Symmetry energy with non-nucleonic degrees of freedom
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Transcript of Symmetry energy with non-nucleonic degrees of freedom
Aug. 19-22, 2013 @ TAMU
Symmetry energy with non-nucleonic degrees of freedom
Wei-Zhou JiangDepartment of Physics,
Southeast University, China
Collaborators: Bao-An Li, et al.
Aug. 19-22, 2013 @ TAMU
Introduction Hyperons, quarks, dark matter? Symmetry energy and quarks &
hyperons Interaction of quarks and its effects In neutron stars, effect of dark
matter? Summaries
Outline
Aug. 19-22, 2013 @ TAMU
— E=
Liquid-drop model for nuclei
SYMMETRY ENERGY
W. D. Myers, W.J. Swiatecki, P. Danielewicz,……
s2 4
ym ( )( , ) ( ), ( ),0) /( n pE OE E
In isospin asymmetric matter:
Aug. 19-22, 2013 @ TAMU
Where it is the matter, there is the symmetry energy.
Aug. 19-22, 2013 @ TAMU
L.W.Chen,et.al., PRC72, 064309 (05)Fuchs, et.al., arXiv:nucl-th/0511070
Aug. 19-22, 2013 @ TAMU
Diverse trends from data
1. Xiao, Li, et.al PRL102, 062502 (2009) 2. Feng&Jin, PLB683 (2010) 140
3. P. Russotto,W. Trauntmann, Q.F. Li et al., PLB697, 471(2011)
31.6(ρ/ρ)γ,with γ=0.9+/-0.4 : almost linear
Aug. 19-22, 2013 @ TAMU
Factor to soften greatly the Symmetry Energy:• Tensor force
C. Xu and B. A. Li, PRC81, 064612:
I. Vidana, A. Polls, and C. Providencia, PRC 84, 062801(R)
.
The dense the matter, the uncertain the symmetry energy
Aug. 19-22, 2013 @ TAMU
Significant points:
• To go ahead to deal with Tensor force with pion & rho: the most important ingredients of the chiral perturbative theory in Density dependent RHF approach: the simple, self-consistent and covariant framework.
• Here, we just go beyond this point to discuss contributions of non-nucleonic components to the symmetry energy.
Aug. 19-22, 2013 @ TAMU
Non-nucleonic degrees of freedom
• Threshold for hyperons reaches at high densities; 2ρ0-4ρ0
• Hadron-Quark transition may occur for nucleon overlaps >2ρ0
• In astrophysical extraction of the symmetry energy, there may be the effect of unknown dark matter.
• What is the effect of these components in dense matter? Matter changes, so does the interaction, so does the symmetry energy?
Aug. 19-22, 2013 @ TAMU
Model Lagrangian (RMF) :
with
Hyperons:
Aug. 19-22, 2013 @ TAMU
).-)/(-(
,)()(// 20
pn
symEeAE
N
F
FNsym E
kCE *
222
0
2
2
6
1
2
1)/(
)1)((4
1)(
pnsymE
EoS with inclusion of hyperons
Definition of symmetry energy:
at given hyperon fraction.
for charge neutral and chemical equilibrated matter
Aug. 19-22, 2013 @ TAMU
RMF models: SLC and SCLd
Jiang, Li, and Chen, PLB653, 184 ( 07);PRC76, 054314 (07); ApJ756, 56( 12)
Demorest, et al., Nature 467, 1081(2010): PSR J1614-2230
RMF model NL3: Lalazissis, et. al. PRC 55, 540(97).
Aug. 19-22, 2013 @ TAMU
symE
Aug. 19-22, 2013 @ TAMU
Symmetry energy with quarks
QH
QH
YY
YY
)1(
)1(
).)/(-(
,),(),(),(),(// 220
pnpnH
QQsymH
Hsym YEYEYeY
3/3/ ,3/23/ , ensdenuQH pp
Y is the quark phase proportion, determined by Gibbs conditions.We just consider the symmetric matterα=0
a function of α
0
2
2 )/(
2
1
symE
Step 1: no interaction between Qs & Ns
Aug. 19-22, 2013 @ TAMU
Critical density
Calculation detail: Charge chemical potential neglected here!
Aug. 19-22, 2013 @ TAMU
HsymE
Aug. 19-22, 2013 @ TAMU
Symmetry energy of quark flavor
Aug. 19-22, 2013 @ TAMU
With Λ hyperons
Jiang et al,PRC87, 064314(2013)
Aug. 19-22, 2013 @ TAMU
Questions:
• Clear model dependence of the transition density and the symmetry energy
• Why the transition density is so small as the strange quarks are included?
• Chemical potential and mechanical equilibriums should be corrected by interactions between quarks
Aug. 19-22, 2013 @ TAMU
Grand thermodynamical potential of quarks
,3
1)1(
34
1
?,)()()(
,
23/44
3/23/20
3/2
3/12
,,QQQQQ
sduiiQM
QM
aa
ppp
p
Qii
ii U
p
;
)/(2
Weissenborn, et al, arXiv:1102.2869Alford, et al, APJ629:969(2005)
Mechanical and chemicalequilibriums
Step 2: interactions for quarks
Aug. 19-22, 2013 @ TAMU
Preliminary results:
3-flavor
2-flavor
No QCD correction
QCD corr., a4=0.6
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No QCD corrections No correction to asymmetric part
Aug. 19-22, 2013 @ TAMU
23/4
3
1QQa
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• Symmetry energy: calculation is yet to make
• Step 3: interaction between Q’s & N’s
),(),(),(),(
),(
),(),(),(),(//
0000
220
YeYeYeYe
YE
YEYEYeY
MQH
QHM
QQsymH
Hsym
Aug. 19-22, 2013 @ TAMU
Dark matter in neutron stars
Only gravitational attraction between normal matter and dark matter
Aug. 19-22, 2013 @ TAMU
Symmetry energy extraction with Dark matter
Steiner:PRL 108, 081102 (2012)
Effect of Dark Matter?
Guillot et al. 2013, ApJ 772
Aug. 19-22, 2013 @ TAMU
DM with interactions
Aug. 19-22, 2013 @ TAMU
Summary
• Non-nucleonic degrees of freedom do affect the symmetry energy.
• Experimental extraction of symmetry energy at high densities should be of caution about the effects of new phases
• The astrophysical extraction of symmetry energy could undergo the influence of celestial dark matter that belongs to an unknown universe.
Aug. 19-22, 2013 @ TAMU
Thank you for your attention!Thank you for your attention!