induced magnetism in color-superconducting media
DESCRIPTION
INDUCED MAGNETISM IN COLOR-SUPERCONDUCTING MEDIA. Efrain J. Ferrer. The University of Texas at El Paso. EJF & de la Incera, PRL 97 (2006) 122301 EJF & de la Incera, PRD 76 (2007) 045011 EJF & de la Incera, PRD 76 (2007) 114012. OUTLINE. Magnetized CS. - PowerPoint PPT PresentationTRANSCRIPT
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INDUCED MAGNETISM IN COLOR-SUPERCONDUCTING MEDIA
Efrain J. FerrerThe University of Texas at El Paso
OUTLINE
• Magnetized CS
• Gluon Vortices and Magnetic Antiscreening in CS
• Chromomagnetic Instabilities & CondensatesG B
EJF & de la Incera, PRL 97 (2006) 122301 EJF & de la Incera, PRD 76 (2007) 045011 EJF & de la Incera, PRD 76 (2007) 114012
Compact stars in the QCD phase diagram II (CSQCD II)May 20-24, 2009, Peking University, Beijing, China
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Boson: Zero Spin and opposite momenta
Electric Charge
Broken Symmetry : U(1)em
2C
23 )*(
2*)TT(*
m̂2xd][F
ud
Electric Superconductivity Color Superconductivity
ee
Color Charge
Barrois ‘77; Frautschi ’78; Bailin and Love’84; Alford, Rajagopal and Wilczek ’98; Rapp, Schafer, Shuryak and Velkovsky ‘98
Broken Symmetry : SU(3)C, U(1)em
J. Bardeen, L. N. Cooper and J. R. Schrieffer
L. D. Landau V. L. Ginzburg
Cooper Pair Condensation
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d
s
ud
d
u
u
s
sA
8G
A
8cos sin A A G 8 8sin cos G A G
In-Medium Magnetic Field
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Diameter:
Mass:
Magnetic fields:
Temperature:
pulsar’s surface: B~ 1012–1014G magnetar’s surface: B~ 1015–1016G
Neutron Stars
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Chromomagnetic
Instability
Magnetic Phases at High Density
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B=0 CFL
SU(3)C × SU(3)L × SU(3)R × U(1)B × U(1)e.m
B 0 MCFL
SU(3)C×SU(2)L×SU(2)R ×U(1)B × U(-)(1)A× U(1)e.m.
C+L+R(2 ) (1)emSU U
(3) (1)C L R emSU U 9 GB
5 GB
Magnetic CFLMagnetic CFL
1 2 3
1 2 3 E.J. Ferrer, V.I. and C. Manuel, PRL ‘05; NPB’06
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1G 3G
2G
Because of the modified electromagnetism, gluons are charged in the color superconductor
G G
I I
0 0 0 1 -1 1 -1 0
8G
Gluon Mean-Field-Effective Action in the CFL Phase:
Magnetic Effects on the Gluon Sector EJF & de la Incera, PRL 97 (2006) 122301
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1G 3G
2G
where
G G
I I
0 0 0 1 -1 1 -1 0
8G
Effective action for the charged gluons within CFL at asymptotic densities
Charged Gluons Effective Action
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Assuming that there is an external magnetic field in the z-direction, one mode becomes unstable when
H2MH m
with corresponding eigenvector:
“Zero-mode problem” for non-Abelian gauge fields whose solution is the formation of a vortex condensate of charged spin-1 fields.
Nielsen & Olesen NPB 144 (1978)
Skalozub, Sov.JNP23 (1978);ibid 43 (1986)
Ambjorn & Olesen, NPB315 (1989)
1 2( , ) (1, )G G G i
Magnetic Instability for Charged Spin-1 Fields
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Gibbs Free-Energy:
Minimum Equations:
In the approximation:
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Minimum Equations:
=0
Magnetic Antiscreening
+
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H < Hc H ≥ Hc
H < Hc H ≥ Hc
Color Superconductor
Conventional Superconductor vs Color Superconductor
Conventional Superconductor
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B
HHc
ismParamagnet
Variation of internal magnetic field (B) with applied magnetic field (H) for Type I, Tipe II and Color Superconductors
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The linear minimum equation for G* around the critical field is
20 2 2
2 11(2
, )
M M
eH me m
where
The solution is given by
0
2k
kx
H
Solution of the Linear Condensate Equation
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The vortex lattice induces a magnetic field that forms a fluxoid along the z-direction. The magnetic flux through each periodicity cell in the vortex lattice is quantized
Vortex lattice, First image 1967
From the experience with conventional type II superconductivity, it is known that the inhomogeneous condensate solutions prefer periodic lattice domains to minimize the energy. Then, putting on periodicity in the y-direction:
,...,, ,/ 2102 nbnkby
The periodicity is also transferred to the x-direction:
Then, the general solution is given by the superposition:
Vortex Solution
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Neutrality Conditions
)(0
B
B
J
0
e
0
8
0
3
)8(08 )2/3( Gg
)3(03 )2/( Gg
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• The optimal Cooper pairing occurs when
• Matter inside a star should be electrically neutral to guarantee the star stability and to minimize the system energy
• There are no enough electrons in β equilibrium to balance the charge deficit
Cooper pairing is consequently distorted by the Fermi sphere mismatch.
Cooper Pairing and Neutrality Conditions
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Color Neutrality and beta equilibrium
Unstable Gapped 2SC
a=1,2,3 masslessa=4,5,6,7 negativea=8 positive
Gapless 2SC
a=1,2,3 masslessa=4,5,6,7 negativea=8 negative
Stable Gapped 2SC
a=1,2,3 masslessa=4,5,6,7 positivea=8 positive
Gluons Masses
1 2 2
Huang/Shovkovy, PRD 70 (2004) 051501
Chromomagnetic Instabilities in 2SC
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Some Suggestions
Crystalline Superconductivity Alford, Bowers & Rajagopal, PRD 63 (2001) 074016
Phases with Additional Bose Condensates Bedaque & Schäfer, NPA 697 (2002) 802
Homogeneous Gluon Condensate Gorbar, Hashimoto & Miransky, PLB 632 (2006) 305
Inhomogeneous Gluon Condensate with an Induced Magnetic Field
Ferrer& Incera, PRD 76 (2007) 114012
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EJF & de la Incera, PRD 76 (2007) 114012
Chromomagnetic Instabilities & G-B Condensates in 2SC
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Neutrality Conditions
)(0
B
B
J
0
e
0
8
0
3
)8(08 )2/3( Gg
)3(03 )2/( Gg
Stable Phase:
/~ , ,0 883 e
Huang/Shovkovy, PLB 564 (2003) 205
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Effective Action
- 8
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At Tachyonic Mode of Charged Gluons
µ8
Weakly First-Order Phase transition
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Free-Energy:
Minimum Equations:
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Linear Equations
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Gluon-Condensate Solution
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Condensate Free-Energy
2
2
~200q
mF
M
g
23
222~
200
)1( 2
2
gs
Mq
g
gm
mF
Inhomogeneous Condensate:
Homogeneous Condensate:
0.1ξ
EJF & de la Incera, hep-ph/0705.2403
Gorbar/Hashimoto/Miransky, PLB 632 (2006) 305
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Fukushima, PRD 72 (2005) 074002; Casalbouni et al, PLB 605 (2005) 362; Alford/Wang JPG 31 (2005) 719.
Meissner Masses & Chromomagnetic Instabilities in Gapless-Three Flavor Quark Matter
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Origin of Stellar Magnetic Fields
G10B 24EW
G10B 4
G10B 8
)Bv(
dt
Bd
.Yrs billion 12~
0Sd)B(4
1
dt
dS
S
22 TRB
.Yrs billion 1~
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Supernova remnants associated with magnetars should be an order of magnitude more energetic.
Recent calculations indicate that their energies are similar.
When a magnetar spins down, the rotational energy output should go into a magnetized wind of ultra-relativistic electrons and positrons that radiate via synchrotron emission.
So far nobody has detected the expected luminous pulsar wind nebulae around magnetars.
Difficulties of the Standard Magnetar Model
Possible Alternative:
B induced by the CS core.
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Conclusionsand Future Directions
Magnetism in Color Superconductivity is totally different from magnetism in Conventional Superconductivity
Magnetism is reinforced in Color Superconductivity
Magnetars CS Cores (?) Numerically solving the nonlinear equation, looking for the
realization of the vortex state
Exploring the possibility to induce a magnetic field in a three-flavor system: vortex state in gCFL
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Three flavors at very high density: CFL phase
C L R BSU( ) S
Symme
U( ) S3 3 3
try Breaking:
1U( ) U( )
C+L+R( )S 3U
Diquark condensate
O = O Dirac⊗ O flavor⊗ O color
in the CFL is:
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B=0
SU(3)C × SU(3)L × SU(3)R × U(1)B × U(1)e.m
B 0
SU(3)C×SU(2)L×SU(2)R ×U(1)B × U(-)(1)A× U(1)e.m.
C+L+R(2 ) (1)emSU U
(3) (1)C L R emSU U
9 GB
5 GB
3-Flavor QCD
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3-Flavor QCD
B = 0
SU(3)C × SU(3)L × SU(3)R × U(1)B × U(1)e.m
B ≠ 0
SU(3)C × SU(2)L × SU(2)R × U(1)B × U(-)(1)A ×
U(1)e.m.
Miransky & Shovkovy, PRD 66(2002)
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Meissner Screening Masses
& Chromomagnetic Instabilities
in Neutral Dense Two-Flavor Quark Matter
Huang/Shovkovy, PRD 70 (2004) 051501
At Tachyonic Mode of Charged Gluons
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plus
Attractive interaction
s
Cooper instability
at the Fermi surface
Baryonic Matter at Very High Density & CSBaryonic Matter at Very High Density & CS
Asymptotic freedom
Color Superconductivity
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Chromomagnetic
Instability
Haas-van Alphen Oscillations of the Gaps
Fukushima and Warringa, ArXiv: 0707.3785
Haas-van Alphen Oscillations of the Magnetization
Noronha and Shovkovy, ArXiv: 0708.0307
Magnetic Phases at High Density