Razlika između verzija stranice "Miranda (mjesec)"
[nepregledana izmjena] | [nepregledana izmjena] |
No edit summary |
No edit summary |
||
Red 34: | Red 34: | ||
| 471.6 km<br/>(480×468.4×465.8 km) |
| 471.6 km<br/>(480×468.4×465.8 km) |
||
|- |
|- |
||
! align="left" | |
! align="left" | [[Površina]] |
||
| 2,790,000 |
| 2,790,000 kvadratni kilometar|km<sup>2</sup> |
||
|- |
|- |
||
! align="left" | [[ |
! align="left" | [[Volumen]] |
||
| 54,835,000 |
| 54,835,000 kubni kilometar|km<sup>3</sup> |
||
|- |
|- |
||
! align="left" | [[ |
! align="left" | [[Masa]] |
||
| 6.59×10<sup>19</sup> [[kilogram|kg]] |
| 6.59×10<sup>19</sup> [[kilogram|kg]] |
||
|- |
|- |
Verzija na dan 3 oktobar 2005 u 15:48
Otkriće | |||||||
---|---|---|---|---|---|---|---|
Otkrio | Gerard P. Kuipera | ||||||
Datum otkrića | 16. februar, 1948 | ||||||
Orbitalne karakteristike | |||||||
Srednji radijus | 129,872 km | ||||||
Eccentricity | 0.0013 | ||||||
Orbitalni period | 1.413479 d | ||||||
Inklinacija | 4.232° (to Uranus' equator) | ||||||
Is a satellite of | Uranus | ||||||
Physical characteristics | |||||||
Mean diameter | 471.6 km (480×468.4×465.8 km) | ||||||
Površina | km2 | ||||||
Volumen | km3 | ||||||
Masa | 6.59×1019 kg | ||||||
Mean density | 1.20 g/cm3 | ||||||
Surface gravity | 0.079 m/s2 | ||||||
Escape velocity | 0.19 km/s | ||||||
Rotation period | synchronous | ||||||
Axial tilt | zero | ||||||
Albedo | 0.32 | ||||||
Temperatura na površini |
| ||||||
Atmosferski pritisak | 0 kPa |
Miranda (mi-ran'-da) je prirodni satelit planete Uran, najmanji i najbliži planeti od svih njenih većih satelita.
Otkrio ju je Gerard Kuiper 2. februara1948 u Fort Davisu. Dobila je ime po kćerki Prospera u Šekspirovom komadu The Tempest. Također je nazvana Uranus V.
Dosada, jedine slike Mirande izbliza su one koje je načinio Voyager 2, koji je prošao pored Urana u januaru 1986, i tom prilikom izvršio i osmatranje njegovih satelita. Prilikom prolijetanja južna hemisfera mjeseca je bila okrenuta prema Suncu, tako da je samo ona i bila predmet istraživanja. Srećna je okolnost to da je Miranda prošla jako blizu Voyagera pokazujući da se radi o geološki najaktivnijem tijelu u Uranovom sistemu.
Fizikalne karakteristike
Miranda's surface may be mostly water ice, with the low density body being made of silicate rock and methane-related organic compounds. Miranda's surface is criss-crossed by huge canyons up to 20 kilometres (12 miles) deep, with patchwork regions of broken terrain indicating intense geological activity in the moon's past. Large grooved structures, called coronae, may be the result of upwelling warm ice. It is thought that this activity is powered by tidal forces from Uranus. Another theory, now considered less likely, suggests that Miranda was at some point struck by a massive object that shattered the moon. Fragments then resettled into different positions forming the current strange pattern.
Miranda's orbital inclination (4.34°) is unusually high for a body so close to the planet. It is possible that it was at some point in a 3:1 orbital resonance with Umbriel. Resulting tidal friction may also have caused warming within the moon and thus be the culprit of the geological activity.
Scientists recognize the following geological features on Miranda:
- Craters
- Coronae (large ovoid features)
- Regiones (geological regions)
- Rupes (scarps)
- Sulci (parallel grooves)