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Yanayin Titan

Daga Wikipedia, Insakulofidiya ta kyauta.
Yanayin Titan
climate of geographic location (en) Fassara
Bayanai
Fuskar Titan (en) Fassara
Jadawalin da ke ba da cikakken bayani game da zafin jiki, matsa lamba, da sauran fannonin yanayin Titan.  Hazo na yanayi yana rage zafin jiki a cikin ƙananan yanayi, yayin da methane ke ɗaga zafin jiki a saman.  Cryovolcanoes na fashewa da methane zuwa cikin sararin samaniya, wanda sai ruwa ya sauka a saman, ya zama tafkuna.

Yanayin Titan, wata mafi girma na Saturn, ya yi kama da na duniya ta fuskoki da yawa, duk da cewa yana da ƙananan zafin jiki.  Yanayi mai kauri, ruwan sama na methane, da yuwuwar cryovolcanism suna haifar da kwatance, kodayake tare da kayan daban-daban, zuwa canjin yanayin da duniya ta yi a cikin ɗan gajeren shekara ta duniya.

Yanayin zafi

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Gudun makamashi a kan Titan yana haifar da tasirin greenhouse da tasirin anti-greenhouse.

Titan yana karɓar kusan 1% na adadin hasken rana da Duniya ke yi.[1] Matsakaicin zafin jiki yana da kusan 90.6 K (-182.55 ° C, ko -296.59 ° F). A wannan zafin jiki ruwan kankara yana da matsin tururi mai yawa, don haka yanayin kusan ba shi da tururi na ruwa. Koyaya methane a cikin yanayi yana haifar da tasirin greenhouse mai mahimmanci wanda ke kiyaye farfajiyar Titan a zafin jiki mafi girma fiye da abin da zai zama daidaitattun zafi.[2][3]   

Haze a cikin yanayin Titan yana ba da gudummawa ga tasirin anti-greenhouse ta hanyar nuna hasken rana a cikin sararin samaniya, yana sa farfajiyarsa ta fi sanyi fiye da yanayin sama.[2] Wannan ya biya wani bangare don dumamawar greenhouse, kuma yana kiyaye farfajiyar dan kadan fiye da yadda za a sa ran daga tasirin greenhouse kadai.[4] A cewar McKay et al., "tasirin anti-greenhouse akan Titan yana rage zafin jiki na ƙasa da 9 K yayin da tasirin greenhouse ke ƙara shi da 21 K. Sakamakon duka shine cewa zafin jiki (94 K) yana da 12 K mai dumi fiye da tasirin zafin jiki 82 K. [watau, daidaito da za a cimma ba tare da kowane yanayi ba]" [2]

Lokaci

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Titin Titan's orbital karkata game da Rana yana da kusanci sosai da karkatar axial na Saturn (kimanin 27°), kuma karkatawar axial game da kewayarsa ba komai bane. Wannan yana nufin cewa alkiblar hasken rana mai shigowa ana tafiyar da shi kusan gaba ɗaya ta hanyar zagayowar rana da daddare na Titan da zagayowar shekara ta Saturn. Zagayowar rana akan Titan yana ɗaukar kwanaki 15.9 na Duniya, wanda shine tsawon lokacin da Titan yake ɗauka don kewaya Saturn. Titan yana kulle sosai, don haka ɓangaren Titan koyaushe yana fuskantar Saturn, kuma babu wata “wata” dabam dabam. "wata".

Canjin yanayi yana motsawa ta hanyar shekara ta Saturn: yana ɗaukar Saturn game da shekaru 29.5 na Duniya don kewaye da Rana, yana fallasa adadi daban-daban na hasken rana ga arewa da kudancin Titan a lokuta daban-daban nke shekara ta Saturnian. Canjin yanayi na yanayi sun haɗa da manyan tabkuna na hydrocarbon a arewacin arewacin lokacin hunturu, raguwar haze a kusa da equinoxes saboda sauya yanayin yanayi, da girgije na kankara da ke tattare da shi a yankunan Kudancin Polar.[5][6] Equinox na karshe ya faru ne a ranar 11 ga watan Agusta, 2009; wannan shine bazara equinox na arewacin arewa, ma'ana kudancin kudancin yana samun karancin hasken rana kuma yana motsawa cikin hunturu.[7]

Iska ta saman tana da ƙarancin gaske (<1 mita a kowace dakika). Kayan kwaikwayon kwamfuta na baya-bayan nan ya nuna cewa manyan dunes na soot kamar kayan da ke ruwan sama daga yanayi a cikin yankunan equatorial na iya zama a maimakon haka ta hanyar iskar guguwa da ke faruwa ne kawai a kowace shekara goma sha biyar lokacin da Titan ke cikin equinox.[8] Guguwar tana haifar da saukowa mai ƙarfi, yana gudana zuwa gabas har zuwa mita 10 a kowane sakan lokacin da suka isa farfajiya. A ƙarshen shekara ta 2010, daidai da farkon bazara a arewacin Titan, an lura da jerin guguwar methane a yankunan hamada na Titan.[9]

Saboda tsinkaye na Saturn, Titan yana da kusan 12% kusa da Sun a lokacin rani na kudancin, yana sa lokacin rani na kudu ya fi guntu amma ya fi zafi fiye da lokacin rani na arewa. Wannan asymmetry na iya ba da gudummawa ga bambance-bambance tsakanin hemispheres - arewacin hemisphere yana da tabkuna da yawa na hydrocarbon.[10] Tafkunan Titan galibi suna da kwanciyar hankali, tare da raƙuman ruwa kaɗan; duk da haka, Cassini ya sami shaidar karuwar rikice-rikice a lokacin rani na arewacin arewa, yana ba da shawarar cewa iskõki na ƙasa na iya ƙarfafawa a wasu lokuta na shekara ta Titanian. Cassini ya kuma ga raƙuman ruwa da raƙuman sama.[11]

Ruwan Methane da tabkuna

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Binciken Binciken <i id="mwcQ">Huygens</i> ya nuna cewa Yanayin Titan yana ruwan sama na methane da sauran kwayoyin halitta a saman wata. A watan Oktoba na shekara ta 2007, masu kallo sun lura da karuwar bayyanar opacity a cikin girgije sama da yankin Xanadu na equatorial, wanda ke nuna "methane drizzle", kodayake wannan ba shaida ce kai tsaye ba don ruwan sama.[12] Koyaya, hotunan da suka biyo baya na tabkuna a kudancin Titan da aka ɗauka sama da shekara guda sun nuna cewa an faɗaɗa su kuma an cika su da ruwan sama na hydrocarbon.[3][13] Yana yiwuwa a rufe yankunan Titan a cikin wani nau'i na Tholins, amma ba a tabbatar da wannan ba.[14] Kasancewar ruwan sama yana nuna cewa Titan na iya zama kawai jikin tsarin hasken rana ban da Duniya wanda bakan gizo zai iya samuwa. Koyaya, idan aka ba da matsanancin duhu na yanayi ga haske mai ganuwa, yawancin kowane bakan gizo zai kasance bayyane ne kawai a cikin infrared.[15]

Adadin tafkunan methane da ake gani kusa da sandar kudancin titan ya yi ƙanƙanta fiye da adadin da aka gani kusa da sandar arewa.  Kamar yadda igiyar kudu take a halin yanzu lokacin rani kuma ta arewa a lokacin hunturu, wani hasashe da ke fitowa shine cewa ruwan methane yana kan dogayen hunturu kuma yana ƙafe a lokacin rani.[1]  A cewar wata takarda da Tetsuya Tokano na Jami'ar Cologne ya yi, ana sa ran guguwar da wannan ƙawance ke haifarwa da kuma ruwan sama da kuma iska mai ƙarfi da zai kai 20 m/s (45 mph) a saman manyan tekuna na arewa (Kraken Mare, Ligeia Mare, Punga Mare) kawai a arewacin bazara, wanda zai wuce kwanaki 2.  Lissafi suna ba da shawarar cewa, yayin da yankin arewa, inda yawancin tafkunan ke zama, ke shiga cikin dogon lokacin rani na Titanean, saurin iska zai iya ƙaruwa zuwa 3 km/h, matakan isa don samar da raƙuman ruwa.[3]  Cassini RADAR da Kayayyakin Kayayyakin Taswirar Taswirar Taswirar Infrared tun daga 2014 an lura da raƙuman ruwa a lokuta da yawa, waɗanda wataƙila an samo su daga iskar bazara[4] [5] ko igiyar ruwa.[6][7]. [16][17][18][19]   

Rarraba

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Wani juyawa mai juyawa sama da kudancin Titan

Simulations na duniya iska tsarin bisa ga iska gudun bayanai da Huygens ya dauka a lokacin da ya sauka ya nuna cewa Titan ta yanayi yana zagayawa a cikin wani daya Hadley cell. Gas mai zafi yana tashi a kudancin Titan - wanda ke fuskantar bazara a lokacin saukowar Huygens - kuma yana nutsewa a arewacin arewa, wanda ke haifar da iskar gas mai tsawo daga kudu zuwa arewa da kuma iskar gas da ke ƙasa daga arewa zuwa kudu. Irin wannan babban kwayar halitta ta Hadley tana yiwuwa ne kawai a duniyar da ke juyawa a hankali kamar Titan.[20] Kwayar iska mai yaduwa daga igiya zuwa igiya ta bayyana tana tsakiya a kan stratosphere; simulations sun nuna cewa ya kamata ya canza kowane shekaru goma sha biyu, tare da lokacin sauyawa na shekaru uku, a cikin shekara ta Titan (shekaru 30 na duniya). [21] Wannan tantanin halitta yana haifar da ƙungiyar duniya ta matsin lamba - abin da ke da tasiri bambancin Yankin Intertropical na Duniya (ITCZ). Ba kamar a Duniya ba, duk da haka, inda teku ke iyakance ITCZ zuwa wurare masu zafi, a kan Titan, yankin yana yawo daga wannan sanda zuwa ɗayan, yana ɗaukar ruwan sama na methane tare da shi. Wannan yana nufin cewa Titan, duk da yanayin sanyi, ana iya cewa yana da yanayi na wurare masu zafi.

A watan Yunin 2012, Cassini ya zana hoton wani juyawa mai juyawa a kan kudancin Titan, wanda ƙungiyar daukar hoto ta yi imanin yana da alaƙa da "polar hood" - wani yanki mai zurfi, mai tsawo da aka gani a kan arewacin arewa tun zuwan binciken a shekara ta 2004. Kamar yadda hemispheres yanzu suna sauya yanayi tun daga 2009 equinox, tare da kudancin kudancin shiga cikin hunturu da arewa shiga lokacin rani, an yi la'akari da cewa wannan vortex na iya nuna alamar kafa sabon, kudancin kudanci.[22]

Girgije

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Titan - Arewacin Pole - tsarin girgije da aka zana a launi na ƙarya.
Titan - South pole - vortex detail

Gizagizai na Titan, mai yiwuwa sun ƙunshi methane, ethane, ko wasu abubuwa masu sauƙi, sun warwatse kuma suna canzawa, suna nuna hazo gaba ɗaya..[23]

A watan Satumbar shekara ta 2006, A cikin watan Satumba na 2006, Cassini ya zana wani babban gajimare a tsayin kilomita 40 a kan sandar arewa ta Titan.  Ko da yake an san methane yana taruwa a sararin samaniyar Titan, girgijen ya fi zama ethane, saboda girman da aka gano na barbashi bai wuce 1-3 micrometers ba kuma ethane shima yana iya daskarewa a wadannan tsaunukan.  A watan Disamba, Cassini ya sake lura da murfin gajimare kuma ya gano methane, ethane da sauran kwayoyin halitta.  Gajimaren ya fi kilomita 2400 a diamita kuma har yanzu ana iya gani yayin tashi sama da wata guda.  Wata hasashe ita ce, a halin yanzu ana ruwan sama (ko, idan ya yi sanyi, dusar ƙanƙara) a kan sandar arewa;  da downdrafts a high arewa latitudes suna da karfi isa ya fitar da kwayoyin barbashi zuwa saman.  Waɗannan su ne mafi ƙaƙƙarfan shaida tukuna don dogon hasashen zagayowar "methanological" (mai kama da zagayowar ruwa ta duniya) akan Titan..[24]  

An kuma sami girgije a yankin kudancin polar. Duk da yake yawanci yana rufe 1% na faifan Titan, an lura da abubuwan fashewa wanda girgije ya fadada cikin sauri zuwa kusan 8%. Ɗaya daga cikin ra'ayoyin ya tabbatar da cewa girgije na kudancin an kafa su ne lokacin da matakan hasken rana suka tashi a lokacin rani na Titanean suka haifar da tashin hankali a cikin yanayi, wanda ya haifar da convection. Wannan bayanin yana da rikitarwa saboda gaskiyar cewa an lura da samar da girgije ba kawai bayan lokacin rani ba har ma a tsakiyar bazara. Ƙarin danshi na methane a kudancin kudancin yana iya taimakawa ga saurin karuwa a girman girgije.[25] Akwai lokacin rani a kudancin Titan har zuwa shekara ta 2010, lokacin da Saturn's orbit, wanda ke jagorantar motsi na wata, ya karkatar da arewacin zuwa Sun.[20] Lokacin da lokutan suka canza, ana sa ran ethane zai fara tarwatsawa a kan kudancin.

Titan methane girgije (mai rai; Yuli 2014). [26]

Samfuran bincike waɗanda suka dace da kyau tare da abubuwan lura suna ba da shawarar cewa gajimare a kan gungu na Titan a daidaitattun abubuwan da aka fi so kuma murfin girgije ya bambanta da nisa daga saman kan sassa daban-daban na tauraron dan adam.  A cikin yankunan polar (sama da digiri na 60), gizagizai masu yaduwa da dindindin na ethane suna bayyana a ciki da sama da troposphere;  a ƙananan latitudes, galibi ana samun gajimare na methane tsakanin 15 zuwa 18 km, kuma sun fi kai-tsaye da kuma na gida.  A lokacin rani, gajimaren methane akai-akai, mai kauri amma mai kauri yana kama da tari kusan 40°. °.[21] 

Binciken ƙasa ya kuma nuna bambancin yanayi a cikin girgije. A cikin shekaru 30 na Saturn, tsarin girgije na Titan ya bayyana ya bayyana har tsawon shekaru 25, sannan ya ɓace har tsawon shekaru hudu zuwa biyar kafin ya sake bayyana.[24]

Cassini ya kuma gano girgije mai tsawo, fari, nau'in cirrus a cikin yanayin Titan na sama, mai yiwuwa an kafa shi da methane.[27]

Kodayake har yanzu ba a lura da wata shaidar aikin walƙiya a kan Titan ba, samfuran kwamfuta sun nuna cewa girgije a cikin ƙananan troposphere na wata na iya tara isasshen caji don samar da walƙiya daga tsawo na kusan kilomita 20.[28] Kasancewar walƙiya a cikin yanayin Titan zai goyi bayan samar da kayan kwayoyin halitta. Cassini bai gano wani walƙiya a cikin yanayin Titan ba, kodayake walƙiya na iya kasancewa idan ya yi rauni sosai don a gano shi. [29][30] Kayan kwaikwayon kwamfuta na baya-bayan nan sun nuna cewa a wasu yanayi fitar da raƙuman ruwa, matakan farko na fitar da walƙiya, na iya zama a kan Titan.[31] 

Manazarta

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  1. ↑ "Titan: A World Much Like Earth". Space.com. August 6, 2009. Retrieved April 2, 2012.
  2. ↑ 2.0 2.1 2.2 McKay, C. P.; Pollack, J. B.; Courtin, R. (September 6, 1991). "Titan: Greenhouse and Anti-greenhouse Effects on Titan". Science. 253 (5024): 1118–1121. Bibcode:1991Sci...253.1118M. doi:10.1126/science.11538492. PMID 11538492. S2CID 10384331. Cite error: Invalid <ref> tag; name "McKay" defined multiple times with different content
  3. ↑ 3.0 3.1 "Titan Has More Oil Than Earth". Space.com. February 13, 2008. Retrieved February 13, 2008. Cite error: Invalid <ref> tag; name "oil" defined multiple times with different content
  4. ↑ "PIA06236: Titan: Complex 'Anti-greenhouse'". Planetary Photojournal. Jet Propulsion Laboratory. May 2, 2005. Retrieved January 30, 2019.
  5. ↑ "Saturn's moon Titan shows surprising seasonal changes". ScienceDaily. September 28, 2012. Retrieved January 30, 2019.
  6. ↑ Morrow, Ashley (November 10, 2015). "Monstrous Ice Cloud in Titan's South Polar Region". NASA. Retrieved January 30, 2019.
  7. ↑ "On Titan, the Sky is Falling!". Solar System Exploration: NASA Science. May 4, 2011. Retrieved January 30, 2019.
  8. ↑ "Violent Methane Storms on Titan May Explain Dune Direction". SpaceRef. April 15, 2015. Archived from the original on July 26, 2020. Retrieved April 19, 2015.
  9. ↑ "Cassini Sees Seasonal Rains Transform Titan's Surface". NASA. March 17, 2011. Archived from the original on May 17, 2017. Retrieved January 20, 2018.
  10. ↑ Aharonson, Oded (November 2009). "Titan's Lakes". California Institute of Technology. Archived from the original on April 15, 2018. Retrieved January 30, 2019.
  11. ↑ Klotz, Irene (March 23, 2014). "Cassini Spies Wind-Rippled Waves on Titan". Space.com. Retrieved January 30, 2019.
  12. ↑ Ádámkovics, Máté; Wong, Michael H.; Laver, Conor; de Pater, Imke (9 November 2007). "Widespread Morning Drizzle on Titan". Science. 318 (5852): 962–965. Bibcode:2007Sci...318..962A. doi:10.1126/science.1146244. PMID 17932256. S2CID 35093635.
  13. ↑ Mason, Joe; Buckley, Michael (January 29, 2009). "Cassini Finds Hydrocarbon Rains May Fill The Lakes". Cassini Imaging Central Laboratory For Operations. Space Science Institute. Archived from the original on July 25, 2011. Retrieved January 29, 2009.
  14. ↑ Somogyi, Arpad; Smith, M. A. (September 2006). "Mass Spectral Investigation of Laboratory Made Tholins and Their Reaction Products: Implications to Tholin Surface Chemistry on Titan". Bulletin of the American Astronomical Society. 38: 533. Bibcode:2006DPS....38.2730S.
  15. ↑ "Rainbows on Titan". NASA Science. February 25, 2005. Archived from the original on October 21, 2011. Retrieved October 8, 2011.
  16. ↑ Barnes, Jason W.; Sotin, Christophe; Soderblom, Jason M.; Brown, Robert H.; Hayes, Alexander G.; Donelan, Mark; Rodriguez, Sebastien; Mouélic, Stéphane Le; Baines, Kevin H.; McCord, Thomas B. (2014-08-21). "Cassini/VIMS observes rough surfaces on Titan's Punga Mare in specular reflection". Planetary Science. 3 (1): 3. Bibcode:2014PlSci...3....3B. doi:10.1186/s13535-014-0003-4. ISSN 2191-2521. PMC 4959132. PMID 27512619.
  17. ↑ Hofgartner, Jason D.; Hayes, Alexander G.; Lunine, Jonathan I.; Zebker, Howard; Lorenz, Ralph D.; Malaska, Michael J.; Mastrogiuseppe, Marco; Notarnicola, Claudia; Soderblom, Jason M. (2016-06-01). "Titan's "Magic Islands": Transient features in a hydrocarbon sea". Icarus (in Turanci). 271: 338–349. Bibcode:2016Icar..271..338H. doi:10.1016/j.icarus.2016.02.022. ISSN 0019-1035.
  18. ↑ Heslar, Michael F.; Barnes, Jason W.; Soderblom, Jason M.; Seignovert, Benoît; Dhingra, Rajani D.; Sotin, Christophe (2020-08-14). "Tidal Currents Detected in Kraken Mare Straits from Cassini VIMS Sun Glitter Observations". The Planetary Science Journal (in Turanci). 1 (2): 35. arXiv:2007.00804. Bibcode:2020PSJ.....1...35H. doi:10.3847/PSJ/aba191. ISSN 2632-3338.
  19. ↑ Sotin, C.; Barnes, J. W.; Lawrence, K. J.; Soderblom, J. M.; Audi, E.; Brown, R. H.; Le Mouelic, S.; Baines, K. H.; Buratti, B. J.; Clark, R. N.; Nicholson, P. D. (2015-12-01). "Tidal Currents between Titan's Seas Detected by Solar Glints". AGU Fall Meeting Abstracts. 12: P12B–04. Bibcode:2015AGUFM.P12B..04S.
  20. ↑ 20.0 20.1 "The Way the Wind Blows on Titan". Jet Propulsion Laboratory. June 1, 2007. Archived from the original on April 27, 2009. Retrieved June 2, 2007. Cite error: Invalid <ref> tag; name "Titan wind" defined multiple times with different content
  21. ↑ 21.0 21.1 Rannou, R.; Montmessin, F.; Hourdin, F.; Lebonnois, S. (January 13, 2006). "The Latitudinal Distribution of Clouds on Titan". Science. 311 (5758): 201–205. Bibcode:2006Sci...311..201R. doi:10.1126/science.1118424. PMID 16410519. S2CID 1190978. Cite error: Invalid <ref> tag; name "Rannou2006" defined multiple times with different content
  22. ↑ "The South Polar Vortex in Motion". Cassini Imaging Central Laboratory For Operations. Space Science Institute. July 10, 2012. Retrieved July 11, 2012.
  23. ↑ Arnett, Bill (2005). "Titan (Saturn VI)". University of Arizona. Archived from the original on November 21, 2005. Retrieved April 10, 2005.
  24. ↑ 24.0 24.1 "Cassini Images Mammoth Cloud Engulfing Titan's North Pole". NASA. February 1, 2007. Archived from the original on October 9, 2011. Retrieved April 14, 2007. Cite error: Invalid <ref> tag; name "nasagov" defined multiple times with different content
  25. ↑ Schaller, Emily L.; Brouwn, Michael E.; Roe, Henry G.; Bouchez, Antonin H. (February 13, 2006). "A large cloud outburst at Titan's south pole" (PDF). Icarus. 182 (1): 224–229. Bibcode:2006Icar..182..224S. doi:10.1016/j.icarus.2005.12.021. Retrieved August 23, 2007.
  26. ↑ Dyches, Preston (August 12, 2014). "Cassini Tracks Clouds Developing Over a Titan Sea". NASA. Retrieved August 13, 2014.
  27. ↑ Atkinson, Nancy (February 4, 2011). "Earth-like Cirrus Clouds Found on Titan". Universe Today. Retrieved February 11, 2011.
  28. ↑ Chow, Denise (May 11, 2010). "Titan's Thunder Could Point to Alien Lightning". Space.com. Retrieved February 11, 2011.
  29. ↑ Fischer, G; Gurnett, D.A.; Kurth, W.S.; Farell, W.M.; Kaiser, M.L.; Zarka, P (2007). "Nondetection of Titan lightning radio emissions with Cassini/RPWS after 35 close Titan flybys". Geophys. Res. Lett. 34 (22): L22104. Bibcode:2007GeoRL..3422104F. doi:10.1029/2007GL031668.
  30. ↑ Fischer, G; Gurnett, D.A. (2011). "The search for Titan lightning radio emissions". Geophys. Res. Lett. 38 (8): L08206. Bibcode:2011GeoRL..38.8206F. doi:10.1029/2011GL047316. S2CID 135052598.
  31. ↑ Köhn, C; Dujko, S; Chanrion, O; Neubert, T (2019). "Streamer propagation in the atmosphere of Titan and other N2:CH4 mixtures compared to N2:O2 mixtures". Icarus. 333: 294–305. arXiv:1802.09906. Bibcode:2019Icar..333..294K. doi:10.1016/j.icarus.2019.05.036.
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