PICT0037

Ć1.ASSIFICATION OF PLANETARY SATELLITES (ACCORDING TO ORBITAL DYNAMICS)

(Burns: Satellites. Turion Univ. Arizona Press. 1986)

REGULAR SATELLITES: most typically originated from accretion of cireumplaneiary fbdi The orfoits are nearty circa lar and Ue dose to planets* equators.

4    Galiłean satellites of Jupiter: lo, Europa, Ganimede, Callisto

8 Saturnian satellites:    Mimas, Enceladus, Tethys, Dionc, Rhea, Ti tan.

Hiperion, lapetus

5    Uranian satellites: Miranda, Ariel, Umbriel, Titania, Oberon

COLLISIONAL SHARDS:

Mnrtian satellites: Phobosand Dcinios (included by elimination)

Jovinn satellites: Amalthea, Andrastca, Thcbe, Metis

Saturnian satellites: coorbital pair Janus - Epimetheus, F ring shepards

and 3 Lagrangian satellites ofTcthys and Dione Smali Uranian and Neptunian satellites.

IRREGULAR SATELLITES: elongated orbits. retrograde and/or highly inclined orbits (in some cases)

e= 0.05490

<e>« 0.15 <e> - 0.25

e = 0.163

ę ■ 0.0000

e i 0.75 e- 0.0076

i- 5.15*

<i>- 28*

<*>" 150° (ret r.)

»= 1753* (retr.) i- 156.8* (retr.)

•= 27.6*

1= 96.16*

The Earth’s Moon Jovian satellites (captured):

Innergroup of 4 (160 Rj) Outer group of 4 (310 Rj) Phoebe (Saturnian satełlite) Triton (Neptunian satełlite) Nereid (Neptunian satełlite) Charon