QUARK MATTER SYMMETRY ENERGY AND QUARK STARS

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QUARK MATTER SYMMETRY ENERGY AND QUARK STARS Peng-cheng Chu( 初初初 ) (INPAC and Department of Physics, Shanghai Jiao Tong University. [email protected]) Collaborators Lie-wen Chen (SJTU)

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QUARK MATTER SYMMETRY ENERGY AND QUARK STARS. Peng-cheng Chu ( 初鹏程 ) ( INPAC and Department of Physics, Shanghai Jiao Tong University. [email protected] ). Collaborators : Lie- wen Chen (SJTU). Outline. Symmetry energy introduction in quark matter. - PowerPoint PPT Presentation

Transcript of QUARK MATTER SYMMETRY ENERGY AND QUARK STARS

Page 1: QUARK MATTER SYMMETRY ENERGY AND QUARK STARS

QUARK MATTER SYMMETRY ENERGY AND QUARK STARS

Peng-cheng Chu(初鹏程 )(INPAC and Department of Physics, Shanghai Jiao Tong

University. [email protected])

Collaborators:Lie-wen Chen (SJTU)

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OutlineSymmetry energy introduction in quark matter.Isospin density-dependent-quark-model.EOS in the Isospin DDQM of Beta-equilibrium strange quark matterProperties of compact star based on the Isospin DDQM.Summary and outlook.

Main References:G.X.Peng,H.C.Chiang,J.J.Yang,L.Li. Phys.Rev.C 61 015201

F . Weber ,Progress in Particle and Nuclear Physics 54 (2005) 193-288G.X.Peng,A.Li,U.Lombardo Phys. Rev.C 77,065807 (2008)

Thomas D.Cohen, R.J.Furnstahl, and David K.Griegel Phys.Rev.C 45 X.J.Wen, X.H.Zhong, G.X.Peng, P.N.Shen, P.Z.Ning Phys.Rev.C 72 015204

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Motivation to learn

Strange quark matter may be the ground state~

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The loop diagram of my work

Maybe 2 solar mass of a compact star

The EoS of quarksThe phenomenological

models of quarks

Constraints of QCD chiral symmetry

Color confinement

The symmetry energy of quarks

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Symmetry energy of quark matter.

In quark matter:

The symmetry energy

In hadron matter:

[-3,3] [-1,1][-1,1]

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In symmetric quark matter , make

And

Then

Symmetry energy of quark matter.

So we deduce the non-interaction symmetry energy of quark matter

Define the symmetry energy as

We can get the non-interaction symmetry energy of quark matter

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Symmetry energy of quark matter.

So we choose the second and discuss the symmetry energy in 3 different models

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Density-dependent-quark-model.

Since bag model incorporate the bag constant ,many ways of effective term can be introduced to meet the principle.

Write the Hamiltonian density as:

Use the effective mass to make the form like a non-interacting system:

mq is the effective mass G.X.Peng,H.C.Chiang,J.J.Yang,L.Li. Phys.Rev.C 61 015201

The two hamiltonian density must have the same eigenenergy

then

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Isospin density-dependent-quark-model.

If we considered as an invariant interacting term for q=u,d or s

Notice that:

Hellmann-Feynman theorem

Give a renormalization-group invariant about quark condensate.

Thomas D.Cohen, R.J.Furnstahl, and David K.Griegel Phys.Rev.C 45

is used in sum-rules as –(225±25MeV)^3 for each flavor of quarks

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Isospin density-dependent-quark-model.

Isospin density-dependent-quark-model "+" for d quark, else for u quarkFor s quark , DI = 0.

With this treatment and doing volume

integral :

We check the range of DI

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Symmetry energy of quark matter.

G.X.Peng,H.C.Chiang,J.J.Yang,L.Li. Phys.Rev.C 61 015201,1999

In Density-dependent-quark-model.

Follow the postulate above ,the symmetry energy is:

The mass is effective mass

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Symmetry energy of quark matter.

The symmetric energy vs. baryon number density in CDDM(D^1/2=160Mev, ms=80Mev)

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Symmetry energy of quark matter.

The equivalent mass when we take the iso-spin dependence is:

Then the symmetry energy under this isospin DDQM is:

The mass is effective mass

"+" for d quark, else for u quark.

Where

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Symmetry energy of quark matter

When DI=0, CDDM and isospin DDQM has the same form

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Symmetry energy of quark matter

DI = 1.0 Isospin DDQM

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Symmetry energy of quark matter

The symmetry energy vs. baryon number density in Isospin DDQM

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Symmetry energy in NJL model

0 4 2i i i i j j k km m G q q K q q q q

We can get the symmetry energy in NJL model

Where i for u,d and s quarks.

22 2 2

3iF

ii k

i

mC k dk

k m

Λ=602.3MeV , G =1.835/602.3^2 , K = 12.36/602.3^5

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Symmetry energy in NJL model

2 2 2 2 2 202

, ,

3 2 ( ) 4iF

NJL i u d s u d ski u d s

k m k dk G C C C KC C C

rhoQs = rhoB

rhoQs = 0.

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Thermodynamic treatment to EOSNow we calculate the EoS of beta equilibrium quark matter

based on the isospin density dependent quark model.

According to the thermodynamic treatment

2 2

u

j j j jBu u u j j

j ju B j u j

d m v m vnu v m n f n fdn n n m n m

2 23

3 [ 1 ( 1 )]2

f x x x ln x xx

where

Define

Then the chemical potential is

2 24 1 12 2

3 3 3

1 (1 ) 2 2 9 ( ) ( )

 

jI I d u I d du u u j u d

j j u d u u d dB B B

vD D DD n v DD n vu v m n f n f n f

m n n m n n mn n n

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Thermodynamic treatment to EOS

Strange quark matter is considered as a mixture of u,d,s quarks and electrons.

chemical equilibrium:

Baryon density :

Charge-neutrality:

Solve this system of equation ,we can get the elements of the EOS

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Thermodynamic treatment to EOS

2 24 1 12 2

3 3

I I

3

1 (1 ) DD DD2 29 ( ) ( )

jI u u u dd d d j d

j j u d u u d d

vD D n v n vu v m n f nu f n fm n n m n n mnB nB nB

And for d,s quark:

2 24

3

1 (1 )9

jIs s s j

j j

vD Du v m n f

mnB

To solve the equations , we make nB given

Mev fm-3 DI=0 DI=0.3 DI=1.0Energy per baryon(min)

919.980 929.018 929.466

Pressure (zero) -.261608 0.923606E-02 -.330257E-01

Energy per baryon’s minimum value and zero pressure plot appear at the same time

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Thermodynamic treatment to EoSNow check DI’s effect in the EoS of quark matter

When DI increases , the minimum of the lines increase too.

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Thermodynamic treatment to EOSCompare the relationship between the Fermi momentum and chemical potential

DI=0.

DI=0.1DI=0.06.

DI=0.02.

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Thermodynamic treatment to EOSCompare the relationship between the quark fraction and rhoB

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The properties of Quark star

M/M

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The properties of Quark star

Set Ms0 as the parameter of the quark star while making DI=1.1 & D^1/2=147 MeV

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Rotating Quark star

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HADRON-QUARK PHASE TRANSITION

HADRONIC PHASE: RMF Theory

where the sum on B runs over the baryon octet :

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HADRON-QUARK PHASE TRANSITION

In the RMF model, the meson fields are treated as classical fields, and the field operators are replaced by their expectation values.

Effective mass

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HADRON-QUARK PHASE TRANSITION

The coupling constants set TM1 to calculate.

For neutron star matter consisting of a neutral mixture ofbaryons and leptons, the β equilibrium conditions without

trapped neutrinos are given by

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HADRON-QUARK PHASE TRANSITION

Then we get the chemical potential of baryons and leptons

The charge neutrality condition is given by

Where

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HADRON-QUARK PHASE TRANSITION

At a given baryon density

The total energy density and pressure ofneutron star matter are written by

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HADRON-QUARK PHASE TRANSITION

Also the pressure is given as :

Phase transition may occur in the core of massive neutron star.

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HADRON-QUARK PHASE TRANSITION

The two crucial equations:

The energy density and the baryon density in the mixed phase are given by

Solve the system of equations , we can get the phase transition diagram, which I haven’t done yet.

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HADRON-QUARK PHASE TRANSITION

Particle fraction vs Baryon number density

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HYBRID STAR

The mass-radius relation for the hybrid star & Quark star.

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OTHER QUARK MODELS

Bag constant for confinement

Quasi-particle bag model

D&T-DQM

Finite temperature may also cause problems.

NJL,PNJL,MIT,CFL,CDM …

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Isospin DDQM at Finite temperature:

EoS at Finite Temperature in Isospin DDQM

X.J.Wen, X.H.Zhong, G.X.Peng , P.N.Shen , and P.Z.Ning Phys.Rev.C 72 015204,2005

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Summary and outlook.

1. We extend the density-dependent-quark- mass(DDQM) model in which the confinement is modeled by the density-dependent quark masses to include the isospin dependence.

2. We make use of the model we provide to discuss the form of symmetry energy in quark matter. And we discuss the reason why people choose the symmetry parameter.

3. Based on the isospin dependent DDQM model ,we study the symmetry energy of quark matter and the EoS of strange quark matter. And we give the symmetry energy in

NJL model.

4. We give the quark star properties based on the Isospin DDQM and acquire a 2 solar mass quark star.

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Get the mass-radius relation for strange stars and study the structure of strange stars with surface effect considered.

We can use RMFT and Isospin DDQM to study the hadron-quark phase transition .

I will study on the stuff about quark matter based on QCD right away.

OUT LOOK

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INPAC

Thank you!