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Red 4: Red 4:
| bgcolor="010101" colspan="2" align="center" | [[Image:Miranda.jpg|250px|Miranda]]
| bgcolor="010101" colspan="2" align="center" | [[Image:Miranda.jpg|250px|Miranda]]
|-
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! bgcolor="#ffc0c0" colspan="2" | Discovery
! bgcolor="#ffc0c0" colspan="2" | Otkriće
|-
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! align="left" | Otkrio
! align="left" | Otkrio
Red 14: Red 14:
! bgcolor="#ffc0c0" colspan="2" | Orbitalne karakteristike
! bgcolor="#ffc0c0" colspan="2" | Orbitalne karakteristike
|-
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! align="left" | Mean [[radius]]
! align="left" | Srednji [[radijus]]
| 129,872 [[kilometre|km]]
| 129,872 [[kilometar|km]]
|-
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! align="left" | [[Eccentricity (orbit)|Eccentricity]]
! align="left" | [[Eccentricity (orbit)|Eccentricity]]

Verzija na dan 3 oktobar 2005 u 13:36

Miranda
Miranda
Otkriće
Otkrio Gerard P. Kuipera
Datum otkrića 16. februar, 1948
Orbitalne karakteristike
Srednji radijus 129,872 km
Eccentricity 0.0013
Orbital period 1.413479 d
Inclination 4.232° (to Uranus' equator)
Is a satellite of Uranus
Physical characteristics
Mean diameter 471.6 km
(480×468.4×465.8 km)
Surface area 2,790,000 km2
Volume 54,835,000 km3
Mass 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
Surface temp.
min mean max
? K ~59 K 86 K
Atmospheric pressure 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

Pogled izbliza na Verona Rupes, veliki kosi rasjed na Mirandi; sa svojih 20 km visine to je najviša litica u solarnom sistemu

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:

See also

External links