Erinevus lehekülje "Phobos" redaktsioonide vahel

Eemaldatud 22 baiti ,  6 aasta eest
 
==Füüsilised karakteristikud==
Phobose mõõtmed on {{nowrap|27 × 22 × 18 km}} ning ta on liiga väike, selleks et muutuda ümaraks iseenda gravitatsiooni toimel. Phobose pindala on 1548.3 km<sup>2</sup>, mis on umbkaudu midagi [[Saaremaa]] ja [[Hiiumaa]] pindala vahepealset. Phobosel puudub oma väikse massi ja gravitatsiooni tõttu atmosfäär.<ref>{{cite web|url=http://solarsystem.nasa.gov/planets/profile.cfm?Object=Mar_Phobos |title=Solar System Exploration: Planets: Mars: Moons: Phobos: Overview |publisher=Solarsystem.nasa.gov |accessdate=19 August 2013}}</ref> Ka on ta üks kõige vähem valgust peegeldav objekt päikesesüsteemis. Spektroskoopiliselt paistab ta olevat sarnane [[D-tüüpi asteroidid]]ega,<ref name="c-type">{{cite web|url=http://www.physorg.com/news115483748.html|title=New Views of Martian Moons}}</ref> andja ison apparentlykoostisel ofilmselt compositionsarnane similar to [[carbonaceous chondritesüsinikkondriit]] materialidega.<ref>{{Cite book|title=Physics and Chemistry of the Solar System|last=Lewis|first=J. S.|authorlink=John S. Lewis|page=425|publisher=Elsevier Academic Press|year=2004|isbn=0-12-446744-X}}</ref> Phobose tihedus on liiga väike, et ta oleks üks monoliitne kivikamakas ja teatakse et ta on märkimisväärselt poorne.<ref>{{cite web|title=Porosity of Small Bodies and a Reassesment of Ida's Density|url=http://www.aas.org/publications/baas/v31n4/dps99/65.htm|quote=When the error bars are taken into account, only one of these, Phobos, has a porosity below 0.2...}}</ref><ref name="Close Inspection for Phobos">{{cite web|title=Close Inspection for Phobos|url=http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=31031|quote=It is light, with a density less than twice that of water, and orbits just {{Convert|5989|km|sp=us}} above the Martian surface.}}</ref><ref>{{Cite journal|last=Busch|first=M. W.|coauthors=''et al.''|year=2007|title=Arecibo Radar Observations of Phobos and Deimos|journal=Icarus|volume=186|issue=2|pages=581–584|doi=10.1016/j.icarus.2006.11.003|bibcode=2007Icar..186..581B}}</ref> Need andmed on viinud oletusele, et Phobos võib sisaldada palju jääd. Spektraalne vaatlus siiski näitab, et Phobose pinnal leiduv regoliit pole hüdratiseerunud,<ref>{{Cite journal|last=Murchie|first=S. L.|coauthors= Erard, S., Langevin, Y., Britt, D. T., Bibring, J. P., and Mustard, J. F.|title=Disk-resolved Spectral Reflectance Properties of Phobos from 0.3-3.2 microns: Preliminary Integrated Results from PhobosH 2 |journal=Abstracts of the Lunar and Planetary Science Conference| volume=22|page=943|year=1991 |bibcode=
1991pggp.rept..249M}}</ref><ref>{{Cite journal|last=Rivkin|first=A. S.|coauthors=''et al.''|date=March 2002|title=Near-Infrared Spectrophotometry of Phobos and Deimos|journal=Icarus|volume=156|issue=1|page=64|bibcode=2002Icar..156...64R|doi=10.1006/icar.2001.6767}}</ref> kuid jää olemasolu regoliidi kihi all pole seetõttu siiski välistatud.<ref>{{ cite journal | last1 = Fanale | first1 = F. P. | first2 = J. R. | last2 = Salvail | year = 1989 | title = Loss of water from Phobos | journal = Geophys. Res. Lett. | volume = 16 | number = 4 | pages = 287–290 | doi = 10.1029/GL016i004p00287 |bibcode = 1989GeoRL..16..287F }}</ref><ref>{{ cite journal | title = Evolution of the water regime of Phobos | first1 = Fraser P. |last1 = Fanale | first2 = James R. | last2 = Salvail | doi = 10.1016/0019-1035(90)90089-R | date = Dec 1990 | journal = Icarus | volume = 88 | pages = 380–395 |bibcode = 1990Icar...88..380F }}</ref>
 
On võimalik, et 3. detsembril 1980 [[Jeemen]]isse kukkunud [[Kaiduni meteoriit]] on tükk Phobosest, kuid seda on raske tõestada, kuna Phobose koostise kohta on liiga vähe teada.<ref>{{Cite journal| last=Ivanov| first=Andrei V.| bibcode=2004SoSyR..38...97I| title=Is the Kaidun Meteorite a Sample from Phobos?|date=March 2004| journal=Solar System Research| volume=38| issue=2| pages=97–107| doi=10.1023/B:SOLS.0000022821.22821.84}}</ref><ref>{{Cite journal|last=Ivanov | first=Andrei | coauthors=Michael Zolensky | title=The Kaidun Meteorite: Where Did It Come From?|url=http://www.lpi.usra.edu/meetings/lpsc2003/pdf/1236.pdf|journal=Lunar and Planetary Science | year=2003 |volume=34 | quote=The currently available data on the lithologic composition of the Kaidun meteorite– primarily the composition of the main portion of the meteorite, corresponding to CR2 carbonaceous chondrites and the presence of clasts of deeply differentiated rock&nbsp;– provide weighty support for considering the meteorite’s parent body to be a carbonaceous chondrite satellite of a large differentiated planet. The only possible candidates in the modern solar system are Phobos and Deimos, the moons of Mars.|format=PDF}}</ref>
 
 
==Viited==