Tidal heating
 Tidal heating | |
|---|---|
| Bayanai | |
| Ƙaramin ɓangare na | thermal phenomenon (en)  |
| Has cause (en) | tidal acceleration (en) da tidal force (en) |
| Yana haddasa | tidal circularization (en) |
| Defining formula (en) | |
Tidal heating (wanda ake kira tidal dissipation ko tidal damping) wani tsari ne da ke faruwa ta hanyar gogayyar ƙarfin tidal (tidal friction), inda ake mayar da makamashin zagayawa (orbital energy) da makamashin juyawa (rotational energy) zuwa zafi a cikin tekun saman ko kuma cikin jikin wata ko duniya.
Lokacin da wani jiki yake cikin zagaye mai siffar oval (elliptical orbit), ƙarfin tidal forces da ke aiki a kansa ya fi ƙarfi idan yana kusa da periapsis fiye da lokacin da yake kusa da apoapsis. Saboda haka, yadda ƙarfin tidal ke karkatar ko gurɓata siffar jikin (tidal deformation), wato samuwar tudun tidal (tidal bulge), yana canzawa yayin da jikin ke zagayawa. Wannan canjin yana haifar da gogayya a cikin jikin, wadda ke dumama cikinsa.
Makamashin da jikin yake samu a matsayin zafi yana fitowa ne daga makamashin zagayawarsa da/ko makamashin juyawarsa. Saboda haka, a cikin tsarin da ya ƙunshi jikkuna biyu, idan babu wasu ƙarin tasirin ƙarfin jan hankali, zagayen oval ɗin da farko zai rika sauyawa a hankali zuwa zagaye mai madauwari (tidal circularization). Haka kuma, lokutan juyawar jikkunan biyu za su daidaita zuwa kusan lokacin zagayawarsu, lamarin da ake kira tidal locking.
Ana samun dumamar tidal mai ɗorewa (sustained tidal heating) idan wasu jikkunan sararin samaniya suna ci gaba da amfani da ƙarfin jan hankalinsu wajen hana zagayen ya zama madauwari, ta hanyar ci gaba da jan jikin zuwa wani elliptical orbit. A irin wannan tsarin mai rikitarwa, har yanzu ana mayar da makamashin zagayawa da na juyawa zuwa makamashin zafi. Sai dai a wannan yanayin, semimajor axis na zagayen zai ragu, maimakon orbital eccentricity kawai ta ragu.
Watannin manyan taurari
[gyara sashe | gyara masomin]Rashin dumama yana da alhakin aikin geologic na mafi yawan jiki mai aiki a cikin Tsarin hasken rana: Io, wata na Jupiter. Io ta eccentricity ya ci gaba ne sakamakon ta orbital resonances tare da Galilean watannin Europa da Ganymede . [1] Wannan hanyar ta samar da makamashi don narkar da ƙananan yadudduka na kankara da ke kewaye da dutsen dutse na Jupiter mafi girma, Europa. Koyaya, dumama na ƙarshe ya fi rauni, saboda raguwar karkatarwa - Europa tana da rabin mitar Io da ƙaramin radius na 14%, kuma, yayin da yanayin Europa ya kusan sau biyu fiye da na Io, ƙarfin ruwa ya faɗi tare da cube na nesa kuma yana da kashi ɗaya cikin huɗu kawai na ƙarfi a Europa. Jupiter yana kula da zagaye na wata ta hanyar raƙuman ruwa da suke tasowa a kansa kuma ta haka ne ƙarfin juyawa ya ba da ikon tsarin.[1] Wata ta Saturn Enceladus ana zaton tana da ruwa mai ruwa a ƙarƙashin ƙanƙara, saboda zafi mai zafi da ke da alaƙa da sautin sa tare da Dione. Ruwan tururi na ruwa wanda ke fitar da kayan daga Enceladus ana zaton ana amfani da shi ta hanyar rikici da aka samar a cikin ciki.
Duniya
[gyara sashe | gyara masomin]Munk & Wunsch (1998) sun kiyasta cewa Duniya tana fuskantar 3.7 TW (0.0073 W / m2) na dumama, wanda 95% (3.5 TW ko 0.0069 W / m) ke da alaƙa da hawan teku kuma 5% (0.2 TW ko 0.54 W / m2 yana da alaƙa ne da hawan ƙasa, tare da 3.2 TW saboda hulɗar hawan ruwa tare da Wata da 0.5 TW saboda hawan ruwa da Sun.[2] Egbert & Ray (2001) sun tabbatar da cewa kimantawa gabaɗaya, rubuce-rubuce "duk adadin makamashi da aka ɓace a cikin tsarin Duniya-Luna-Sun yanzu an ƙaddara shi sosai. Hanyoyin geodesy na sararin samaniya - altimetry, laser na tauraron dan adam, laser na wata - sun haɗu zuwa 3.7 TW ..." [3]
Heller et al. (2) sun kiyasta cewa jim kadan bayan an kafa wata, lokacin da wata ta kewaye da sau 10-15 kusa da Duniya fiye da yadda take yi yanzu, dumama ta ruwa na iya ba da gudummawa ~ 10 W / m2 na dumama. Wannan dumama ya faru a kan watakila shekaru miliyan 100, kuma zai iya haifar da karuwar zafin jiki har zuwa 5 ° C a farkon Duniya.[4][5]
Wata
[gyara sashe | gyara masomin]Harada et al. (2014) sun ba da shawarar cewa dumama ruwa na iya haifar da wani nau'i mai narkewa a iyakar core-mantle a cikin Moon na Duniya.[6]
Tsarin
[gyara sashe | gyara masomin]Adadin zafin da dumamar ƙarfin jan hankali (tidal heating) ke samarwa, wanda ake rubutawa da (ETidal), a cikin wani tauraron dan Adam da ke juyawa daidai da zagayawarsa (spin-synchronous), yake da shimfiɗar zagayawa a jirgi ɗaya (coplanar), wato (I=0), kuma yake da zagaye mai karkacewa (eccentric orbit), ana iya bayyana shi da wannan ma'auni:
- (R) — matsakaicin radius na tauraron dan Adam.
- (n) — matsakaicin saurin motsinsa a zagayen sararin samaniya (mean orbital motion).
- (a) — tazarar zagayawar tauraron dan Adam, wato semi-major axis.
- (e) — karkacewar zagayen tauraron dan Adam (orbital eccentricity).
- (M_h) — yawan/ƙarfin nauyin jikin da yake kewaye da shi, wato jikin tsakiya ko mai masaukin baki (host/central body).
- (\operatorname{Im}(k_2)) — ɓangaren hasashen lamba na Love Number na mataki na biyu, wanda ke auna yadda tauraron dan Adam ke iya juya makamashin tidal zuwa zafin gogayya (frictional heat).
Wannan ɓangaren na Love Number yana samuwa ne sakamakon hulɗar rheology, wato yadda kayan da ke cikin jikin tauraron dan Adam suke yin ɗabi'a yayin da aka matsa ko aka ja su, da kuma karfin jan hankalin jikin da kansa (self-gravitation).
Saboda haka, (\operatorname{Im}(k_2)) yana dogara ne da radius, yawan abu a kowace ƙara (density), da kuma wasu sigogin rheology, kamar shear modulus (ma'aunin tsayayyar abu ga karkacewa) da viscosity (ɗanko), da sauran sigogi waɗanda suka danganta da tsarin da ake amfani da shi wajen bayyana rheology.
Haka kuma, ƙimomin waɗannan sigogin rheology suna dogara ne da zafin cikin jikin tauraron dan Adam da kuma yawan narkewar wani ɓangare (partial melt) da ke cikin cikinsa.
Dubi kuma
[gyara sashe | gyara masomin]- Dutsen da ke cikin wuta
- Hawan ruwa
- Rufewar ruwa
- Io Mai lura da Dutsen Volcano
- Bambancin duniya
Manazarta
[gyara sashe | gyara masomin]- 1 2 Peale, S.J.; Cassen, P.; Reynolds, R.T. (1979). "Melting of Io by Tidal Dissipation". Science. 203 (4383): 892–894. Bibcode:1979Sci...203..892P. doi:10.1126/science.203.4383.892. JSTOR 1747884. PMID 17771724. S2CID 21271617.
- ↑ Munk, Walter; Wunsch, Carl (1998). "Abyssal recipes II: energetics of tidal and wind mixing" (PDF). Deep Sea Research Part I: Oceanographic Research Papers. 45 (12): 1977–2010. Bibcode:1998DSRI...45.1977M. doi:10.1016/S0967-0637(98)00070-3. Retrieved 26 March 2023.
- ↑ Egbert, Gary D.; Ray, Richard D. (October 15, 2001). "Estimatesof tidal energy dissipationfrom TOPEX/Poseidon altimeter data". Journal of Geophysical Research. 106 (C10): 22475–22502. Bibcode:2001JGR...10622475E. doi:10.1029/2000JC000699.
- ↑ Heller, R; Duda, JP; Winkler, M; Reitner, J; Gizon, L (2021). "Habitability of the early Earth: liquid water under a faint young Sun facilitated by strong tidal heating due to a closer Moon". PalZ. 95 (4): 563–575. arXiv:2007.03423. Bibcode:2021PalZ...95..563H. doi:10.1007/s12542-021-00582-7. S2CID 244532427 Check
|s2cid=value (help). - ↑ Jure Japelj (11 January 2022). "How Much Did the Moon Heat Young Earth?". EOS. 103. doi:10.1029/2022EO220017. Retrieved 26 March 2023.
- ↑ Harada, Y; Goosens, S; Matsumoto, K; Yan, J; Ping, J; Noda, H; Harayama, J (27 July 2014). "Strong tidal heating in an ultralow-viscosity zone at the core–mantle boundary of the Moon". Nature Geoscience. 7 (8): 569–572. Bibcode:2014NatGe...7..569H. doi:10.1038/ngeo2211.