherche scientifique) / IMCCE (Institut de mécanique céleste et de calcul des éphémérides), Licencja: CC BY 3.0
Pasiphaë (Jupiter VIII) photographed by the OHP (Observatoire de Haute-Provence) on 20 August 1998 at 22h34 UTC. Jupiter is off frame.
Autor: OHP (Observatoire de Haute-Provence) / CNRS (Centre national de la recherche scientifique) / IMCCE (Institut de mécanique céleste et de calcul des éphémérides), Licencja: CC BY 3.0
Pasiphaë (Jupiter VIII) photographed by the OHP (Observatoire de Haute-Provence) on 20 August 1998 at 22h34 UTC. Jupiter is off frame.