简介：

简介：IntheBigBangtheory,primordialnucleosynthesiswasfinishedduringfirsthalfhouroftheuniverse’sexistence.Thisprocessyieldedthemainlightelementsincludinghydrogen,deuterium,heliumandlithium.Thetheoreticalpredictionsmatchverywelltheobserveddeuteriumandheliumabundance,butthe7Liabundanceisoverpredictedbyafactorathree[1].Thisinconsistencyiscalled“cosmologicallithiumproblem”.Inthepastdecade,manyattemptstosolvethisproblemusingconventionalastrophysicsandnuclearphysicsfailed.Recently,weproposedanewsolutiontolithiumproblembyintroducingnon-extensivestatisticsintoBigBangnucleosynthesis[2].

简介：TheCADSdemofacilityisaimedtobuildaprototypelinacforthelowenergypartofthecontinuouswave(CW)superconductingprotonlinacanddemonstratetechnologyinthissection[1].IntheCADSroadmap,therealizationof25MeV10mAbeamisakeypoint.Thus,basedonthe10MeVCADSInjectorIIatIMP,IMPandIHEPwillbothcontributeacryomoduletoreach25MeVatthesiteofIMP[2].Todumpthebeamfromthelinac,webuildanewhighenergybeamtransportlinewithbendingangleof90°,toavoidback-scatteringgammaandneutronbeamstodamagethelinac.Fig.1showsthelayoutofthe25MeVdemofacility.

简介：ThepresolarSiCgrains[1]carrytheoriginalstellarnucleosynthesissignature.Theirisotopicanomaliescomparedtothesunarethestrongconstrainsinthesupernovae(SN)modelcalculations.The15N-excessinsomeSiC-ABgrains(12C/13C<10and14N/15N<272)isoneofthechallengesofcore-collapsesupernovae(CCSNe)models[2].Recently,PignataripointedoutthattheentrainmentofH-richmaterialintotheHeshellbeforetheSNexplosionallowsthecoproductionof13C,15Nand26Al,whichprovidesanewproductionscenarioforSiC-ABgrains[2].IntheHeshellnucleosynthesis,the13Cisproducedthrough12C(p,γ)13N(β+γ)13Creaction.The14Nissynthesizedthrough13N(n,γ)and13C(p,γ)reactions.

简介：The12C+13Csystemhasbeenstudiedextensively,becauseofthesimilarityoftheentrancechanneltotheastrophysicallyimportant12C+12Creaction[1??3].Untilnow,threedifferentmethodshavebeenexploitedtoperformthefusioncrosssectionmeasurementsfor12C+13CundertheCoulombbarrier:(1)measuringtheyieldofcharacteristicrays,(2)thetotal-rayyieldsusingNaIsummingdetectorsand(3)theactivityofthereactionresidue24Na(T1=2=15.0h).Recently,thefusioncrosssectionof12C+13Chasbeenmeasureddownto0.9nbthroughtheactivitymeasurementbyourgroup[4].Althoughthestatisticalmodelcalculationsinallthesethreemethodshavebeenroutinelyusedtoconverttheobservedpartialcrosssectionsintothetotalfusioncrosssections[5],thesystematicuncertaintyinducedbythestatisticalcorrectionshasnotbeenstudiedverywell.