Exoplaneta : Diferéncia entre versions

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Un '''exoplaneta''' o '''planeta extrasolar''' es un [[planeta]] situat en defòra del [[Sistèma Solar]]. La primièra pròva d'un exoplaneta foguèt notada en 1917, mas foguèt pas reconeguda coma tala. Pasmens, la primièra deteccion scientifica d'un exoplaneta se faguèt en 1988, e mai que foguèsse pas confirmats coma essent un exoplaneta abans 2012. En 2018, i a aperaquí 3900 exoplanetas confirmats dins 2900 sistèmas planetaris descobèrts.
Existisson mai d'un metòdes de deteccion dels exoplanetas. Lo [[Cercador de Planetas per Velocitat Radiala de Nauta Precision]] o HARPS (acronim en anglés) descobriguèt aperaquí cent exoplanetas dempuèi 2004, mentre que lo [[Kepler (telescòpi espacial)|telescòpi espacial ''Kepler'']], dempuèi 2009, ne trobèt mai de dos mila. ''Kepler'' detectèt tanben mantun milièrs<ref name=keplersite>{{cite web |title=Kepler |url=http://www.nasa.gov/mission_pages/kepler/main/index.html |archive-url=https://web.archive.org/web/20131105082102/http://www.nasa.gov/mission_pages/kepler/main/index.html |archive-date=5 November 2013 |publisher=NASA |website=nasa.gov |author=Jerry Colen |access-date=4 November 2013 |date=4 November 2013}}</ref><ref name="usher">{{cite web |last1=Harrington |first1=J. D.
|last2=Johnson |first2=M. |date=4 November 2013 |title=NASA Kepler Results Usher in a New Era of Astronomy |url=http://www.nasa.gov/press/2013/november/nasa-kepler-results-usher-in-a-new-era-of-astronomy/}}</ref> de planetas candidatascandidats,<ref>{{Cite journal | doi = 10.1088/0067-0049/206/1/5|arxiv=1212.2915| title = Detection of Potential Transit Signals in the First 12 Quarters of ''Kepler'' Mission Data| journal = The Astrophysical Journal Supplement Series| volume = 206|issue=1| page = 5| year = 2013| last1 = Tenenbaum | first1 = P. | last2 = Jenkins | first2 = J. M. | last3 = Seader | first3 = S. | last4 = Burke | first4 = C. J. | last5 = Christiansen | first5 = J. L. | last6 = Rowe | first6 = J. F. | last7 = Caldwell | first7 = D. A. | last8 = Clarke | first8 = B. D. | last9 = Li | first9 = J. | last10 = Quintana | first10 = E. V. | last11 = Smith | first11 = J. C. | last12 = Thompson | first12 = S. E. | last13 = Twicken | first13 = J. D. | last14 = Borucki | first14 = W. J. | last15 = Batalha | first15 = N. M. | last16 = Cote | first16 = M. T. | last17 = Haas | first17 = M. R. | last18 = Hunter | first18 = R. C. | last19 = Sanderfer | first19 = D. T. | last20 = Girouard | first20 = F. R. | last21 = Hall | first21 = J. R. | last22 = Ibrahim | first22 = K. | last23 = Klaus | first23 = T. C. | last24 = McCauliff | first24 = S. D. | last25 = Middour | first25 = C. K. | last26 = Sabale | first26 = A. | last27 = Uddin | first27 = A. K. | last28 = Wohler | first28 = B. | last29 = Barclay | first29 = T. | last30 = Still | first30 = M. |bibcode=2013ApJS..206....5T}}</ref> que mai de 40% son benlèu de falsas positivas.<ref>{{cite journal |arxiv=1310.2133 |last1=Santerne |first1=A. |last2=Díaz |first2=R. F. |last3=Almenara |first3=J.-M. |last4=Lethuillier |first4=A. |last5=Deleuil |first5=M. |last6=Moutou |first6=C. |title=Astrophysical false positives in exoplanet transit surveys: Why do we need bright stars? |journal=SF2A-2013: Proceedings of the Annual Meeting of the French Society of Astronomy and Astrophysics. Eds.: L. Cambresy |page=555 |date=2013|bibcode=2013sf2a.conf..555S}}</ref>
Sovent, de multiples planetas son estat observats a l'entorn d'una estela.<ref name="Nature-20120111">{{Cite journal | last1 = Cassan | first1 = A. | last2 = Kubas | first2 = D. | last3 = Beaulieu | first3 = J. -P. | last4 = Dominik | first4 = M. | last5 = Horne | first5 = K. | last6 = Greenhill | first6 = J. | last7 = Wambsganss | first7 = J. | last8 = Menzies | first8 = J. | last9 = Williams | first9 = A. | last10 = Jørgensen | doi = 10.1038/nature10684 | first10 = U. G. | last11 = Udalski | first11 = A. | last12 = Bennett | first12 = D. P. | last13 = Albrow | first13 = M. D. | last14 = Batista | first14 = V. | last15 = Brillant | first15 = S. | last16 = Caldwell | first16 = J. A. R. | last17 = Cole | first17 = A. | last18 = Coutures | first18 = C. | last19 = Cook | first19 = K. H. | last20 = Dieters | first20 = S. | last21 = Prester | first21 = D. D. | last22 = Donatowicz | first22 = J. | last23 = Fouqué | first23 = P. | last24 = Hill | first24 = K. | last25 = Kains | first25 = N. | last26 = Kane | first26 = S. | last27 = Marquette | first27 = J. -B. | last28 = Martin | first28 = R. | last29 = Pollard | first29 = K. R. | last30 = Sahu | first30 = K. C. | title = One or more bound planets per Milky Way star from microlensing observations | journal = Nature | volume = 481 | issue = 7380 | pages = 167–169 | date=11 January 2012| pmid = 22237108| bibcode=2012Natur.481..167C| pmc = |arxiv = 1202.0903 }}</ref>
Aperaquí 1 sus 5 estelas de tipe solar<ref>For the purpose of this 1 in 5 statistic, "Sun-like" means [[G-type star]]. Data for Sun-like stars was not available so this statistic is an extrapolation from data about [[K-type star]]s</ref> ten un planeta de talha terrèstra<ref>For the purpose of this 1 in 5 statistic, Earth-sized means 1–2 Earth radii</ref> dins sa zona abitabla.<ref>For the purpose of this 1 in 5 statistic, "habitable zone" means the region with 0.25 to 4 times Earth's stellar flux (corresponding to 0.5–2 AU for the Sun).</ref><ref name="ucb1in5">{{cite web|last=Sanders |first=R.|date=4 November 2013|title=Astronomers answer key question: How common are habitable planets?|url=http://newscenter.berkeley.edu/2013/11/04/astronomers-answer-key-question-how-common-are-habitable-planets/
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