1、EoS of quark matter and structure of compact stars,G. X. PengUniversity of Chinese Academy of SciencesInstitute of High Energy Physics (UCAS/IHEP),Quarks and compact stars，2014.10.20-22,Sunset view of UCAS,Nearby-APEC2014,, ,1、Introduction2、EoS of quark matter 3、M-R of compact stars4、Summary,EoS of
2、quark matter and structure of compact stars,G.X. Peng UCAS/IHEP,Ref.: 1 Xia & Peng et al. Phys. Rev. D 89 (2014) 105027.2 J.F.Xu, Peng et al. Sci. Chin. Phys. Mech. Astron. 2014.3 G.X. Peng et al. Phys. Rev. C 77 (2008) 065807.,Quarks and compact stars，2014.10.20-22,, ,Quarks and compact stars,Quark
3、s and compact stars，2014.10.20-22,, ,Modern physics and QCD,Quarks and compact stars，2014.10.20-22,Asymptotic FreedomQuark ConfinementChiral symmetry,, ,Effective masses in physics,RMF:,NJL:,NMB:,Walecka 1995,NPA513:667,QMD:,IJMPE06:515,Quarks and compact stars，2014.10.20-22,, ,Free-particle system,
4、Quarks and compact stars，2014.10.20-22,, ,The equivalent mass m(n) - density dependent,Z. Phys. C 9:271,PLB229:112,EPL56 (2001) 361; PRC67:015202,PRC61:015201 62: 025801,PRC72: 015204,Quarks and compact stuars，2014.10.20-22,ApJ 780: 135,, ,Scaling with both confinement & perturbative interaction,Ref
5、: Xia, Peng, et al, PRD89 (Oct. 2014) 100527,Quarks and compact stuars，2014.10.20-22,“The structure of compact stars with a new quark mass scaling” -Xia C J, 22 Oct. 2014 quarks and compact stars,, ,Confinement by the density dependence,Quarks and compact stars，2014.10.20-22,, ,Thermodynamics with e
6、quivalent masses,ZPC9(1981)271; PLB229(1989)112,PRD51(1995)1989; 52:1276,PRC62(2000)025801; 72(2005)01520477(2008)065807; PRD89(2014)105027,PRC62(2000)15204,PRC77(2008) 055204,3,5,1,4,2,Quarks and compact stars，2014.10.20-22,Inconsistency in the previous,PRD 51(95)1989,Quarks and compact stars，2014.
7、10.20-22,, ,Necessary condition for thermodynamic consistency,Quarks and compact stars，2014.10.20-22,, ,Necessary condition for thermodynamic consistency,Path-independency,Pressure ballence,Specially，the pressure must be zero at the (free-)energy minimum,Quarks and compact stars，2014.10.20-22,, ,Num
8、erical check,Quarks and compact stuars，2014.10.20-22,, ,Numerical check,Quarks and compact stuars，2014.10.20-22,M-R relation in the equiv-particle model,Quarks and compact stuars，2014.10.20-22,宇宙的不同层次,Perturbatiion model with running coupling, mass, and confnement,Thermodynamic potential at leading
9、orderin the modified minimum-subtraction scheme,Running coupling and running quark mass,Perturbation thermo. potential and density,Thermo. exptrapolation by an additional term,Determine the additional term by thermodynamic consistency,At the first-order level,At the first-order level,Determine the R
10、G scale,For 2-flavors:,Range of the parameters,M-R of compact stars,Summary,We study the M-R relation of compactstars considering both perturbation confinement interactions. For parameters With which SQM is absolutely stable, the maximum mass of quark stars can be about two time the solar mass.,A po
11、em to the conference,There are compact body in the remote sky.They are fascinlating and so high Oh, one doesnt know what they really are,but we can measure the M and R to explore a neutron or quark star.Thats why we are happily here, discussing models and observational data G.X.Peng, 21 Oct. 2014,Congradulations on Quarks & Conpact Stars,
