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[[Berkas:Jupiter Belt System.svg| |
[[Berkas:Jupiter Belt System.svg|jmpl|300px|Pola awan di Jupiter tahun 2000]] |
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'''Atmosfer [[ |
'''Atmosfer [[Jupiter]]''' adalah [[atmosfer benda langit|atmosfer keplanetan]] terbesar dalam [[Tata Surya]]. Atmosfernya sebagian besar terbentuk dari [[Hidrogen|hidrogen molekuler]] dan [[helium]] dalam [[Matahari#Komposisi|proporsi solar]] yang lebih kurang sama; senyawa kimia lainnya hanya ada dalam jumlah kecil dan meliputi [[metana]], [[amonia]], [[hidrogen sulfida]], dan [[air]]. Meskipun air diduga berada jauh di dalam atmosfer, konsentrasi terukur langsungnya sangat rendah. [[Nitrogen]], [[sulfur]], dan [[gas mulia]] melimpah dalam atmosfer Jupiter melebihi nilai solar yang disebabkan oleh sekitar tiga faktor.{{sfn|Atreya Mahaffy Niemann et al.|2003}} |
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Atmosfer Jupiter tidak memiliki batas bawah yang jelas dan secara bertahap bertransisi menjadi bagian dalam planet yang cair.<ref name=Guillot1999>[[#Guillot|Guillot (1999)]]</ref> Dari yang terendah sampai tertinggi, lapisan atmosfer adalah [[troposfer]], [[stratosfer]], [[termosfer]], dan [[eksosfer]]. Setiap lapisan memiliki karakteristik [[gradien suhu]].<ref name=Sieff1998>[[#Sieff|Sieff ''et al.'' (1998)]]</ref> Lapisan terendah, troposfer, memiliki sistem awan dan kabut yang rumit, yang terdiri dari lapisan amonia, [[amonium hidrosulfida]], dan air.{{sfn|Atreya|Wong|2005}} |
Atmosfer Jupiter tidak memiliki batas bawah yang jelas dan secara bertahap bertransisi menjadi bagian dalam planet yang cair.<ref name=Guillot1999>[[#Guillot|Guillot (1999)]]</ref> Dari yang terendah sampai tertinggi, lapisan atmosfer adalah [[troposfer]], [[stratosfer]], [[termosfer]], dan [[eksosfer]]. Setiap lapisan memiliki karakteristik [[gradien suhu]].<ref name=Sieff1998>[[#Sieff|Sieff ''et al.'' (1998)]]</ref> Lapisan terendah, troposfer, memiliki sistem awan dan kabut yang rumit, yang terdiri dari lapisan amonia, [[amonium hidrosulfida]], dan air.{{sfn|Atreya|Wong|2005}} |
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* {{cite journal| doi = 10.1016/S0032-0633(02)00144-7| last1 = Atreya| first1 = Sushil K.| last2 = Mahaffy| first2 = P. R.| last3 = Niemann| first3 = H. B.| last4 = Wong| first4 = M. H.| last5 = Owen| first5 = T. C.| date=February 2003 | title = Composition and origin of the atmosphere of Jupiter—an update, and implications for the extrasolar giant planets| journal = [[Planetary and Space Science]]| issn = 0032-0633| volume = 51| issue = 2| pages = 105–112| bibcode = 2003P&SS...51..105A| ref = {{sfnRef|Atreya Mahaffy Niemann et al.|2003}}}} |
* {{cite journal| doi = 10.1016/S0032-0633(02)00144-7| last1 = Atreya| first1 = Sushil K.| last2 = Mahaffy| first2 = P. R.| last3 = Niemann| first3 = H. B.| last4 = Wong| first4 = M. H.| last5 = Owen| first5 = T. C.| date=February 2003 | title = Composition and origin of the atmosphere of Jupiter—an update, and implications for the extrasolar giant planets| journal = [[Planetary and Space Science]]| issn = 0032-0633| volume = 51| issue = 2| pages = 105–112| bibcode = 2003P&SS...51..105A| ref = {{sfnRef|Atreya Mahaffy Niemann et al.|2003}}}} |
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* {{cite journal| doi = 10.1007/s11214-005-1951-5| last1 = Atreya| first1 = Sushil K.| last2 = Wong| first2 = Ah-San| year = 2005| title = Coupled Clouds and Chemistry of the Giant Planets — A Case for Multiprobes| journal = Space Science Reviews| issn = 0032-0633| volume = 116| pages = 121–136| url = http://www-personal.umich.edu/~atreya/Chapters/2005_JovianCloud_Multiprobes.pdf| format = PDF| bibcode = 2005SSRv..116..121A| ref = harv}} |
* {{cite journal| doi = 10.1007/s11214-005-1951-5| last1 = Atreya| first1 = Sushil K.| last2 = Wong| first2 = Ah-San| year = 2005| title = Coupled Clouds and Chemistry of the Giant Planets — A Case for Multiprobes| journal = Space Science Reviews| issn = 0032-0633| volume = 116| pages = 121–136| url = http://www-personal.umich.edu/~atreya/Chapters/2005_JovianCloud_Multiprobes.pdf| format = PDF| bibcode = 2005SSRv..116..121A| ref = harv}} |
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* {{cite journal| doi = 10.1016/j.pss.2004.04.002| last1 = Atreya| first1 = Sushil K.| last2 = Wong| first2 = Ah-San| last3 = Baines| first3 = K. H.| last4 = Wong| first4 = M. H.| last5 = Owen| first5 = T. C.| year = 2005| title = Jupiter's ammonia clouds—localized or ubiquitous?| journal = [[Planetary and Space Science]]| issn = 0032-0633| volume = 53| issue = 5| pages = 498–507| url = http://www-personal.umich.edu/~atreya/Articles/2005_Jupiters_Ammonia.pdf| format = PDF| |
* {{cite journal| doi = 10.1016/j.pss.2004.04.002| last1 = Atreya| first1 = Sushil K.| last2 = Wong| first2 = Ah-San| last3 = Baines| first3 = K. H.| last4 = Wong| first4 = M. H.| last5 = Owen| first5 = T. C.| year = 2005| title = Jupiter's ammonia clouds—localized or ubiquitous?| journal = [[Planetary and Space Science]]| issn = 0032-0633| volume = 53| issue = 5| pages = 498–507| url = http://www-personal.umich.edu/~atreya/Articles/2005_Jupiters_Ammonia.pdf| format = PDF| bibcode = 2005P&SS...53..498A| ref = {{sfnRef|Atreya Wong Baines et al.|2005}}}} |
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* {{cite journal| doi = 10.1126/science.1147912| last1 = Baines| first1 = Kevin H.| last2 = Simon-Miller| first2 = Amy A| last3 = Orton| first3 = Glenn S.| last4 = Weaver| first4 = Harold A.| last5 = Lunsford| first5 = Allen| last6 = Momary| first6 = Thomas W.| last7 = Spencer| first7 = John| last8 = Cheng| first8 = Andrew F.| last9 = Reuter| first9 = Dennis C.| date = 12 October 2007| title = Polar Lightning and Decadal-Scale Cloud Variability on Jupiter| url = https://archive.org/details/sim_science_2007-10-12_318_5848/page/226| journal = [[Science (journal)|Science]]| volume = 318| issue = 5848| pages = 226–229| pmid = 17932285| pmc = | bibcode = 2007Sci...318..226B| ref = {{sfnRef|Baines Simon-Miller et al.|2007}}}} |
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{{refend}} |
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|location=London|isbn=0-571-18026-4 |
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* {{Commons category-inline}} |
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[[Kategori: |
[[Kategori:Jupiter]] |
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[[Kategori:Atmosfer keplanetan| |
[[Kategori:Atmosfer keplanetan|Jupiter]] |
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[[Kategori:Atmosfer keplanetan Tata Surya|Jupiter]] |
[[Kategori:Atmosfer keplanetan Tata Surya|Jupiter]] |
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Revisi terkini sejak 12 Desember 2023 03.58
Atmosfer Jupiter adalah atmosfer keplanetan terbesar dalam Tata Surya. Atmosfernya sebagian besar terbentuk dari hidrogen molekuler dan helium dalam proporsi solar yang lebih kurang sama; senyawa kimia lainnya hanya ada dalam jumlah kecil dan meliputi metana, amonia, hidrogen sulfida, dan air. Meskipun air diduga berada jauh di dalam atmosfer, konsentrasi terukur langsungnya sangat rendah. Nitrogen, sulfur, dan gas mulia melimpah dalam atmosfer Jupiter melebihi nilai solar yang disebabkan oleh sekitar tiga faktor.[1]
Atmosfer Jupiter tidak memiliki batas bawah yang jelas dan secara bertahap bertransisi menjadi bagian dalam planet yang cair.[2] Dari yang terendah sampai tertinggi, lapisan atmosfer adalah troposfer, stratosfer, termosfer, dan eksosfer. Setiap lapisan memiliki karakteristik gradien suhu.[3] Lapisan terendah, troposfer, memiliki sistem awan dan kabut yang rumit, yang terdiri dari lapisan amonia, amonium hidrosulfida, dan air.[4]
Referensi
[sunting | sunting sumber]Sumber kutipan
[sunting | sunting sumber]- Atreya, Sushil K.; Wong, M. H.; Owen, T. C.; Mahaffy, P. R.; Niemann, H. B.; de Pater, I.; Drossart, P.; Encrenaz, T. (October–November 1999). "A comparison of the atmospheres of Jupiter and Saturn: Deep atmospheric composition, cloud structure, vertical mixing, and origin". Planetary and Space Science. 47 (10–11): 1243–1262. Bibcode:1999P&SS...47.1243A. doi:10.1016/S0032-0633(99)00047-1. ISSN 0032-0633. PMID 11543193.
- Atreya, Sushil K.; Mahaffy, P. R.; Niemann, H. B.; Wong, M. H.; Owen, T. C. (February 2003). "Composition and origin of the atmosphere of Jupiter—an update, and implications for the extrasolar giant planets". Planetary and Space Science. 51 (2): 105–112. Bibcode:2003P&SS...51..105A. doi:10.1016/S0032-0633(02)00144-7. ISSN 0032-0633.
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