La ithiyori ye-inflationary yendawo yonke isiphakamiso sesayensi esifuna ukuchaza izimfihlakalo zemvelaphi nokuziphendukela kwemvelo kokuqala kwendawo yonke. Yahlongozwa ngeminyaka yawo-1980 isazi sesayensi yemvelo u-Alan Guth futhi kusukela lapho iye yamukelwa kabanzi umphakathi wesayensi njengencazelo ekholisayo yezikhathi zakuqala zomhlaba.
Kulesi sihloko sizokutshela konke odinga ukukwazi mayelana nethiyori ye-inflation, ukuthi ihlanganisani nokuthi kuyini okutholakele.
Iyini i-inflationary theory
Ithiyori yokwenyuka kwamanani emali isuselwe embonweni wokuthi indawo yonke yaba nokwanda okusheshayo nokusheshisa kakhulu ezikhathini zayo zokuqala, ngemva nje kweBig Bang. Lokhu kwanda, okwaziwa nge-cosmic inflation, bekuzokwenzeka ngengxenyana yomzuzwana futhi bekuyoba ngokushesha kakhulu kunanoma yikuphi okunye ukwanda emlandweni wendawo yonke.
Ithiyori yokwenyuka kwamanani emali isekelwe ekuhlolweni nasebufakazini obuhlukahlukene bezinkanyezi, okuhlanganisa ukufana nokufana kwendawo yonke ngezinga elikhulu, ukuba khona kokuguquguquka emisebeni engemuva kwendawo yonke, nokusatshalaliswa kwemithala endaweni yonke. Ngokombono wokwehla kwamandla emali, lezi zici zendawo yonke zingachazwa ngokwenyuka kwamandla emali endaweni yonke.
I-inflation ye-cosmic ngabe ibangelwa uhlobo lwamandla olungaziwa olubizwa ngokuthi i-inflationary energy, okuyinto kwakuyodala amandla anyanyekayo anamandla kakhulu ayeyoqhubeza ukwanda kwendawo yonke. Ngemva kwengxenyana yomzuzwana, amandla okwehla kwamandla emali abeyobe esenyamalele, okuvumela indawo yonke ukuba iqhubeke yanda ngezinga eliphansi, elingaguquki.
Izici eziyinhloko
Ithiyori ye-inflationary isiphakamiso se-cosmological esichaza ukuthi indawo yonke yabhekana kanjani nesigaba sokukhula okusheshayo ezikhathini zayo zokuqala zokuba khona. Yasungulwa ngeminyaka yawo-1980 yiqembu lezazi zefiziksi ezithiyori elaliholwa ngu-Alan Guth no-Andrei Linde., futhi kusukela ngaleso sikhathi iye yamukelwa kabanzi umphakathi wesayensi njengencazelo ekholisa kakhulu yemvelaphi yendawo yonke.
Esinye sezici eziyinhloko zethiyori yokwenyuka kwamanani emali ukuthi iphakamisa ukuthi indawo yonke yaba nokwanda okusheshayo nokusheshayo phakathi nengxenye yomzuzwana ngemva kweBig Bang. Lokhu kwanda kwakuzoqhutshwa uhlobo olukhethekile lwamandla olubizwa ngokuthi amandla e-inflationary, okwakungaba nesibopho ekudaleni yonke indawo yonke ebonakalayo.
Esinye isici esiyinhloko se-inflationary theory ukuthi iphakamisa ukuthi amandla okwehla kwamandla emali asheshe aphela ngemva kokwanda kokuqala, okuvumela indawo yonke ukuba ingene esigabeni sokwandisa kancane kancane esiye saqhubeka kuze kube yilolu suku. Ngaphezu kwalokho, ithiyori ye-inflation iphakamisa ukuthi lokhu kwanda kokuqala bekungaba nesibopho sokwakheka kwezakhiwo ezinkulu endaweni yonke.
Ukubaluleka kwethiyori ye-inflationary
Ukubaluleka kwethiyori ye-inflation kusezindaweni eziningana. Okokuqala nje, ichaza ukuthi kwenzeka kanjani ukuba indawo yonke yahluke kangaka ekwakhiweni kwayo ngezinga elikhulu. Ngaphambi kokwehla kwamandla emali, kwakukholelwa ukuthi indawo yonke inesiphithiphithi, kunokuhlukahluka okuphawulekayo kokuminyana kanye nezinga lokushisa lezinto ezifundeni ezihlukahlukene. Ukwehla kwamandla emali kuvumela lokhu kuguquguquka ukuthi kwande futhi kube bushelelezi ukuze kubangele ukusatshalaliswa kwendaba okulinganayo.
Okwesibili, inkolelo-mbono yokwenyuka kwamanani emali ibikezela ukuba khona kwamagagasi adonsela phansi endaweni yonke, okuye kwaqinisekiswa ukuphawulwa kwamuva nje. Lawa maza abalulekile ngoba anikeza ubufakazi obuqondile bomkhathi wokuqala wokwehla kwamandla emali futhi angasiza ukuqonda kangcono imvelo yamandla adonsela phansi nezinto ezikhona endaweni yonke.
Okwesithathu, ithiyori ye-inflation ingasiza ukuxazulula izinkinga kwezinye izindawo ze-theoretical physics, njenge-particle physics kanye ne-quantum cosmology. Ngokwesibonelo, ingachaza ukuthi kungani indawo yonke ibonakala inamandla amnyama angaguquki, okunzima ukuwachaza ngezinye izinkolelo-mbono.
Ithiyori ye-Inflationary ibalulekile ngoba isisiza ukuthi siqonde kangcono indawo yonke futhi sixazulule izinkinga emikhakheni eyahlukene ye-theoretical physics. Ukwengeza, ukuhlolwa kokubuka nokuhlola kwethiyori yokwehla kwamandla emali kuqinise ukuthembela kwethu ekuba semthethweni kwe-physics yesimanje.
izinkinga elizixazululayo
Ukwehla kwamandla emali kuxazulula izinkinga ezimbalwa ku-Big Bang cosmology ezavezwa eminyakeni yawo-1970. Lezi zinkinga zivela ekuqapheliseni ukuthi ukuze sifane nendawo yonke namuhla, indawo yonke kufanele iqale "ezimweni ezikhethekile" noma ezincane kakhulu zokuqala. Kucushwe i-Big Bang. Ukwehla kwamandla emali kuzixazulula lezi zinkinga ngokunikeza indlela eguquguqukayo eletha indawo yonke kulesi simo, okwenza indawo yonke ifane neyethu kumongo wenkolelo-mbono yokuqhuma okukhulu.
i-cosmic inflation idlala indima ebalulekile ekuxazululeni i-heterogeneity, i-anisotropy, kanye nokugoba kwendawo. Lokhu kushiya indawo yonke esimweni esilula kakhulu lapho ibuswa ngokuphelele inkambu ye-inflaton, okuwukuphela kwe-heterogeneity ephawulekayo ukuguquguquka kwe-quantum okubuthakathaka ku-inflaton. Ukunwetshwa kuphinda kuhlukanise izinhlayiya ezisindayo zangaphandle, njengama-monopole kazibuthe abikezelwa izandiso eziningi ze-Standard Model ye-particle physics. Ukube i-Universe ibishisa ngokwanele ukuba yenze izinhlayiya ezinjalo zangaphambi kokwehla kwamandla emali, bezingeke zibonwe emvelweni ngoba ziyivelakancane kangangokuthi cishe azikho nhlobo endaweni ebonwayo. Ngokuhlangene le miphumela yaziwa ngokuthi "i-inflationary no-hair theorem", efana ne-no-hair theorem yezimbobo ezimnyama.
I-"no hair theorem" empeleni ingenxa yokuthi indawo yonke yanda ngento enkulu phakathi nokwanda kwayo. Emkhathini okhulayo, ukuminyana kwamandla ngokuvamile kuyehla njengoba umthamo wendawo yonke ukhula. Isibonelo, ukuminyana kwento evamile "ebandayo" (uthuli) ihambisana ngokuphambene nevolumu: lapho ubukhulu bomugqa buphindwe kabili, ukuminyana kwamandla kuncipha izikhathi eziyisishiyagalombili. Njengoba indawo yonke ikhula, ukuminyana kwamandla okukhazimulayo kwehla ngokushesha okukhulu: lapho ubukhulu bomugqa buphindeka kabili, ukuminyana kwamandla okukhazimulayo kwehla izikhathi eziyishumi nesithupha. Ngesikhathi sokwehla kwamandla emali, ukuminyana kwamandla emkhakheni wokwehla kwamandla emali kucishe kube njalo. Kodwa-ke, ukuminyana kwamandla we-heterogeneity, i-curvature, i-anisotropy, nezinhlayiya ezingavamile ziyehla futhi, ngokunwetshwa okwanele, ziba yinto encane. Lokhu kwashiya indawo yonke engenalutho, eyisicaba, elinganayo, egcwele imisebe lapho ukunwetshwa kuphela.
Ngithemba ukuthi ngalolu lwazi ungafunda kabanzi mayelana ne-inflation theory kanye nezici zayo.