第十三屆核結(jié)構(gòu)研討會暨第九次“核結(jié)構(gòu)與量子力學(xué)”專題討論會內(nèi)蒙古·赤峰2010年7月夸克核心的混合星及致密星第三家族特木爾巴根（南陽師范學(xué)院）第十三屆核結(jié)構(gòu)研討會暨第九次“核結(jié)構(gòu)與量子力學(xué)”專題討論會內(nèi)1IIntruductionIITheoryIIIThirdFamilyofCompactStarsIIntruduction2Introduction1.HistoryofNeutronStarsStudy2.ModelsforNeutronStar3.PresentsituationsforNeutronStarInvestication4.MotivationIntroduction1.HistoryofNeut3Intro.

--HistoryIn1932,Chadwickdiscovedneutron,andLandaupredictedneutronstarsimmediately

.In1934,Baade

and

ZwickyIn1939,Tolman-Oppenheimer-Volkoff(TOV)equations.In1967,HewishandBelldetectedthefirstpulsar,andknownasrotatingneutronstar.Intro.--HistoryIn1932,4Intro.—ModelsforNSIntro.—ModelsforNS5Intro.--TOVEquations

Oppenheimer-Volkoff(OV)方程：r→距星體中心的距離；p(r)→距中心為r處的壓強；(r)→能量密度；M(r)→半徑為r的球體內(nèi)的物質(zhì)的質(zhì)量。

由物態(tài)方程p=p(),給定星的中心密度，由OV方程就可進行數(shù)值求解。Intro.--TOVEquationsOppenhe6Intro.–PresentSituationsforNSStudy1.Neutronstarwithhyperons(orwithkaoncondensation):

n,p,e,,

,,,,k-(-)2.Strange(quark)stars:

u,d,s，e3.Hybridstarswithquarkcore:

n,p,e,,

,,,,

u,d,s4.ThirdfamilyofcompactstarsIntro.–PresentSituationsfor7IITheories1HadronicPhase:RMFT2QuarkPhase:MITBagModel，NJLModel,M-D-Dquarkmodel,QMFM,EMQM,D-D-BintheframeworkofMITbagModel

3MixedPhase:Gibbscriterionforphaseequilibriumandglobalelectricchargeneutrality.IITheories1HadronicPhase:8Quarkmodels

1Effectivemassbagmodel(EMBM)K.SchertlerNuclear,C.GreinerPhysicsA616(1997)

2Nambu—Jona-Lasinio（NJL）ModelY.NambuandG.Jona-LasinioPhys.rev.122,124(1961)3Mass-density-dependentQuarkmodel(MDDQM)—

G.X.PengPhys.Rev.C62(025801)

4

Density-dependentbagconstantintheframewokofMITbagmodelQuarkmodels1Effectivemass9IIIHybridsarswithquarkcoreandthirdfamilyofcompactstars

Hadronphase：TM2parametersetsintheframeworkofRMFTTM1,TM2:Y.Sugahara,H.Toki,Relativisticmean-fieldtheoryorunstablenucleiwithnon-linearsigmaandomegaterms,Nucl.Phys.A579(1994)557-572

IIIHybridsarswithquarkco10ThermodynamicalPotencial

ThermodynamicalPotencial11FomulaeforquarkmodelsMass-density-denpendentquarkmodelEffectivemassquarkmodelNJLmodelQuarkcondensationFomulaeforquarkmodelsMass-d12Energydensityandpressure(EOS)Energydensityandpressure(E13EOS-IfBagParameterisDensityDependentEOS-IfBagParameterisDensit14FormulasformixedphaseGibbscriterionforphaseequilibriumChemicalpotencialssatisfyFormulasformixedphaseGibbs15Conservationofbaryonnumberdensity,globalelectricchargeneutralityandtotalenergydensityformixedphasewhereConservationofbaryonnumber16

Calculationalresults

1.GL85,TM2-D-D-BintheframeworkofbagmodelSubmittedtoEPJA,

ChinesePhysicsCVol.332.GL85-NJLModelHP&NP,2006,30(10)3.GL85-MDDQMHP&NP,2006,30(12)4.GL85,TM2-EMBMCommun.Theor.Phys.45(2006)5.GL85—SEBMEur.Phys.J.AVol.38,287-293(2008)Calculationalresults1.GL8517Density-dependentbagparameterDensity-dependentbagparamete18EnergyDensity/BaryonVersusTotalBaryonNumberDensity

EnergyDensity/BaryonVersus19SQMEOS

SQMEOS20HybridstarEOSHybridstarEOS21Mass-radiusrelationofSSMass-radiusrelationofSS22Mass-radiusrelationofhybridstars-ThirdfamilyofcompactstarsMass-radiusrelationofhybrid23PossibleExistenceofTFTM2+EMBMg=0—1.0TFPossibleExistenceofTFTM2+E24PossibleExistenceofTFTM2+EMBM,g=0,B1/4=175-180MeVPossibleExistenceofTFTM2+E25ConclusionsConclusions26結(jié)論(續(xù))

以TM2為核物質(zhì)狀態(tài)方程的混合星質(zhì)量-半徑曲線中，口袋常數(shù)B1/4在175MeV-178MeV（g=0）之間或耦合常數(shù)在g=0-1(口袋常數(shù)B1/4=180MeV時)很小范圍內(nèi)存在TF。這些計算結(jié)果為觀測具有相同質(zhì)量而不同結(jié)構(gòu)和半徑的雙星提供了理論依據(jù)。TF的存在亦是混合星內(nèi)存在夸克相變的有力證據(jù)。

在有效質(zhì)量口袋模型中,強耦合常