第十一届全国核结构会议课件.ppt

1、第十三届核结构研讨会暨第九次第十三届核结构研讨会暨第九次“核结构与量子力学核结构与量子力学”专题讨论会专题讨论会内蒙古内蒙古赤峰赤峰2010年年7月月夸克核心的混合星及致密星第三家族夸克核心的混合星及致密星第三家族特木尔巴根（南阳师范学院）特木尔巴根（南阳师范学院）I IntruductionII TheoryIII Third Family of Compact StarsIntroduction1.History of Neutron Stars Study2.Models for Neutron Star3.Present situations for Neutron Star Inve

2、stication4.MotivationIntro.-History In 1932,Chadwick discoved neutron,and Landau predicted neutron stars immediately.In 1934,Baade andand Zwicky In 1939,Tolman-Oppenheimer-Volkoff(TOV)equations.In 1967,Hewish and Bell detected the first pulsar,and known as rotating neutron star.Intro.Models for NS I

3、ntro.-TOV EquationsrrdrrrMrMrrrprrMrrpdrdp023)(4)()(2()(4)()()(Oppenheimer-Volkoff(OV)Oppenheimer-Volkoff(OV)方程：方程：r r距星体中心的距离；距星体中心的距离；p(r)p(r)距中心为距中心为r r处的压强；处的压强；(r)(r)能量密度；能量密度；M(r)M(r)半径为半径为r r的球体内的物质的质量的球体内的物质的质量。由物态方程由物态方程p=p(),给定星的中心密度，给定星的中心密度，由由OV方程就方程就可进行数可进行数 值求解。值求解。0)(RpgravityMRM)(Int

4、ro.Present Situations for NS Study1.Neutron star with hyperons(or with kaon condensation):n,p,e,k-(-)2.Strange(quark)stars:u,d,s，e3.Hybrid stars with quark core:n,p,e,u,d,s4.Third family of compact starsII Theories1 Hadronic Phase:RMFT2 Quark Phase:MIT Bag Model，NJL Model,M-D-D quark model,QMFM,EMQM

5、,D-D-B in the framework of MIT bag Model 3 Mixed Phase:Gibbs criterion for phase equilibrium and global electric charge neutrality.Quark models 1 Effective mass bag model(EMBM)K.SchertlerNuclear,C.Greiner Physics A616(1997)2 NambuJona-Lasinio（NJL）Model Y.Nambu and G.Jona-Lasinio Phys.rev.122,124(196

6、1)3 Mass-density-dependent Quark model(MDDQM)G.X.Peng Phys.Rev.C 62(025801)4 Density-dependent bag constant in the framewok of MIT bag modelIII Hybrid sars with quark core and third family of compact stars Hadron phase：TM2 parameter sets in the framework of RMFT TM1,TM2:Y.Sugahara,H.Toki,Relativisti

7、c mean-field theory or unstable nuclei with non-linear sigma and omega terms,Nucl.Phys.A579(1994)557-572 Thermodynamical Potencial ln352481212122422222iiiiiiiiiiiimmmmmgFomulae for quark modelsZbiinDmm0Mass-density-denpendent quark modelEffective mass quark model2222642*)(fffgmmffmNJL modelkkjjiiiiq

8、qqqKqqGmm24022223pmmdppqqiipiiiFQuark condensationEnergy density and pressure(EOS)iiiiiiBpB EOS-If Bag Parameter is Density Dependent()iiiiiiBBpB Formulas for mixed phase),(),(enQPenHPppdun2Gibbs criterion for phase equilibriumChemical potencials satisfyConservation of baryon number density,global e

9、lectric charge neutrality and total energy density for mixed phase0)1(QPHPMPqqqQPHPMP)1(qHqVVVVV,/QPHPMPqqq)1(where Calculational results 1.GL85,TM2-D-D-B in the framework of bag model Submitted to EPJ A,Chinese Physics C Vol.33 2.GL85-NJL Model HP&NP,2006,30(10)3.GL85-MDDQM HP&NP,2006,30(12)4.GL85,

10、TM2-EMBM Commun.Theor.Phys.45(2006)5.GL85SEBM Eur.Phys.J.A Vol.38,287-293(2008)Density-dependent bag parameterEnergy Density/Baryon Versus Total Baryon Number Density SQM EOS Hybrid star EOSMass-radius relation of SSMass-radius relation of hybrid stars-Third family of compact starsPossible Existence

11、 of TFTM2+EMBMg=01.0 TFPossible Existence of TFTM2+EMBM,g=0,B1/4=175-180MeVConclusions结论结论(续续)以以TM2为核物质状态方程的混合星质量为核物质状态方程的混合星质量-半半径曲线中，口袋常数径曲线中，口袋常数B1/4在在175MeV-178MeV（g=0）之间或耦合常数在）之间或耦合常数在g=0-1(口袋常数口袋常数 B1/4=180MeV时时)很小范围内存在很小范围内存在TF。这些。这些计算结果为观测具有相同质量而不同结构和计算结果为观测具有相同质量而不同结构和半径的双星提供了理论依据。半径的双星提供了理论依据。TF的存在亦的存在亦是混合星内存在夸克相变的有力证据。是混合星内存在夸克相变的有力证据。在有效质量口袋模型中在有效质量口袋模型中,强耦合常数和口袋强耦合常数和口袋常数所起的作用在一定范围内相同常数所起的作用在一定范围内相同.Thank your Attentions！