Ara\u015fd\u0131rma g\u00f6st\u0259rir ki,\u00a0helium hidridi\u00a0il\u0259\u00a0neytral hidrogen\u00a0v\u0259\u00a0deyterium\u00a0aras\u0131ndak\u0131 reaksiyalar erk\u0259n kainat kimyas\u0131nda \u0259vv\u0259l d\u00fc\u015f\u00fcn\u00fcld\u00fcy\u00fcnd\u0259n daha m\u00fch\u00fcm rol oynay\u0131b. Aliml\u0259r kainat\u0131n \u0259n ilkin anlar\u0131nda ba\u015f vermi\u015f \u0259sas kimy\u0259vi reaksiyalar\u0131 yenid\u0259n yaratma\u011fa m\u00fcv\u0259ff\u0259q olublar. Onlar ilk ulduzlar\u0131n nec\u0259 yarand\u0131qlar\u0131n\u0131 anlama\u011fa k\u00f6m\u0259k ed\u0259c\u0259k t\u0259\u0259cc\u00fcbl\u00fc n\u0259tic\u0259l\u0259r \u0259ld\u0259 edibl\u0259r. 13.8 milyard il \u0259vv\u0259l ba\u015f vermi\u015f\u00a0B\u00f6y\u00fck partlay\u0131\u015fdan\u00a0d\u0259rhal sonra kainat \u00e7ox s\u0131x v\u0259 isti bir yer idi. C\u0259mi bir ne\u00e7\u0259 saniy\u0259 \u0259rzind\u0259 kainat bir q\u0259d\u0259r soyudu v\u0259 bu, subatom hiss\u0259cikl\u0259rinin birl\u0259\u015f\u0259r\u0259k ilk kimy\u0259vi elementl\u0259ri – hidrogen v\u0259 heliumu yaratmas\u0131na \u015f\u0259rait yaratd\u0131. H\u0259min vaxt elektronlar h\u0259l\u0259 atom n\u00fcv\u0259l\u0259ri il\u0259 birl\u0259\u015fm\u0259mi\u015fdi. Yaln\u0131z 380 000 il sonra kainat o q\u0259d\u0259r soyudu ki, neytral atomlar\u0131n meydana g\u0259lm\u0259si m\u00fcmk\u00fcn oldu.\u00a0Rekombinasiya\u00a0adlanan bu proses elektronlar\u0131n atom n\u00fcv\u0259l\u0259rin\u0259 birl\u0259\u015fm\u0259sin\u0259 imkan verdi v\u0259 bu da ilk kimy\u0259vi reaksiyalar \u00fc\u00e7\u00fcn \u0259sas yaratd\u0131.<\/p>\n
\u018fn ilk kimy\u0259vi reaksiyalardan biri helium hidridi ionunun (HeH+) yaranmas\u0131 olub v\u0259 bu, kainat tarixind\u0259ki ilk molekul hesab edilir. Bu molekul neytral helium atomunun m\u00fcsb\u0259t y\u00fckl\u00fc hidrogen n\u00fcv\u0259si il\u0259 birl\u0259\u015fm\u0259si n\u0259tic\u0259sind\u0259 yaran\u0131b. Molekulun yaranmas\u0131 sonradan molekulyar hidrogenin (H2) – kainatda \u0259n geni\u015f yay\u0131lm\u0131\u015f molekulun – \u0259m\u0259l\u0259 g\u0259lm\u0259sin\u0259 s\u0259b\u0259b olan kimy\u0259vi reaksiyalar\u0131 ba\u015flad\u0131b. Rekombinasiyadan sonra kainatda \u201ckosmik qaranl\u0131q \u00e7a\u011f\u201d adl\u0131 d\u00f6vr ba\u015flad\u0131. Bu zaman kainat \u015f\u0259ffaf oldu, \u00e7\u00fcnki s\u0259rb\u0259st elektronlar art\u0131q atomlarla birl\u0259\u015fmi\u015fdi, lakin h\u0259l\u0259 ulduzlar v\u0259 dig\u0259r i\u015f\u0131q m\u0259nb\u0259l\u0259ri yaranmam\u0131\u015fd\u0131. Yaln\u0131z bir ne\u00e7\u0259 100 milyon il sonra ilk ulduzlar kainat\u0131 i\u015f\u0131qland\u0131rma\u011fa ba\u015flad\u0131. Kainat\u0131n m\u00f6vcudlu\u011funun erk\u0259n m\u0259rh\u0259l\u0259sind\u0259 HeH+ v\u0259 H2 kimi sad\u0259 molekullar ilk ulduzlar\u0131n yaranmas\u0131nda h\u0259lledici rol oynay\u0131blar. G\u0259l\u0259c\u0259k ulduzun n\u00fcv\u0259sind\u0259 termon\u00fcv\u0259 sintezinin ba\u015flaya bilm\u0259si \u00fc\u00e7\u00fcn qaz buludunun cazib\u0259 q\u00fcvv\u0259sinin t\u0259siri il\u0259 kifay\u0259t q\u0259d\u0259r s\u0131x\u0131lmas\u0131na ehtiyac var.<\/p>\n
Bu is\u0259 istiliyin yay\u0131lmas\u0131 il\u0259 m\u00fcmk\u00fcn olur. \u0130stiliyin yay\u0131lmas\u0131 atom v\u0259 molekullar\u0131n toqqu\u015faraq h\u0259y\u0259canlanmas\u0131 v\u0259 ard\u0131nca enerjini foton \u015f\u0259klind\u0259 buraxmas\u0131 il\u0259 ba\u015f verir. Lakin temperatur t\u0259xmin\u0259n\u00a010 000 d\u0259r\u0259c\u0259 Selsid\u0259n\u00a0a\u015fa\u011f\u0131 d\u00fc\u015fd\u00fckd\u0259, bu proses hidrogen atomlar\u0131n\u0131n \u00fcst\u00fcnl\u00fck t\u0259\u015fkil etm\u0259si s\u0259b\u0259bil\u0259 qeyri-effektiv olur. Daha da soyuma yaln\u0131z d\u00f6nm\u0259 v\u0259 vibrasiya vasit\u0259sil\u0259 \u0259lav\u0259 enerji yayma\u011fa qadir molekullar\u0131n k\u00f6m\u0259yi il\u0259 ba\u015f ver\u0259 bil\u0259r. Dipol momentin\u0259 g\u00f6r\u0259 HeH+ ionu bu c\u00fcr a\u015fa\u011f\u0131 temperaturda x\u00fcsusil\u0259 effektiv say\u0131l\u0131r v\u0259 uzun m\u00fcdd\u0259t ilk ulduzlar\u0131n formala\u015fmas\u0131 zaman\u0131 soyuducu madd\u0259 kimi potensial \u0259h\u0259miyy\u0259tli namiz\u0259d hesab olunub. Bu is\u0259 o dem\u0259kdir ki, helium hidridi ionlar\u0131n\u0131n kainatdak\u0131 konsentrasiyas\u0131 ilk ulduzlar\u0131n yaranma s\u0259m\u0259r\u0259liliyin\u0259 \u0259h\u0259miyy\u0259tli d\u0259r\u0259c\u0259d\u0259 t\u0259sir ed\u0259 bil\u0259r.<\/p>\n
Bu d\u00f6vrd\u0259 helium hidridi ionunun (HeH+) s\u0259rb\u0259st hidrogen atomlar\u0131 il\u0259 toqqu\u015fmas\u0131 onun par\u00e7alanmas\u0131n\u0131n \u0259sas yolu idi. Bu proses n\u0259tic\u0259sind\u0259 neytral helium atomu v\u0259\u00a0H2+\u00a0ionu \u0259m\u0259l\u0259 g\u0259lirdi. Daha sonra H2+ dig\u0259r hidrogen atomu il\u0259 reaksiyaya gir\u0259r\u0259k neytral H2 molekulu v\u0259 proton yarad\u0131rd\u0131 ki, bu da molekulyar hidrogenin formala\u015fmas\u0131na g\u0259tirib \u00e7\u0131xar\u0131rd\u0131. \u0130ndi is\u0259 aliml\u0259r ilk d\u0259f\u0259 bu kimy\u0259vi reaksiyan\u0131 erk\u0259n kainat\u0131n \u015f\u0259raitin\u0259 yax\u0131n laboratoriya m\u00fchitind\u0259 u\u011furla t\u0259krarlay\u0131blar. Onlar HeH+ ionunun deyteriumla – atom n\u00fcv\u0259sind\u0259 protonla yana\u015f\u0131 \u0259lav\u0259 neytron da da\u015f\u0131yan hidrogen izotopu il\u0259 reaksiyas\u0131n\u0131 \u00f6yr\u0259nibl\u0259r.<\/p>\n
Bu reaksiya zaman\u0131 HeH+ il\u0259 deyterium qar\u015f\u0131l\u0131ql\u0131 t\u0259sir\u0259 gir\u0259r\u0259k neytral helium atomu il\u0259 yana\u015f\u0131 H2+ \u0259v\u0259zin\u0259\u00a0HD+\u00a0ionu yarad\u0131r. Aliml\u0259r toqqu\u015fma tezliyinin toqqu\u015fman\u0131n enerjisin\u0259 – y\u0259ni birba\u015fa temperaturla \u0259laq\u0259li olan amil\u0259 – nec\u0259 d\u0259yi\u015fdiyini ara\u015fd\u0131ra bilibl\u0259r. Onlar m\u00fc\u0259yy\u0259n edibl\u0259r ki, m\u00f6vcud f\u0259rziyy\u0259l\u0259rin \u0259ksin\u0259 olaraq, bu reaksiyan\u0131n s\u00fcr\u0259ti temperatur azald\u0131qca z\u0259ifl\u0259m\u0259k \u0259v\u0259zin\u0259, dem\u0259k olar ki, sabit qal\u0131r. T\u0259dqiqat\u0131n m\u00fc\u0259llifl\u0259ri bildirirl\u0259r ki, \u0259vv\u0259lki proqnozlara \u0259sas\u0259n a\u015fa\u011f\u0131 temperaturlarda kimy\u0259vi reaksiyan\u0131n ba\u015f verm\u0259 ehtimal\u0131n\u0131n \u0259h\u0259miyy\u0259tli d\u0259r\u0259c\u0259d\u0259 azalaca\u011f\u0131 g\u00f6zl\u0259nilirdi, lakin apar\u0131lan t\u0259cr\u00fcb\u0259l\u0259r bunu t\u0259sdiql\u0259m\u0259yib. Bel\u0259likl\u0259, HeH+ ionunun neytral hidrogen v\u0259 deyteriumla reaksiyalar\u0131 erk\u0259n kainat\u0131n kimyas\u0131 \u00fc\u00e7\u00fcn \u0259vv\u0259l d\u00fc\u015f\u00fcn\u00fcl\u0259nd\u0259n qat-qat daha \u0259h\u0259miyy\u0259tli olmu\u015fdur.<\/p>\n