BABU ALAMAR WANI ƁOYAYYEN ƘARFI DA KE LANƘWASA TAURARIN GALAXY

Sabbin awon faɗaɗar Sararin Halitta (Universe) suna barin wuri ga duhun kuzari da ke canzawa da lokaci, maimakon wani tsayayyen cosmological constant. Wani bayani da aka gabatar shi ne cewa duhun kuzari yana hulɗa da duhun abu. Hakan zai karya wani ginshiƙi na kimiyyar lissafi, ƙa’idar daidaito (equivalence principle), wadda ke cewa komai yana faɗuwa ta hanya ɗaya, amma a ɓangaren duhu kawai.

Irin waɗannan samfura suna samar da ƙarfi na biyar da ke aiki a kan duhun abu kaɗai. Gwaje-gwajen ɗakin bincike na ƙa’idar daidaito suna kai wa ga kashi ɗaya cikin 10¹³ zuwa 10¹⁵, amma bisa tsarinsu ba za su iya ganin ƙarfin da ke watsi da abu na yau da kullum ba. Mafi kyawun iyakoki zuwa yanzu sun fito ne daga ilimin sararin samaniya, a kashi kaɗan cikin dubu na ƙarfin jan hankali, kuma wasu fassarori na sabbin bayanan ma suna fifita ƙarfi mai wannan girma.

Faifan da aka bari a baya

Harry Desmond (Jami’ar Portsmouth) da Pedro G. Ferreira (Jami’ar Oxford) suna neman sa a cikin galaxies. Galaxy mai karkace (spiral) faifai ne na taurari da iskar gas da ke zaune a cikin wani kwanson duhun abu (halo) mafi girma sosai. Idan ƙarfi na biyar yana jan kwanson zuwa gine-ginen da ke maƙwabtaka amma ba taurari ba, kwanson yana gaba kuma faifan yana jinkiri a baya, da ’yan dubun parsecs.

Faifan yana ci gaba da kasancewa a ɗaure da kwanson, amma jan dawowar kwanson yana raunana zuwa gefuna. Don haka taurarin waje dole su motsa nesa fiye da na ciki, kuma faifan yana lanƙwasa ya zama siffar U, kwano da ke buɗewa nesa da ƙarfin. Zurfin kwanon yana daidai da ƙarfin ƙarfin kai tsaye.

Zanen faifan taurari ja mai lanƙwasa a saman tsakiyar kwanso, da kibiya kore da ke nuna ƙarfi na biyar yana jan kwanson ƙasa.

Yadda ƙarfi a kan duhun abu kaɗai ke lanƙwasa faifai: ana jan kwanson nesa (kibiya kore), faifan yana zama a wajen tsakiya kuma yana lanƙwasa ya zama U. — Figure 1, Desmond & Ferreira (2026), arXiv:2610.24618, CC BY 4.0.

Dubban faifai da ake gani ta gefe

Lanƙwasar da aka hasashe ta yi ƙanƙanta sosai da ba za a iya ganin ta a kowane galaxy guda ba, kuma galaxies na gaske suna lanƙwasa saboda dalilai na yau da kullum da yawa. Don haka gwajin na ƙididdiga ne. Marubutan sun auna layin tsakiya na faifai 3,968 da ake gani ta gefe a cikin hotunan Sloan Digital Sky Survey, da wani ma’auni da ke amsa lanƙwasa masu siffar U kawai kuma yana watsi da lanƙwasa masu siffar S da suka zama ruwan dare a galaxies masu karkace.

Daga taswirar abu a cikin Sararin Halitta na kusa, har zuwa megaparsecs 290, sun lissafa ga kowane galaxy alkibla da ƙarfin ƙarfi na biyar da zai ji. Idan ƙarfin ya wanzu, lanƙwasar za ta jeru da waɗannan hasashe.

Ba su jeru ba. Lanƙwasar da aka auna ba ta nuna wata alamar dangantakar da aka hasashe ba, har ma tana ɗan karkata ta ɗaya hanyar kaɗan, wani tasiri da marubutan suka gano kusan gaba ɗaya ya fito daga galaxy ɗaya da wani tauraro na gaba ya rage a cikin hotonsa.

Iyaka mafi tsauri sau uku

Sakamakon iyaka ce ta sama: ƙarfi na biyar dole ya kasance ƙasa da 7.7 × 10⁻⁴ na ƙarfin jan hankali (yaƙinin 95%) ga zangon megaparsecs 8 zuwa sama. Bayan gwada sauye-sauye goma sha biyar na zatonsu, marubutan sun ba da iyaka mai taka-tsantsan ta 1.7 × 10⁻³.

Zanen yankin da aka hana na ƙarfin ƙarfi na biyar idan aka kwatanta da zango, da layukan iyaka ja da baƙi da ɗigogi daga wasu bincike a samansu.

Yankin da aka hana (toka) na ƙarfin wani ƙarfi na ɓangaren duhu idan aka kwatanta da zangonsa; a dama, yanayin zango marar iyaka, inda wasu ƙimomi da daidaitawar bayanan DESI suka fi so (shuɗi, shunayya) suke sama da sabuwar iyakar. — Figure 3, Desmond & Ferreira (2026), arXiv:2610.24618, CC BY 4.0.

Ga zango marar iyaka a zahiri, ko da iyaka mai taka-tsantsan ta fi mafi tsauraran iyakar ilimin sararin samaniya ƙarfi sau uku, kuma ta fi gwaje-gwajen falaki na baya ƙarfi sau 43 zuwa 360. Tana hana goyon baya, a kusan sigma 2 zuwa 3, ga ƙimomin haɗaka (couplings) da wasu daidaitawa na baya-bayan nan na duhun kuzari mai hulɗa da bayanan binciken DESI suka fi so.

Hanyoyin biyu suna cike juna. Iyakokin ilimin sararin samaniya sun dogara ga yadda filin (field) ya kasance a tsawon tarihin sararin samaniya; gwajin lanƙwasa yana auna ƙarfin da ke aiki a kan duhun abu a yau. A zango na tsakiya, nazarin ilimin sararin samaniya na mafi sauƙin samfuri har yanzu yana ba da iyaka mafi tsauri fiye da mai taka-tsantsan ta nan.

Hanyoyin tsira

Wata ka’ida har yanzu za ta iya ɓoye ƙarfin a cikin galaxies da wata dabarar “kariya” (screening). Marubutan sun nuna cewa nau’o’in kariya da aka saba ba za su iya yin hakan ba yayin da suke riƙe ƙarfin da muhimmanci ga ilimin sararin samaniya. Wasu zaɓuɓɓuka biyu masu ban mamaki, Vainshtein screening da abin da ake kira disformal coupling, har yanzu a buɗe suke kuma an bar su ga aiki na gaba. Har zuwa lokacin, suna ganin daidaitawar duhun kuzari mai hulɗa ya kamata su ɗauki 1.7 × 10⁻³ na ƙarfin jan hankali a matsayin rufin.