\u00c7in aliml\u0259rind\u0259n ibar\u0259t qrup ilk d\u0259f\u0259 qalaktikam\u0131zda y\u00fcks\u0259k enerjili kosmik z\u0259rr\u0259cikl\u0259rin m\u0259nb\u0259yini k\u0259\u015ff ed\u0259r\u0259k astrofizika sah\u0259sind\u0259 yeni bir m\u0259rh\u0259l\u0259y\u0259 ke\u00e7id edibl\u0259r.<\/p>\n
Elm v\u0259 T\u0259hsil Nazirliyinin \u015eamax\u0131 Astrofizika R\u0259s\u0259dxanas\u0131ndan veril\u0259n m\u0259lumata g\u00f6r\u0259, m\u00fc\u015fahid\u0259l\u0259r \u00c7inin LHAASO (Large High-Altitude Air Shower Observatory) r\u0259s\u0259dxanas\u0131nda apar\u0131l\u0131b.<\/p>\n
T\u0259dqiqat qrupu t\u0259r\u0259find\u0259n ulduz \u0259m\u0259l\u0259g\u0259lm\u0259 b\u00f6lg\u0259si olan Qu X istiqam\u0259tind\u0259 \u0259n az\u0131 100 ultra-y\u00fcks\u0259k enerjili (bir ne\u00e7\u0259 PeV) qamma \u015f\u00fcas\u0131 m\u0259nb\u0259yinin a\u015fkar olunmas\u0131 bildirilib. M\u0259s\u0259l\u0259nin aktuall\u0131\u011f\u0131 ondan ibar\u0259tdir ki, kosmik s\u00fcr\u0259tl\u0259ndiricil\u0259rin mahiyy\u0259ti tam ayd\u0131n deyil v\u0259 bu m\u0259nb\u0259l\u0259rin k\u0259\u015ffi n\u0259z\u0259riyy\u0259nin i\u015fl\u0259nilm\u0259si \u00fc\u00e7\u00fcn a\u00e7ar rolunu oynay\u0131r. Super PeVatronlar\u0131n, y\u0259ni y\u00fcks\u0259k enerjili protonlar\u0131n m\u0259nb\u0259yinin k\u0259\u015ffi bu m\u0259s\u0259l\u0259nin h\u0259llind\u0259 m\u00fch\u00fcm add\u0131md\u0131r. Bu k\u0259\u015ff kosmik s\u00fcr\u0259tl\u0259ndiricil\u0259rin t\u0259bi\u0259tini v\u0259 qalaktikan\u0131n t\u0259kam\u00fcl\u00fcnd\u0259ki rolunu a\u00e7ma\u011fa k\u00f6m\u0259k ed\u0259 bil\u0259r.<\/p>\n
A\u015fkar olunan m\u0259nb\u0259d\u0259 qeyd olunan fotonlar\u0131n enerjisi 1 PeV-d\u0259n (1015 eV) \u00e7oxdur (maks: 2.5 PeV). Bu is\u0259 m\u0259nb\u0259nin daxilind\u0259 bu enerjini yarada bil\u0259c\u0259k s\u00fcr\u0259tl\u0259ndirici mexanizmin oldu\u011funu g\u00f6st\u0259rir. Aliml\u0259rin fikrinc\u0259\u00a0\u00a0protonlar\u0131n s\u00fcr\u0259tl\u0259nm\u0259sinin s\u0259b\u0259bi Qu OB2 regionundak\u0131 O v\u0259 B spektal sinifli massiv ulduzlar\u0131n \u00e7oxlu\u011fudur. Onlar\u0131n qamma dipazondak\u0131 \u015f\u00fcalanmalar\u0131n\u0131n intensivliyi v\u0259 ulduz k\u00fcl\u0259kl\u0259rinin yaratd\u0131\u011f\u0131 z\u0259rb\u0259 dal\u011falar\u0131 protonlar\u0131n bel\u0259 y\u00fcks\u0259k enerjil\u0259r\u0259d\u0259k s\u00fcr\u0259tl\u0259nm\u0259sin\u0259 s\u0259b\u0259b olur.<\/p>\n
Enerjisi 1 PeV-d\u0259n a\u015fa\u011f\u0131 olan kosmik \u015f\u00fcalar\u0131n m\u0259n\u015f\u0259yinin qalaktikan\u0131n daxili b\u00f6lg\u0259l\u0259rind\u0259n g\u0259ldiyi g\u00fcman olunur. Enerjisi 10 PeV-d\u0259n yuxar\u0131 olan \u015f\u00fcalar\u0131n is\u0259 m\u0259n\u015f\u0259yi h\u0259l\u0259 d\u0259 nam\u0259lumdur. Bu suallara cavab tapmaq \u00fc\u00e7\u00fcn t\u0259dqiqat i\u015fl\u0259ri davam etdirilir, dig\u0259r ulduz\u0259m\u0259l\u0259g\u0259lm\u0259 b\u00f6lg\u0259l\u0259ri ara\u015fd\u0131r\u0131l\u0131r.<\/p>\n