Sawubona, bahlali baseKhabro! Kungenzeka yini ukukhuluma ngemfashini, ukholo noma inganekwane kusayensi eyisisekelo?
Umkhathi awunandaba nemfashini yomuntu. Isayensi ayinakuchazwa njengokholo, ngoba izinkulumo zesayensi zihlala zivivinywa ngokuqinile futhi ziyalahlwa ngokushesha nje lapho imfundiso yenkolo iqala ukungqubuzana neqiniso eliwumgomo. Futhi amaphupho ngokuvamile awanaki kokubili amaqiniso nokunengqondo. Noma kunjalo, uRoger Penrose omkhulu akafuni ukwenqaba ngokuphelele lezi zenzakalo, ngoba imfashini yesayensi ingaba injini yenqubekelaphambili, ukholo luvela lapho inkolelo-mbono iqinisekiswa ukuhlolwa kwangempela, futhi ngaphandle kokundiza kwefantasy umuntu akakwazi ukuqonda zonke izimangaliso zethu. Umkhathi.
Esahlukweni esithi "Imfashini", uzofunda mayelana nethiyori yezintambo, ithiyori esemfashinini yamashumi eminyaka akamuva. "Ukholo" lunikezelwe ezimfundisweni lapho i-quantum mechanics ime khona. Futhi elithi “Fantasy” alikhathazeki ngalutho ngaphandle kwemibono yemvelaphi Yomhlaba Wonke eyaziwa yithi.
3.4. I-Big Bang Paradox
Ake siqale siphakamise umbuzo wokuqaphela. Yibuphi ubufakazi obuqondile obukhona bokuthi yonke i-Universe ebonakalayo yake yaba sesimweni esicindezela kakhulu nesishisa ngendlela emangalisayo esingahambisana nesithombe sokuqhuma okukhulu esivezwe kuSigaba 3.1? Ubufakazi obuqakatheke kakhulu yi-cosmic microwave background radiation (CMB), ngezinye izikhathi ebizwa ngokuthi i-big bang. Imisebe ye-CMB ilula, kodwa inobude beza obude kakhulu, ngakho-ke akunakwenzeka ngokuphelele ukuyibona ngamehlo akho. Lokhu kukhanya kuthululela phezu kwethu kuzo zonke izinhlangothi ngokulinganayo kakhulu (kodwa ikakhulukazi ngokungahambisani). Imele imisebe eshisayo enezinga lokushisa elingu-~2,725 K, okungukuthi, ngaphezu kwamadigri amabili ngaphezu kweziro ngokuphelele. “Ukucwebezela” okuphawuliwe kukholakala ukuthi kwavela endaweni eshisa ngendlela emangalisayo (~3000 K ngaleso sikhathi) cishe eminyakeni engu-379 ngemva kweBig Bang - phakathi nenkathi yokuhlakazeka kokugcina, lapho i-Universe iqala ukuphumela obala emisebeni kagesi (yize). lokhu akwenzekanga nhlobo ngesikhathi se-Big Bang) ukuqhuma; lesi sigameko senzeka engxenyeni yokuqala engu-000/1 yengqikithi yeminyaka Yomhlaba Wonke - kusukela ku-Big Bang kuze kube namuhla). Kusukela esikhathini sokugcina sokuhlakazeka, ubude bala maza okukhanya buye banda cishe njengoba i-Universe ngokwayo iye yanda (ngesilinganiso esingaba ngu-40), kangangokuthi ukuminyana kwamandla kuye kwehle kakhulu ngendlela efanayo. Ngakho-ke, izinga lokushisa elibonwayo le-CMB lingu-000 K kuphela.
Iqiniso lokuthi le misebe empeleni ayihambisani (okungukuthi, eshisayo) iqinisekiswa ngokumangazayo yiyona kanye imvamisa yayo, eboniswe ku-Fig. 3.13. Ukuqina kwemisebe kufrikhwensi ngayinye ethile kuhlelwa ngokuma kugrafu, futhi imvamisa iyanda ukusuka kwesokunxele kuye kwesokudla. Ijika eliqhubekayo lihambisana ne-Planck blackbody spectrum okukhulunywe ngayo eSigabeni 2.2 ngezinga lokushisa elingu-2,725 K. Amaphoyinti akujika ayidatha evela ekubhekisisweni okuqondile okunikezwa amabha wamaphutha. Ngasikhathi sinye, imigoqo yephutha ikhuphuka izikhathi ezingama-500, ngoba ngaphandle kwalokho bekungeke kwenzeke ukucatshangelwa, ngisho ngakwesokudla, lapho amaphutha efinyelela khona umkhawulo wawo. Isivumelwano phakathi kwejika lethiyori kanye nemiphumela yokuqaphela simane siphawuleka—mhlawumbe isivumelwano esihle kakhulu ne-thermal spectrum etholakala endalweni.
Nokho, lokhu kuvumelana kubonisani? Iqiniso lokuthi sicabangela isimo, ngokusobala, esasisondelene kakhulu ne-thermodynamic equilibrium (yingakho igama elithi incoherent lisetshenziswe ngaphambili). Kodwa isiphi isiphetho esilandela eqinisweni lokuthi i-Universe esanda kudalwa yayisondelene kakhulu ne-thermodynamic equilibrium? Masibuyele kuFig. 3.12 kusukela esigabeni 3.3. Isifunda esinabile kakhulu esimahhadlahhadla sizoba (ngokwencazelo) sibe sikhulu kakhulu kunanoma yisiphi esinye isifunda esinjalo, futhi sizoba sikhulu kakhulu uma siqhathaniswa nezinye kangangokuthi sizozenza zibe mncane kakhulu! I-Thermodynamic equilibrium ihambisana nesimo se-macroscopic, okungenzeka ukuthi, noma iyiphi isistimu izofika ngokushesha noma kamuva. Ngezinye izikhathi kubizwa ngokuthi ukufa okushisayo kwe-Universe, kodwa kulokhu, ngokumangalisayo, kufanele sikhulume ngokuzalwa okushisayo kwe-Universe. Isimo siba nzima yiqiniso lokuthi i-Universe esanda kuzalwa yanda ngokushesha, ngakho isimo esisicabangelayo empeleni asilingani. Noma kunjalo, ukwanda kuleli cala kungabhekwa njenge-adiabatic - leli phuzu laziswa ngokugcwele nguTolman emuva ku-1934 [Tolman, 1934]. Lokhu kusho ukuthi inani le-entropy alizange lishintshe phakathi nokunwetshwa. (Isimo esifana nalesi, lapho ukulingana kwe-thermodynamic kugcinwa ngenxa yokwanda kwe-adiabatic, kungachazwa esikhaleni sesigaba njengeqoqo lezifunda ezinomthamo olinganayo nokwahlukanisa okusanhlamvu okuqinile, okuhlukile komunye nomunye kuphela ngamavolumu athile e-Universe. . Singacabanga ukuthi lesi simo esiyinhloko besibonakala nge-entropy ephezulu - naphezu kokunwetshwa!).
Ngokusobala, sibhekene nendida engavamile. Ngokuvumelana nezimpikiswano ezethulwe eSigabeni 3.3, uMthetho Wesibili udinga (futhi, ngokomthetho, ochazwa) I-Big Bang ukuthi ube yisifunda esine-entropy ephansi kakhulu. Kodwa-ke, ukubonwa kwe-CMB kubonakala kukhombisa ukuthi isimo se-Big Bang siphawulwe nge-entropy enkulu, mhlawumbe nobukhulu obungenzeka. Kuphi lapho siphutha kakhulu kangaka?
Nansi incazelo eyodwa evamile yale ndida: kucatshangwa ukuthi, njengoba i-Universe esanda kuzalwa "yayincane" kakhulu, kungase kube nomkhawulo we-entropy enkulu, futhi isimo sokulingana kwe-thermodynamic, okusobala ukuthi sasigcinwa ngaleso sikhathi, sasikhona. umane umkhawulo ezingeni entropy kungenzeka ngaleso sikhathi. Nokho, lena impendulo engalungile. Isithombe esinjalo singahambisana nesimo esihluke ngokuphelele, lapho ubukhulu be-Universe buzoncika ekuvimbeleni okuthile kwangaphandle, isibonelo, njengasendabeni yegesi equkethwe ku-cylinder ene-piston evaliwe. Kulokhu, ukucindezela kwe-piston kuhlinzekwa ngenye indlela yangaphandle, efakwe umthombo wangaphandle (noma i-outlet) yamandla. Kodwa lesi simo asisebenzi ku-Universe wonkana, i-geometry namandla ayo, kanye “nobukhulu bayo bawo wonke,” kunqunywa kuphela ukwakheka kwangaphakathi futhi kubuswa izilinganiso eziguquguqukayo zethiyori evamile ka-Einstein yokuhlobana (okuhlanganisa Izibalo ezichaza isimo sendaba; bheka izigaba 3.1 no-3.2). Ngaphansi kwezimo ezinjalo (lapho izibalo zinquma ngokuphelele futhi zingaguquki ngokuphathelene nesiqondiso sesikhathi - bheka isigaba 3.3), ingqikithi yevolumu yesikhala sesigaba ayikwazi ukushintsha ngokuhamba kwesikhathi. Kucatshangwa ukuthi indawo yesigaba P ngokwayo akufanele "iguquke"! Konke ukuziphendukela kwemvelo kumane kuchazwe ngendawo yejika C esikhaleni P futhi kulokhu kumelela ukuguquguquka okuphelele kwe-Universe (bheka isigaba 3.3).
Mhlawumbe inkinga izocaca kakhudlwana uma sicabangela izigaba zakamuva zokuwohloka komkhathi, lapho kusondela i-Big Crash. Khumbula imodeli kaFriedman ka-K > 0, Λ = 0, eboniswe ku-Fig. 3.2a esigabeni 3.1. Manje sikholelwa ukuthi iziphazamiso kulo modeli zivela ekusabalaliseni okungajwayelekile kwezinto, futhi kwezinye izingxenye ukuwohloka kwendawo sekuvele kwenzeka, okushiya izimbobo ezimnyama endaweni yazo. Khona-ke kufanele sicabange ukuthi ngemva kwalokhu ezinye izimbobo ezimnyama zizohlangana zodwa futhi ukugoqeka kube ubunye bokugcina kuzophenduka inqubo eyinkimbinkimbi kakhulu, cishe akukho lutho olufana ngayo ne-Big Crash ehambisanayo eqinile ye-symmetric eyisiyingi ka-Friedmann. imodeli ethulwe ku-Fig. 3.6 a. Ngokuphambene nalokho, ngokwemibandela yekhwalithi, isimo sokuwa sizosikhumbuza kakhulu ukungcola okukhulu okuboniswe ku-Fig. 3.14 a; ubunye obuwumphumela obuvela kulesi simo, ngokwezinga elithile, bungase buhambisane nenkolelo-mbono ye-BCLM okukhulunywe ngayo ekupheleni kwesigaba 3.2. Isimo sokugcina sokuwa sizoba ne-entropy engacabangeki, nakuba i-Universe izohlehla ibuyele kusayizi omncane. Nakuba le modeli ethile (evalwe ngokwendawo) egoqa kabusha imodeli kaFriedmann okwamanje ingathathwa njengemelela okubambekayo Yendawo Yonke yethu, ukucatshangelwa okufanayo kuyasebenza nakwamanye amamodeli kaFriedmann, anokuhambisana noma ngaphandle kokuguquguquka kwendawo yonke. Inguqulo ebhidlikayo yanoma iyiphi imodeli enjalo, ehlangabezana nokuphazamiseka okufanayo ngenxa yokusatshalaliswa okungalingani kwendaba, kufanele iphinde iphenduke isiphithiphithi esiqeda konke, ubunye obufana nomgodi omnyama (Fig. 3.14 b). Ngokuhlehlisa isikhathi endaweni ngayinye yalezi zifundazwe, sizofinyelela ebunyeni bokuqala obungase bube khona (okungaba yi-Big Bang), okunayo, ngokufanelekile, i-entropy enkulu, ephikisana nomcabango owenziwe lapha mayelana "nophahla" lwe-entropy (Fig. 3.14 c).
Lapha kufanele ngidlulele kwezinye izindlela ezibuye zicatshangelwe ngezinye izikhathi. Abanye osolwazi basikisela ukuthi umthetho wesibili kufanele ngandlela thize uzihlehlisele emuva kumamodeli anjalo adilikayo, ukuze ingqikithi ye-entropy yendawo yonke ibe ncane ngokuqhubekayo (ngemuva kokunwetshwa okukhulu) njengoba Ukuphahlazeka Okukhulu kusondela. Kodwa-ke, isithombe esinjalo sinzima kakhulu ukusicabanga lapho kukhona izimbobo ezimnyama, okuthi, lapho zakha, zizoqala ukusebenza ukwandisa i-entropy (ehlotshaniswa ne-asymmetry yesikhathi endaweni yezigaxa zero eduze nomkhathizwe womcimbi, bheka umfanekiso 3.9). Lokhu kuzoqhubeka kuze kube ikusasa elikude - okungenani kuze kube yilapho izimbobo ezimnyama zihwamuka ngaphansi kwethonya lomshini we-Hawking (bheka izigaba 3.7 no-4.3). Kunoma ikuphi, lokhu kungenzeka akuzisebenzisi izimpikiswano ezivezwe lapha. Kukhona enye inkinga ebalulekile ehlotshaniswa namamodeli anjalo abhidlikayo futhi okungenzeka ukuthi abafundi ngokwabo bake bacabanga ngakho: ukungafani kwezimbobo ezimnyama kungase kungaveli nhlobo ngesikhathi esisodwa, ngakho-ke lapho sihlehlisa isikhathi, ngeke sithole i-Big Bang, okwenzeka “konke futhi ngokushesha”. Kodwa-ke, lokhu kungenye yezimpawu ze-(engakafakazelwa, kodwa ekholisayo) yokucabanga okuqinile kwe-cosmic censorship [Penrose, 1998a; I-PkR, isigaba 28.8], ngokusho ukuthi, esimweni esivamile, ubunye obunjalo buyoba njengesikhala (isigaba 1.7), ngakho-ke singabhekwa njengomcimbi wesikhathi esisodwa. Ngaphezu kwalokho, kungakhathaliseki umbuzo wobuqiniso be-hypothesis eqinile ye-cosmic censorship ngokwayo, izixazululo eziningi ziyaziwayo ezanelisa lesi simo, futhi zonke izinketho ezinjalo (uma zandiswa) zizoba namanani aphezulu e-entropy. Lokhu kunciphisa kakhulu ukukhathazeka mayelana nokuba semthethweni kokutholakele kwethu.
Ngakho-ke, asibutholi ubufakazi bokuthi, uma kubhekwa ubukhulu bendawo obuncane boMkhathi, bekungaba khona “uphahla oluphansi” oluthile lwe-entropy engenzeka. Empeleni, ukunqwabelana kwendaba ngendlela yezimbobo ezimnyama kanye nokuhlanganiswa kobunye “bomgodi omnyama” kube isiphithiphithi esisodwa esisodwa kuyinqubo ehambisana ngokuphelele nomthetho wesibili, futhi le nqubo yokugcina kufanele ihambisane nokwanda okukhulu. ku-entropy. Isimo sokugcina se-Universe, "esincane" ngezindinganiso zejometri, singase sibe ne-entropy engacabangeki, ephakeme kakhulu kunasezigabeni zakuqala zemodeli ewayo yendawo yonke, futhi indawo encane ngokwayo ayibeki "uphahla" lwenani eliphakeme. ye-entropy, nakuba "uphahla" olunjalo (uma uhlehlisa ukuhamba kwesikhathi) lungachaza nje ukuthi kungani i-entropy yayiphansi kakhulu ngesikhathi seBig Bang. Eqinisweni, isithombe esinjalo (Fig. 3.14 a, b), ngokuvamile esimelela ukuwa kwe-Universe, siphakamisa isisombululo sendida: kungani ngesikhathi se-Big Bang kwakukhona i-entropy ephansi kakhulu uma kuqhathaniswa nalokho okungenzeka kube khona, naphezu kokuqhuma okukhulu. iqiniso lokuthi ukuqhuma kwakushisa (futhi isimo esinjalo kufanele sibe ne-entropy ephezulu). Impendulo iwukuthi i-entropy ingakhula kakhulu uma ukuphambuka okukhulu okuvela ekufaniseni kwendawo kuvunyelwe, futhi ukwanda okukhulu kwalolu hlobo kuhlotshaniswa nokungahambi kahle ngenxa yokuvela kwezimbobo ezimnyama. Ngenxa yalokho, i-Big Bang enendawo efanayo ingaba ne-entropy ephansi ngokumangalisayo, naphezu kweqiniso lokuthi okuqukethwe kuyo kwakushisa ngendlela emangalisayo.
Obunye bobufakazi obuqand' ikhanda bokuthi i-Big Bang ngempela yayifana ngokwendawo, ihambisana nejometri yemodeli ye-FLRU (kodwa ayihambisani nesimo esivamile kakhulu sobunye obuphazamisekile obuboniswe ku-Fig. 3.14c), futhi iyafika futhi. kusuka ku-RI, kodwa kulokhu nge-angular homogeneity kunesimo sayo se-thermodynamic. Le homogeneity ibonakala eqinisweni lokuthi izinga lokushisa le-RI liyafana kunoma yisiphi isikhathi esibhakabhakeni, futhi ukuphambuka kusuka ku-homogeneity akukho ngaphezu kwe-10-5 (kulungiselwe umphumela omncane we-Doppler ohambisana nokunyakaza kwethu ngendaba ezungezile. ). Ngaphezu kwalokho, kukhona cishe ukufana kwendawo yonke ekusabalaliseni imithala nezinye izinto; Ngakho-ke, ukusatshalaliswa kwamabhayoni (bheka Isigaba 1.3) ngezikali ezinkulu kakhulu kubonakala ngokufana okuphawulekayo, nakuba kukhona okungaqondakali okuphawulekayo, ikakhulukazi lokho okubizwa ngokuthi ama-voids, lapho ukuminyana kwezinto ezibonakalayo kuphansi kakhulu kunesilinganiso. Ngokuvamile, kungase kuthiwe i-homogeneity iphakeme kakhulu esikhathini esidlule se-Universe esibukeka ngayo, futhi i-RI iwubufakazi obudala kakhulu bokusabalalisa kwendaba esingayibona ngokuqondile.
Lesi sithombe sihambisana nombono wokuthi ekuqaleni kokukhula kwawo i-Universe empeleni yayifana kakhulu, kodwa inokuminyana okungajwayelekile. Ngokuhamba kwesikhathi (nangaphansi kwethonya lezinhlobo ezihlukahlukene “zokungqubuzana” - izinqubo ezehlisa ijubane ukunyakaza okuhlobene), lokhu kungahambi kahle kokuminyana kwaqina ngaphansi kwethonya lamandla adonsela phansi, okuhambisana nomqondo wokugoqana kancane kancane kwendaba. Ngokuhamba kwesikhathi, i-clumping iyanda, okuholela ekwakhekeni kwezinkanyezi; bahlangana babe imithala, ngamunye wabo ovula umgodi omkhulu omnyama phakathi nendawo. Ekugcineni, lokhu kugoqa kungenxa yomphumela ongenakugwemeka wamandla adonsela phansi. Izinqubo ezinjalo zihlotshaniswa ngempela nokwanda okunamandla kwe-entropy futhi zibonisa ukuthi, ngokucabangela amandla adonsela phansi, lelo bhola elikhanyayo lokuqala, okusele kulo i-RI kuphela namuhla, lingaba kude ne-entropy ephezulu. Imvelo eshisayo yaleli bhola, njengoba kufakazelwa i-Plack spectrum eboniswe ku-Fig. I-3.13, isho lokhu kuphela: uma sicabangela i-Universe (ngenkathi yokuhlakazeka kokugcina) njengesistimu ehlanganisa indaba namandla asebenzisanayo, khona-ke singacabanga ukuthi empeleni bekuku-equilibrium ye-thermodynamic. Nokho, uma futhi sicabangela amathonya adonsela phansi, isithombe sishintsha kakhulu.
Uma sicabanga, isibonelo, igesi esitsheni esivaliwe, khona-ke kungokwemvelo ukucabanga ukuthi izofinyelela i-entropy yayo ephezulu kuleso simo se-macroscopic lapho isakazwa ngokulinganayo kuwo wonke isitsha (Fig. 3.15 a). Kulokhu, izofana nebhola elishisayo elikhiqize i-RI, esabalaliswe ngokulinganayo esibhakabhakeni. Kodwa-ke, uma ushintsha ama-molecule egesi ngohlelo olukhulu lwemizimba exhunywe komunye nomunye ngamandla adonsela phansi, isibonelo, izinkanyezi ngazinye, uthola isithombe esihluke ngokuphelele (Fig. 3.15 b). Ngenxa yemiphumela yamandla adonsela phansi, izinkanyezi zizosatshalaliswa ngokungalingani, ngendlela yamaqoqo. Ekugcineni, i-entropy enkulu kakhulu izotholwa lapho izinkanyezi eziningi ziwa noma zihlangana zibe izimbobo ezimnyama. Nakuba le nqubo ingase ithathe isikhathi eside (yize izokwenziwa lula ukungqubuzana ngenxa yokuba khona kwegesi ye-interstellar), sizobona ukuthi ekugcineni, lapho amandla adonsela phansi ebusa, i-entropy iphakeme, kancane kancane indaba isatshalaliswa ohlelweni. .
Imiphumela enjalo ingalandelelwa ngisho nasezingeni lokuhlangenwe nakho kwansuku zonke. Omunye angase abuze: ithini indima yoMthetho Wesibili ekugcineni ukuphila eMhlabeni? Ngokuvamile ungezwa ukuthi siphila kulo mhlaba ngenxa yamandla atholakala eLangeni. Kodwa lesi akusona isitatimende esiyiqiniso ngokuphelele uma sicabangela uMhlaba uwonke, njengoba cishe wonke amandla atholwa uMhlaba emini asheshe ahwamuke aye emkhathini, aye esibhakabhakeni esimnyama ebusuku. (Yebo, ukulingana okuqondile kuzolungiswa kancane yizici ezinjengokufudumala kwembulunga nokushisisa kweplanethi ngenxa yokubola kwemisebe.) Uma kungenjalo, uMhlaba ubuyomane ushise kakhulu futhi ungahlali muntu phakathi nezinsuku ezimbalwa! Kodwa-ke, ama-photon atholwe ngokuqondile eLangeni ane-frequency ephezulu uma kuqhathaniswa (agxile engxenyeni ephuzi ye-spectrum), futhi uMhlaba ukhiphela ama-photon aphansi kakhulu ku-spectrum ye-infrared emkhathini. Ngokwefomula ka-Planck (E = hν, bheka isigaba 2.2), i-photon ngayinye efika evela eLangeni ngayinye inamandla amakhulu kakhulu kunama-photon akhishwa emkhathini, ngakho-ke, ukuze kutholakale ibhalansi, ama-photon amaningi kufanele ahambe eMhlabeni kunokufika ( bheka umfanekiso 3.16). Uma ama-photon ambalwa efika, khona-ke amandla angenayo azoba namadigri ambalwa enkululeko futhi amandla aphumayo azoba nokuningi, ngakho-ke, ngokusho kwefomula kaBoltzmann (S = k log V), ama-photons angenayo azoba ne-entropy encane kakhulu kunalawo aphumayo. . Sisebenzisa amandla ane-entropy ephansi aqukethwe ezitshalweni ukuze sehlise i-entropy yethu: sidla izitshalo noma izilwane ezidla uhlaza. Kunjalo ukuphila eMhlabeni kusinda futhi kuchuma. (Ngokusobala, le micabango yaqala ukucaciswa ngokucacile ngu-Erwin Schrödinger ngo-1967, lapho ebhala incwadi yakhe yenguquko ethi Life as It Is [Schrödinger, 2012]).
Iqiniso elibaluleke kakhulu ngalebhalansi ye-entropy ephansi yileli: ILanga liyindawo eshisayo esibhakabhakeni esimnyama ngokuphelele. Kodwa zavela kanjani izimo ezinjalo? Izinqubo eziningi eziyinkimbinkimbi zadlala indima, kuhlanganise nalezo ezihambisana nokusabela kwe-thermonuclear, njll., kodwa into ebaluleke kakhulu ukuthi iLanga likhona nhlobo. Futhi kwavela ngenxa yokuthi i-solar (njengendaba eyenza ezinye izinkanyezi) yathuthukiswa ngenqubo yokudonsela phansi, futhi konke kwaqala ngokusatshalaliswa okufanayo kwegesi nezinto ezimnyama.
Lapha sidinga ukusho into engaqondakali ebizwa ngokuthi i-dark matter, ngokusobala eyenza u-85% wokuqukethwe (okungeyona i-Λ) ye-Universe, kodwa itholwa kuphela ngokusebenzisana kwamandla adonsela phansi, futhi ukwakheka kwayo akwaziwa. Namuhla sicabangela le ndaba lapho silinganisa isamba sengqikithi, edingekayo lapho kubalwa amanani athile ezinombolo (bheka izigaba 3.6, 3.7, 3.9, nokuthi iyiphi indima ebaluleke kakhulu yethiyori engadlalwa indaba emnyama, bheka isigaba 4.3). Ngaphandle kodaba olumnyama, sibona ukuthi ibaluleke kangakanani imvelo ephansi yokusatshalaliswa kwento efanayo ezimpilweni zethu. Ukuba khona kwethu, njengoba sikuqonda, kuncike endaweni engaphansi kwe-entropy gravitational reserve ewuphawu lokusatshalaliswa okufanayo kwento yokuqala.
Lapha sifika esicini esimangalisayo—empeleni, esimangalisayo—se-Big Bang. Impicabadala ayigcini nje ngokuthi kwenzeke kanjani, kodwa naseqinisweni lokuthi kwakuwumcimbi ophansi kakhulu we-entropy. Ngaphezu kwalokho, okuphawulekayo akusona lesi simo kakhulu njengoba iqiniso lokuthi i-entropy yayiphansi kuphela ngenhlonipho eyodwa, okungukuthi: amazinga adonsela phansi enkululeko, ngasizathu simbe, acindezelwa ngokuphelele. Lokhu kuhluke kakhulu kumadigri enkululeko yendaba kanye nemisebe (ye-electromagnetic), njengoba bebonakala bejabule kakhulu endaweni eshisayo ene-entropy ephezulu. Ngokombono wami, lena mhlawumbe imfihlakalo ejulile ye-cosmological, futhi ngesizathu esithile isalokhu ithathwa kancane!
Kudingekile ukuba uhlale ngokuningiliziwe mayelana nokuthi isimo se-Big Bang sasikhethekile kangakanani nokuthi iyiphi i-entropy engavela ohlelweni lokudonsa amandla adonsela phansi. Ngakho-ke, okokuqala udinga ukuqaphela ukuthi iyiphi i-entropy emangalisayo engokwemvelo emgodini omnyama (bheka umfanekiso 3.15 b). Lolu daba sizoludingida esigabeni 3.6. Kodwa okwamanje, ake siphendukele kwenye inkinga ehlobene nalokhu okulandelayo, okungenzeka kakhulu: ngemva kwakho konke, i-Universe ingase ibonakale ingapheli ngokwendawo (njengoba kwenzeka kumamodeli e-FLRU ane-K. 0, bheka isigaba 3.1) noma okungenani ingxenye enkulu ye-Universe ingase ingabonakali ngokuqondile. Ngakho-ke, sibhekana nenkinga ye-cosmological horizons, esizoxoxa ngayo esigabeni esilandelayo.
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Source: www.habr.com