🥇Incwadi ethi "Imfashini, Ukholo, Amaphupho kanye Nefiziksi Entsha Yomhlaba Wonke"

Sawubona, bahlali baseHabro! Kungenzeka yini ukukhuluma ngemfashini, ukholo, noma inganekwane esayensini eyisisekelo?

I-Universe ayinandaba nemfashini yomuntu. Isayensi ayinakuchazwa njengokholo, njengoba izinkulumo zesayensi zihlala zihlolwa ngokuqinile futhi ziyalahlwa ngokushesha nje lapho imfundiso yenkolo iqala ukungqubuzana neqiniso eliwumgomo. Futhi inganekwane ngokuvamile ayiwanaki kokubili amaqiniso nokunengqondo. Noma kunjalo, uRoger Penrose omkhulu akazimisele ukuzichitha ngokuphelele lezi zenzakalo, njengoba imfashini yesayensi ingaba umshayeli wenqubekelaphambili, ukholo luvela lapho inkolelo-mbono iqinisekiswa ukuhlola kwangempela, futhi ngaphandle kokuthatha umcabango, asikwazi ukuqonda konke okuyinqaba komkhathi wethu.

Esahlukweni esithi "Imfashini", uzofunda mayelana nethiyori yezintambo—ithiyori esemfashinini yamashumi eminyaka akamuva. "Ukholo" lunikezelwe ezimfundisweni eziyisisekelo ze-quantum mechanics. Futhi elithi "Fantasy" alikhathazi lutho ngaphandle kwemibono yemvelaphi yendawo yonke eyaziwayo.

3.4 I-Big Bang Paradox

Ake siqale sibhekane nombuzo wokuqaphela. Yibuphi ubufakazi obuqondile obukhona bokuthi wonke umkhathi obonakalayo wake waba sesimweni esicindezelayo nesishisa ngendlela emangalisayo, ngokuhambisana nesithombe sokuqhuma okukhulu esivezwe kuSigaba 3.1? Ubufakazi obuqakatheke kakhulu yisizinda se-cosmic microwave (CMB), kwesinye isikhathi esibizwa ngokuthi i-Big Bang glow. I-CMB ilula, kodwa inobude obude ngokwedlulele, iyenza ingabonakali ngokuphelele ngeso lenyama. Lokhu kukhanya kukhanya phezu kwethu kuzo zonke izinhlangothi, ngendlela efanayo kakhulu (kodwa ngokuvamile ngokungahambisani). Kuyimisebe eshisayo enezinga lokushisa elingu ~2,725 K, noma ngaphezu kwamadigri amabili ngaphezu kweziro ngokuphelele. "Ukucwebezela" okuphawuliwe kucatshangwa ukuthi kwavela endaweni eshisa ngendlela emangalisayo (~3000 K ngaleso sikhathi) cishe eminyakeni engu-379,000 ngemva kweBig Bang - phakathi nenkathi yokuhlakazeka kokugcina, lapho umkhathi uqala obala emisebeni kazibuthe (nakuba lokhu kungenzeki kuBig Bang, lesi senzakalo sokuqala se-Universe iminyaka—kusuka ku-Big Bang kuze kube namuhla). Kusukela esikhathini sokuhlakazeka kokugcina, ubude begagasi balawa maza okukhanya bukhuphuke cishe ngenani elifanayo nelokuthi i-Universe ngokwayo iye yanda (cishe izikhathi ezingu-1100), ngakho ukuminyana kwamandla kuye kwehle ngendlela emangalisayo. Ngakho-ke, izinga lokushisa elibonwayo le-CMB lingu-2,725 K kuphela.

Iqiniso lokuthi le misebe empeleni ayihambisani (okungukuthi, ukushisa) iqinisekiswa ngokumangazayo imvelo ye-spectrum yayo, eboniswe kuMfanekiso 3.13. I-eksisi eqondile yegrafu imelela ukushuba kwemisebe kufrikhwensi ngayinye ethile, nemvamisa ekhuphukayo ukusuka kwesokunxele kuye kwesokudla. Ijika eliqhubekayo lihambisana ne-Planck spectrum ye-blackbody, okuxoxwe ngayo kuSigaba 2.2, ngezinga lokushisa elingu-2,725 K. Amaphuzu aku-curve amelela ukubhekwa okuqondile, okuhlinzekwa ngamabha amaphutha. Amabha amaphutha enziwa ihaba ngenani elingu-500, ngoba uma kungenjalo bekungeke kwenzeke ukubonwa, ngisho kwesokudla, lapho amaphutha amakhulu kakhulu. Isivumelwano phakathi kwejika lethiyori nedatha yokuqaphela siyaphawuleka nje—mhlawumbe ukufana okuhle kakhulu ne-thermal spectrum eyake yatholakala emvelweni.

Incwadi ethi “Fashion, Faith, Fantasy and the New Physics of the Universe”
Kodwa lokhu kuvumelana kubonisani? Ukuthi sicabangela isimo ngokusobala ebesisondelene kakhulu ne-thermodynamic equilibrium (yingakho igama elithi alihlangani). Kodwa kusho ukuthini ukuthi i-Universe esanda kwakhiwa yayisondelene kakhulu ne-thermodynamic equilibrium? Ake sibuyele kuMdwebo 3.12 sisuka eSigabeni 3.3. Isifunda esikhulu kunazo zonke esinama-coarse-grained (ngokwencazelo) sizoba sikhulu kakhulu kunanoma yisiphi esinye isifunda esinjalo, futhi, njengomthetho, sikhulu kakhulu uma siqhathaniswa nabanye ukuthi sizodlula kakhulu umthamo wabo! I-Thermodynamic equilibrium ihambisana nesimo se-macroscopic, umuntu angasilindela, noma iyiphi isistimu izogcina ifinyelele. Ngezinye izikhathi kubizwa ngokuthi ukufa okushisayo kwe-Universe, kodwa kulokhu, ngokungavamile, 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-iphuzu elaziswa ngokugcwele nguTolman emuva ku-1934 [Tolman, 1934]. Lokhu kusho ukuthi inani le-entropy alizange lishintshe ngesikhathi sokunwetshwa. (Isimo esinjengalesi, lapho ukulingana kwe-thermodynamic kugcinwa khona ngenxa yokwandiswa kwe-adiabatic, kungachazwa esikhaleni sesigaba njengesethi yezifunda ezilinganayo ezinomthamo we-coarse-graining partitioning, ehluke komunye nomunye kuphela emiqulwini ethile yendawo yonke. Lesi simo sokuqala singabhekwa njengesibonakaliso sokwanda ngaphandle kokunwetshwa okukhulu!)

Sibonakala sibhekene nendida eyodwa. Ngokuvumelana nezimpikiswano ezethulwe eSigabeni 3.3, uMthetho Wesibili udinga (futhi, ngokomthetho, uchazwa) yi-Big Bang ukuthi kube yisifunda esikhulu esine-entropy ephansi kakhulu. Kodwa-ke, ukubonwa kwe-CMB kubonakala kukhombisa ukuthi isimo se-Big Bang sasibonakala nge-entropy enkulu, mhlawumbe ephakeme kakhulu ngangokunokwenzeka. Kuphi lapho senza iphutha elikhulu kangaka?

Incazelo eyodwa evamile yalendida ukuthi, ngenxa yokuthi indawo ezungezile “yayimncane,” kumelwe ukuba kwakunomkhawulo othile ku-entropy yayo enkulu, futhi isimo sokulingana kwe-thermodynamic okwakusobala ukuthi sasikhona ngaleso sikhathi kwakumane kuyizinga eliphezulu le-entropy elalingenzeka ngaleso sikhathi. Nokho, lena impendulo engalungile. Isithombe esinjalo singahambisana nesimo esihluke ngokuphelele, lapho ubukhulu bendawo yonke buncike ekuvimbeleni okuthile kwangaphandle, njengegesi evalelwe kusilinda nepiston evaliwe. Esimweni esinjalo, ukucindezela kwe-piston kunikezwa indlela ethile yangaphandle, efakwe umthombo wangaphandle (noma i-outlet) yamandla. Kodwa lesi simo asisebenzi endaweni yonke, i-geometry namandla ayo, kanye "nobukhulu bayo bawo wonke," kunqunywa kuphela ukwakheka kwawo kwangaphakathi futhi kubuswa ukulingana okuguquguqukayo kwethiyori evamile ka-Einstein yokuhlobana (kuhlanganise nezibalo ezichaza isimo sendaba; bheka Izigaba 3.2 no-3.1). Ngaphansi kwalezi zimo (lapho izibalo zinquma ngokuphelele futhi zingaguquki ngokuphathelene nesiqondiso sesikhathi—bona Isigaba 3.3), isamba sevolumu yesikhala sesigaba asikwazi ukushintsha ngokuhamba kwesikhathi. Lokhu kusho ukuthi indawo yesigaba P ngokwayo akufanele "iguquke"! Konke ukuziphendukela kwemvelo kuchazwa kalula njengendawo yejika C esikhaleni esingu-P futhi, kulokhu, kumelela ukuvela okuphelele kwendawo yonke (bona Isigaba 3.3).

Incwadi ethi “Fashion, Faith, Fantasy and the New Physics of the Universe”
Mhlawumbe inkinga iba sobala kakhulu uma sicabangela izigaba zokugcina zokubhidlika komkhathi, njengoba kusondela i-Big Crash. Khumbula imodeli kaFriedmann ye-K > 0, Λ = 0, eboniswe ku-Fig. 3.2a kuSigaba 3.1. Manje sicabanga ukuthi ukuphazamiseka kule modeli kuvela ekusabalaleni okungajwayelekile kwento, nokuthi kwezinye izingxenye ukuwohloka kwendawo sekuvele kwenzekile, okushiya ngemuva izimbobo ezimnyama. Khona-ke kufanele sicabange ukuthi ezinye izimbobo ezimnyama zizobe sezihlangana zodwa futhi ukugoqeka ebunyeni bokugcina kuzophenduka inqubo eyinkimbinkimbi kakhulu, cishe engenalutho efana ne-Big Crash eqinile elinganayo yemodeli ye-Friedmann eyindilinga eyindilinga eboniswe ku-Fig. 3.6a. Ngokuphambene nalokho, ngokwekhwalithi isimo sokuwa sizokhumbuza kakhulu isiphithiphithi esikhulu esiboniswe ku-Fig. 3.14a; Ubunye obuwumphumela bungase buhambisane ngandlela-thile nenkoleloze ye-BCLM okukhulunywe ngayo ekupheleni kweSigaba 3.2. Isimo sokugcina sokuwa singaba ne-entropy engacabangeki, naphezu kokuthi Umkhathi uhlehla waba usayizi omncane. Nakuba le modeli ethile (evalwe ngokwendawo) egoqa kabusha imodeli kaFriedmann okwamanje ingabhekwa njengokumelela okubambekayo kwe-Universe yethu siqu, ukucatshangelwa okufanayo kusebenza kwamanye amamodeli kaFriedmann, anokuhambisana noma ngaphandle kwe-cosmological constant. Inguqulo egoqayo yanoma iyiphi imodeli enjalo, ehlangabezana nokuphazamiseka okufanayo ngenxa yokusatshalaliswa okungalingani kwezinto, izophinde iwele ibe yisiphithiphithi esiqeda konke, ubunye obufana nembobo emnyama (Umfanekiso 3.14b). Ngokuhlehlisa isikhathi endaweni ngayinye yalezi zifundazwe, sifinyelela ebunyeni bokuqala obungase bube khona (i-Big Bang engaba khona), okuthi, ngokufanelekile, ibe ne-entropy enkulu, ephikisana nomcabango ovezwe lapha mayelana “nophahla” lwe-entropy (Fig. 3.14c).

Lapha kufanele ngiphendukele kwamanye amathuba nawo acatshangelwa ngezinye izikhathi. Abanye osolwazi basikisela ukuthi umthetho wesibili kumele ngandlela thize uhlehlise amamodeli anjalo, ukuze ingqikithi ye-entropy ye-Universe izoba yincane kakhulu (ngemuva kokwanda okukhulu) njengoba i-Big Crunch isondela. Kodwa-ke, lesi sithombe sinzima kakhulu ukucabanga phambi kwezimbobo ezimnyama, ezithi, lapho kwakhiwa, zizobe ngokwazo zenze ukwandisa i-entropy (ngenxa ye-asymmetry yesikhathi ekuhlelweni kwama-null cones eduze nomkhathizwe womcimbi, bheka Fig. 3.9). Lokhu kuzoqhubeka kuye esikhathini esizayo esikude—okungenani kuze kube yilapho izimbobo ezimnyama zihwamuka ngaphansi komshini we-Hawking (bona Izigaba 3.7 kanye no-4.3). Kunoma ikuphi, ukuba nokwenzeka okunjalo akuzisebenzisi izimpikiswano ezivezwe lapha. Kukhona enye inkinga ebalulekile ehlotshaniswa namamodeli anjalo okugoqa ayinkimbinkimbi, okungenzeka abafundi bazicabangele bona: ubunye bembobo emnyama kungenzeka bungaveli kanyekanye, ukuze ukuguqulwa kwesikhathi kungakhiqizi i-Big Bang eyenzeka "ngasikhathi sinye." Nokho, lokhu kungenye yezimpawu ze-(ongakaqinisekiswa, kodwa ezikholisayo) i-cosmic censorship hypothesis eqinile [Penrose, 1998a; I-R&D, Isigaba 28.8], ngokuya ngokuthi, esimweni esivamile, ubunye obunjalo buzofana nomkhathi (Isigaba 1.7), ngakho-ke kungabhekwa njengomcimbi wesikhathi esisodwa. Ngaphezu kwalokho, kungakhathaliseki umbuzo wobuqiniso be-hypothesis eqinile ye-cosmic censorship ngokwayo, izixazululo eziningi ziyaziwayo ezenelisa lesi simo, futhi zonke izinhlobo ezinjalo (ngaphansi kokunwetshwa) zizoba namanani aphezulu we-entropy. Lokhu kunciphisa kakhulu izinga lokukhathazeka mayelana nokuba semthethweni kweziphetho zethu.

Ngakho-ke, asitholi bufakazi bokuthi "uphahla oluphansi" lwe-entropy engenzeka lungaba khona ngempela ku-Universe uma kubhekwa ubukhulu bayo bendawo encane. Empeleni, ukuhlanganiswa kwezinto ngendlela yezimbobo ezimnyama kanye nokuhlanganiswa kwezinhlamvu "zembobo emnyama" zibe isiphithiphithi esisodwa esisodwa kuyinqubo evumelana ngokuphelele noMthetho Wesibili, futhi le nqubo yokugcina kufanele ihambisane nokwanda okukhulu kwe-entropy. Isimo sokugcina se-Universe, "esincane" ngezindinganiso zejiyomethri, singaba ne-entropy engacabangeki, ephakeme kakhulu kunasezigabeni zokuqala zokuwa kwemodeli yendawo yonke, kanye ne-miniaturization yendawo ngokwayo ayisunguli "uphahla" lwenani eliphakeme le-entropy, nakuba "uphahla" olunjalo (ngaphansi kwesikhathi lwalungachaza ngokuhlehlisayo) ukuthi kungani i-bag ehlehlisiwe. Eqinisweni, lesi sithombe (Fig. 3.14 a, b), ngokuvamile esibonisa ukuwa kwe-Universe, siphakamisa isisombululo sendida: kungani i-Big Bang ibe ne-entropy ephansi kakhulu uma iqhathaniswa nalokho okungenzeka yayinakho, naphezu kokuqhuma kushisa (futhi isimo esinjalo kufanele sibe ne-entropy ephezulu). Impendulo iwukuthi i-entropy ingakhula kakhulu uma ukuphambuka okuphawulekayo okuvela ku-homogeneity yendawo kuvunyelwe, futhi ukwanda okukhulu kwalolu hlobo kuhlotshaniswa nokungahambi kahle okubangelwa ngokuqondile ukwakheka kwezimbobo ezimnyama. Ngakho-ke, i-Big Bang enendawo efanayo yayingaba ne-entropy ephansi ngokumangalisayo, naphezu kweqiniso lokuthi okuqukethwe kuyo kwakushisa ngendlela emangalisayo.

Obunye bobufakazi obuqand’ ikhanda bokuthi i-Big Bang ngempela yayifana ncamashí nendawo, ihambisana nejometri yemodeli ye-FLUE (kodwa ayihambisani necala elivamile kakhulu lobunye obuphazamisekile obuboniswe ku-Fig. 3.14c), iphinde ihlobene ne-CMB, kodwa kulokhu ukufana kwayo kwe-angular kunesimo sayo se-thermodynamic. Lokhu kufana kubonakala ngokuthi izinga lokushisa le-CMB licishe lifane noma kunini esibhakabhakeni, futhi ukuchezuka ekufaneni akudluli ku-10–5 (kulungiswe ngenxa yomphumela omncane we-Doppler ohambisana nokunyakaza kwethu ngendaba ezungezile). Ngaphezu kwalokho, kunokufana emhlabeni wonke ekusabalaliseni imithala nezinye izinto; isibonelo, ukusatshalaliswa kwamabhayoni (bheka Isigaba 1.3) esikalini esikhulu 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 inkulu uma sibheka phambili esikhathini esedlule se-Universe, futhi i-RI iwubufakazi obudala kakhulu bokusabalalisa kwendaba esingayibona ngokuqondile.

Lesi sithombe sihambisana nombono wokuthi, ezigabeni zokuqala zokukhula kwawo, i-Universe empeleni yayifana kakhulu, kodwa inokuminyana okungajwayelekile kancane. Ngokuhamba kwesikhathi (nangaphansi kwethonya lezinhlobo ezihlukahlukene "zokungqubuzana" -izinqubo ezihamba kancane ezihambisanayo), lokhu kungahambi kahle kokuminyana kwandiswa amandla adonsela phansi, okuhambisana nomqondo wokugoqa kancane kancane kwendaba. Ngokuhamba kwesikhathi, lokhu kunqwabelana kuyanda, okuphumela ekwakhekeni kwezinkanyezi; bahlangana babe imithala, ngamunye ovula imbobo enkulu emnyama phakathi nendawo. Ekugcineni, lokhu kugoqa kuqhutshwa isenzo esingenakunyakaziswa samandla adonsela phansi. Izinqubo ezinjalo empeleni zihlotshaniswa nokwanda okunamandla kwe-entropy futhi zibonisa ukuthi, ngokucabangela amandla adonsela phansi, i-primordial glowing sphere, okusele i-CMB kuphela namuhla, ibingaba kude ne-entropy ephezulu. Imvelo eshisayo yale sphere, njengoba kuboniswa i-spectrum ye-Planck ekhonjiswe ku-Fig. 3.13 imane isho lokhu: uma sicabangela i-Universe (ngesikhathi sokuhlakazeka kokugcina) njengesistimu ehlanganisa indaba namandla asebenzisana nomunye nomunye, khona-ke singacabanga ukuthi ngokuyinhloko bekuku-equilibrium ye-thermodynamic. Nokho, uma futhi sicabangela amathonya adonsela phansi, isithombe sishintsha kakhulu.

Incwadi ethi “Fashion, Faith, Fantasy and the New Physics of the Universe”
Uma sicabanga, isibonelo, igesi esitsheni esivaliwe, kungokwemvelo ukucabanga ukuthi izofinyelela i-entropy yayo ephezulu esimweni se-macroscopic lapho isakazwa ngokulinganayo kuwo wonke isitsha (Fig. 3.15 a). Kulokhu, izofana nebhola elishisayo elikhiqize i-CMB, esatshalaliswa ngokufanayo esibhakabhakeni. Nokho, uma sishintsha amangqamuzana egesi ngohlelo olukhulu lwemizimba ehlanganiswe amandla adonsela phansi, njengezinkanyezi ezingazodwana, sithola isithombe esihluke ngokuphelele (Fig. 3.15 b). Ngenxa yemiphumela yamandla adonsela phansi, izinkanyezi zizosatshalaliswa ngokungalingani, ngamaqoqo. Ekugcineni, i-entropy ephakeme kakhulu izofinyelelwa lapho izinkanyezi eziningi ziwa noma zihlangana zibe izimbobo ezimnyama. Nakuba le nqubo ingase ithathe isikhathi eside (yize izokwenziwa lula ukungqubuzana ngenxa yokuba khona kwegesi ephakathi kwezinkanyezi), sizobona ukuthi, ekugcineni, ngaphansi kokubusa kwamandla adonsela phansi, i-entropy iyanda ngokusatshalaliswa okuncane okufanayo kwento ohlelweni.

Le miphumela ibonakala ngisho nasezingeni lokuhlangenwe nakho kwansuku zonke. Omunye angase abuze: Iyiphi indima edlalwa uMthetho Wesibili ekusekeleni ukuphila eMhlabeni? Ngokuvamile kuthiwa siphila kulo mhlaba ngenxa yamandla esiwathola eLangeni. Kodwa lokhu akulona iqiniso ngokuphelele uma kucatshangelwa Umhlaba uwonke, njengoba cishe wonke amandla omhlaba owathola emini asheshe abaleke abuyele emkhathini, esibhakabhakeni esimnyama ebusuku. (Yebo, ibhalansi enembile izolungiswa kancane yizici ezinjengokufudumala kwembulunga kanye nokushisisa kweplanethi ngokubola kwemisebe.) Ngaphandle kwalokho, uMhlaba ubuyomane ushise kakhulu futhi ungahlali muntu phakathi nezinsuku! Kodwa-ke, ama-photon atholwe ngokuqondile eLangeni ane-frequency ephezulu uma kuqhathaniswa (agxile engxenyeni ephuzi ye-spectrum), kuyilapho uMhlaba ukhiphela ama-photon ama-low-frequency emkhathini, okuyingxenye ye-infrared spectrum. Ngokwezibalo zika-Planck (E = hν, bheka Isigaba 2.2), i-photon ngayinye efika ivela eLangeni iyodwa inamandla amakhulu kakhulu kunama-photon akhishelwa emkhathini, ngakho-ke ukuze kuzuzwe ibhalansi, ama-photon amaningi kufanele ahambe eMhlabeni kunokufika (bheka Umfanekiso 3.16). Uma ama-photon ambalwa efika, amandla angenayo azoba namadigri ambalwa enkululeko, kuyilapho amandla aphumayo azoba nokuningi, ngakho-ke, ngokusho kwe-equation kaBoltzmann (S = k log V), ama-photons angenayo azoba ne-entropy ephansi kakhulu kunalawo aphumayo. Sisebenzisa amandla ane-entropy aphansi agcinwe ezitshalweni ukuze sehlise i-entropy yethu: sidla izitshalo noma izilwane ezidla uhlaza. Yile ndlela impilo eMhlabeni igcinwa futhi ichuma ngayo. (Le mibono ngokusobala yaqalwa ngokucacile ngu-Erwin Schrödinger ngo-1967, encwadini yakhe eyisiqalo ethi Life as We Know It [Schrödinger, 2012].)

Incwadi ethi “Fashion, Faith, Fantasy and the New Physics of the Universe”
Iqiniso elibaluleke kakhulu elihlobene nalokhu kulinganisa okuphansi kwe-entropy yileli: ILanga liyindawo eshisayo esibhakabhakeni esimnyama ngokuphelele. Kodwa lezi zimo zaba khona kanjani? Izinqubo eziningi eziyinkimbinkimbi, ezihlanganisa ukusabela kwe-thermonuclear nokunye, zadlala indima, kodwa okubaluleke kakhulu ukuthi iLanga likhona nhlobo. Futhi kwavela ngenxa yokuthi i-solar matter (njengento eyenza ezinye izinkanyezi) yavela ngokuhlangana kwamandla adonsela phansi, kwaqala ngokusatshalaliswa okufanayo kwegesi nezinto ezimnyama.

Lapha, kufanelekile ukusho into engaqondakali eyaziwa ngokuthi i-dark matter, ebonakala ihlanganisa u-85% wezinto ezibonakalayo (okungezona u-Λ) zokuqukethwe kwendawo yonke, kodwa itholakala kuphela ngokusebenzisana kwamandla adonsela phansi, futhi ukwakheka kwayo akwaziwa. Namuhla, simane sicabangele lolu daba lapho silinganisa isamba sengqikithi, edingekayo ukuze kubalwe amanani athile ezinombolo (bona Izigaba 3.6, 3.7, 3.9; ukuze uthole indima ebaluleke kakhulu yetiyori yendaba emnyama, bheka Isigaba 4.3). Ngaphandle kwenkinga yendaba emnyama, sibona ukuthi ibaluleke kangakanani imvelo ephansi yokusatshalaliswa kwento efanayo ezimpilweni zethu. Ukuba khona kwethu, njengoba sikuqonda, kuncike endaweni engaphansi kwe-entropy gravitational reserve ewuphawu lokuqala lokusatshalaliswa kwezinto ezifanayo.

Lapha sifika esicini esimangalisayo—empeleni, esimangalisayo—se-Big Bang. Impicabadala ayigcini nje ngokuthi yenzeka kanjani, kodwa futhi eqinisweni ukuthi kwakuwumcimbi ophansi kakhulu. Ngaphezu kwalokho, okuphawulekayo akusona lesi simo kakhulu njengoba iqiniso lokuthi i-entropy yayiphansi ngenhlonipho eyodwa kuphela: amazinga adonsela phansi enkululeko ayecindezelwe ngokuphelele ngasizathu simbe. Lokhu kuhluke kakhulu kumadigri enkululeko yendaba kanye nemisebe (ye-electromagnetic), njengoba kubonakala sengathi bajabule kakhulu esimweni esishisayo ne-entropy ephezulu. Ngokubona kwami, lena mhlawumbe imfihlakalo ye-cosmological ejulile, futhi ngasizathu simbe, ihlala ingabongwa!

Kuhle ukucatshangelwa ngokuningiliziwe ukuthi isimo se-Big Bang sasikhethekile kangakanani nokuthi iyiphi i-entropy engase iqhamuke ngesikhathi sokuqubuka kwamandla adonsela phansi. Ngakho, kufanele siqale siqonde entropy Amazing ukuthi umgodi omnyama empeleni unazo (bheka Fig. 3.15 b). Sizoxoxa ngalolu daba eSigabeni 3.6. Kodwa okwamanje, ake siphendukele kwenye inkinga ehlobene nalokhu okulandelayo, okungenzeka kakhulu: Umkhathi ungahle ungapheli ngokwendawo (njengasendabeni yamamodeli we-FLUE ane-K. 0, bheka Isigaba 3.1), noma okungenani ingxenye enkulu Yomhlaba Wonke ingase ingafinyeleleki ekubonweni okuqondile. Ngakho-ke, sibhekana nenkinga ye-cosmological horizons, esizoxoxa ngayo esigabeni esilandelayo.