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EoS of quark matter and structure of compact stars
G. X. PengUniversity of Chinese Academy of Sciences
Institute of High Energy Physics (UCAS/IHEP)
Quarks and compact stars , 2014.10.20-22
Sunset view of UCAS
Nearby-APEC2014
[email protected], [email protected]
1 、 Introduction2 、 EoS of quark matter
3 、 M-R of compact stars4 、 Summary
EoS of 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
[email protected], [email protected]
Quarks and compact stars
Quarks and compact stars , 2014.10.20-22
[email protected], [email protected]
Modern physics and QCD
Quarks and compact stars , 2014.10.20-22
Asymptotic FreedomQuark ConfinementChiral symmetry
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Effective masses in physics
RMF:
NJL:
NMB:
Walecka 1995
NPA513:667
QMD:IJMPE06:515
……
Quarks and compact stars , 2014.10.20-22
[email protected], [email protected]
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
[email protected], [email protected]
Scaling with both confinement & perturbative interaction
Ref: 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
[email protected], [email protected]
Confinement by the density dependence
Quarks and compact stars , 2014.10.20-22
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Thermodynamics with equivalent 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 , 2014.10.20-22
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Necessary condition for thermodynamic consistency
Quarks and compact stars , 2014.10.20-22
[email protected], [email protected]
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
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 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 RG 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 poem to the conference
There are compact body in the remote sky.They are fascinlating and so high …Oh, one doesn’t know what they really are,but we can measure the M and R to explore a neutron or quark star.That’s why we are happily here, discussing models and observational data
G.X.Peng, 21 Oct. 2014
Congradulations on Quarks & Conpact Stars