EoS of quark matter and structure of compact stars

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

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Quarks and compact stars

Quarks and compact stars ， 2014.10.20-22

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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

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Free-particle system

Quarks and compact stars ， 2014.10.20-22

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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

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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

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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

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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

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Numerical check

Quarks and compact stuars ， 2014.10.20-22

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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 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