low energy theory of the neutron star crust and its ... · star crust and its observable...
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Low Energy Theory of the Neutron Star Crust and its Observable
Implications. Sanjay Reddy
Los Alamos National Laboratory
Collaborators: Aguilera, Cirigliano, Chamel, Cumming, Page, Pethick, Pons &
Sharma
INT @ 20. The future of nuclear physics and its intersections. July 1-2, 2010Tuesday, July 6, 2010
nuclei
neutronsuperfluid
Neutron Star Crust:
Tuesday, July 6, 2010
New Phenomena in Neutron Stars
• Crustal heating and subsequent thermal relaxation in accreting neutron stars.
• Possible excitation of shear modes in the solid crusts of magnetars during giant flares.
- a window into the thermal and mechanical properties of the crust.
Tuesday, July 6, 2010
Simulations by Dany Page
Transient Accretion• Nuclear reactions heat the crust during accretion.
• Crust relaxes during quiescence. Haensel & Zdunik 1990, Brown, Bildsten, Rutledge (1998)
Shternin & Yakovlev (2007), Brown & Cumming (2009)
crust
Tuesday, July 6, 2010
Simulations by Dany Page
Transient Accretion• Nuclear reactions heat the crust during accretion.
• Crust relaxes during quiescence. Haensel & Zdunik 1990, Brown, Bildsten, Rutledge (1998)
Shternin & Yakovlev (2007), Brown & Cumming (2009)
Tuesday, July 6, 2010
Simulations by Dany Page
Transient Accretion• Nuclear reactions heat the crust during accretion.
• Crust relaxes during quiescence. Haensel & Zdunik 1990, Brown, Bildsten, Rutledge (1998)
Shternin & Yakovlev (2007), Brown & Cumming (2009)
Tuesday, July 6, 2010
More than one source !Cackett et al. 2006 Cackett et al. 2008
4.4 yr6.6 yrMXB 1659-29 KS 1731-260
!Cool = 305± 50 days!Cool = 465± 25 days
Tuesday, July 6, 2010
Connecting to Crust Microphysics
!Cool !CV
"(!R)2
Tuesday, July 6, 2010
Connecting to Crust Microphysics
!Cool !CV
"(!R)2
Crustal Specific Heat
Tuesday, July 6, 2010
Connecting to Crust Microphysics
!Cool !CV
"(!R)2
Crustal Specific Heat
Thermal Conductivity
Tuesday, July 6, 2010
Connecting to Crust Microphysics
!Cool !CV
"(!R)2
Crust ThicknessCrustal Specific Heat
Thermal Conductivity
Tuesday, July 6, 2010
Explosions on Magnetars: Giant Flares
SGRs exhibit powerful outburst ~ 1046 ergs/s
http://www.physics.mcgill.ca/~pulsar/magnetar/main.html
Anomalous X-Ray Pulsars (10)Soft Gamma Repeaters (8)
Inferred to have surface fields of the order of 1015 Gauss.
SGR 0525-66 : (1979)SGR 1806-20 (1979/1986/2004)* SGR 1900+14 (1979/1986/1998)SGR 1627-41 (1998)
SGR 1806-20: 2004 Flare
Hurley et al. (2005)
Tuesday, July 6, 2010
QPOs are likely to be shear modes in the solid crustDuncan (1998), Strohmayer, Watts (2006)
!n=0,l=2 ! 2 ctR
!n=1 ! " ctR
!R
R
Similar frequencies observed in 2 sources.
SGR 1806 2004 Giant Flare
Tuesday, July 6, 2010
Shear mode
velocity
QPOs are likely to be shear modes in the solid crustDuncan (1998), Strohmayer, Watts (2006)
!n=0,l=2 ! 2 ctR
!n=1 ! " ctR
!R
R
Similar frequencies observed in 2 sources.
SGR 1806 2004 Giant Flare
Tuesday, July 6, 2010
Microscopic Structure of the Crust
Negele & Vautherin (1973)
2 aneutrons
protons
Out
er C
rust
Inner Crustdripped
superfluid neutrons
Baym Pethick & Sutherland (1971)Tuesday, July 6, 2010
Microscopic Structure of the Crust
Negele & Vautherin (1973)
2 aneutrons
protons
Out
er C
rust
Inner Crustdripped
superfluid neutrons
Baym Pethick & Sutherland (1971)
Theory of electr
ons and phonon
s
Tuesday, July 6, 2010
Separation of Scales•Protons cluster (pairing + shell gaps) •Proton clusters form a Coulomb lattice. •Neutrons pair to form a superfluid.
!Debye !c
a! 0.45 !plasma
Ener
gy (
Tem
pera
ture
)
Longitudinal and Transverse Lattice
Phonons
!plasma =
!4"# Z2 nI
A mn
Nuclei (protons)
Superfluid Phonons
! ! EFn exp!
"1N(0) Vnn
"
Neutrons
Sing
le p
artic
le
exci
tatio
nsC
olle
ctiv
e ex
cita
tions
Tuesday, July 6, 2010
Superfluid Critical Temperature
Pairing gap is difficult to calculate in strong coupling.No small expansion parameter kF a > 1.
Cold atom experiments at kF a =∞ validate QMC. Polarization measurements in imbalanced systems are exponentially sensitive to the gap.
Tc ! 0.57 !
At kF a =∞: ! =!EF
= 0.45± 0.05
Gezerlis & Carlson (2009)
Carlson & Reddy (2010)
(?)
Tuesday, July 6, 2010
Superfluid Critical Temperature
Pairing gap is difficult to calculate in strong coupling.No small expansion parameter kF a > 1.
Cold atom experiments at kF a =∞ validate QMC. Polarization measurements in imbalanced systems are exponentially sensitive to the gap.
Tc ! 0.57 !
At kF a =∞: ! =!EF
= 0.45± 0.05
Gezerlis & Carlson (2009)
Carlson & Reddy (2010)
(?)
Tuesday, July 6, 2010
Relevant Temperature Scales in the Crust
Electro
ns TF
Ion TPlasma
Ions TDeBroglie
Ion TMelt (Γ=200)
TUmklapp
InnerCrust
OuterCrust
Tuesday, July 6, 2010
Relevant Temperature Scales in the Crust
Electro
ns TF
Ion TPlasma
Ions TDeBroglie
Ion TMelt (Γ=200)
TUmklapp
InnerCrust
OuterCrust
Acc
retin
g an
d M
agne
tized
Neu
tron
Sta
rs
Tuesday, July 6, 2010
Relevant Temperature Scales in the Crust
Electro
ns TF
Ion TPlasma
Ions TDeBroglie
Ion TMelt (Γ=200)
TUmklapp
InnerCrust
OuterCrust
Tc
Acc
retin
g an
d M
agne
tized
Neu
tron
Sta
rs
Tuesday, July 6, 2010
1011 1012 1013 1014
ρ (g/cm3)
0.01
0.1
Spee
d (in
uni
ts o
f c=3
x1010
cm
/s)
Longitudinal Lattice PhononsTransverse Lattice PhononsSuperfluid Phonons
Low Energy Excitations
1011 1012 1013 1014
ρ (g/cm3)
0.01
0.1
Spee
d (in
uni
ts o
f c=3
x1010
cm
/s)
Longitudinal Lattice PhononsTransverse Lattice PhononsSuperfluid Phonons
vs
cl
ct
!lPh(q) = cl q
!tPh(q) = ct q
!sPh(q) = vs q
!electron = q
How are these low energy modes coupled ? Tuesday, July 6, 2010
Low Energy Effective Field Theory
Neutron superfluid: Goldstone excitation is the phase of the condensate.
Proton (clusters) move collectively on lattice sites. Displacement is a good coordinate.
neutrons
protons
neutrons
protons
Tuesday, July 6, 2010
Low Energy Effective Field Theory
!i(x, y, z)
Neutron superfluid: Goldstone excitation is the phase of the condensate.
Proton (clusters) move collectively on lattice sites. Displacement is a good coordinate.
neutrons
protons
neutrons
protons
Tuesday, July 6, 2010
Low Energy Effective Field Theory
!i(x, y, z)
Neutron superfluid: Goldstone excitation is the phase of the condensate.
Proton (clusters) move collectively on lattice sites. Displacement is a good coordinate.
neutrons
protons
neutrons
protons
“coarse-grain”
Collective coordinates:
Vector Field: Scalar Field:
!i(r, t)!(r, t)
!!!(r)!"(r)" = |!| exp (#2i ")
Tuesday, July 6, 2010
Inner Crust EFT
Lp =12npm !t"i !t"i !
12
K !i"i!i"i !14
µs "ij "ij + · · ·
Compressibility
K ! !2E
!np!np
Shear Modulus
µs !Z2 e2
a4
!ij = "i!j + "j!i !23#ij "k!k
Protons:
Neutrons:
Son & Wingate (2006)
!!!(r)!"(r)" = |!| exp (#2i ")
! = µn t
Ground-state
Ln = P (µn)Tuesday, July 6, 2010
Inner Crust EFT
Lp =12npm !t"i !t"i !
12
K !i"i!i"i !14
µs "ij "ij + · · ·
Compressibility
K ! !2E
!np!np
Shear Modulus
µs !Z2 e2
a4
!ij = "i!j + "j!i !23#ij "k!k
Protons:
Neutrons:
Son & Wingate (2006)
!!!(r)!"(r)" = |!| exp (#2i ")
! = µn t
Ground-state
! !
Fluctuations (Superfluid Phonons)
Ln = P (µn)Tuesday, July 6, 2010
Coupling Neutrons and Protons. (or the superfluid and the lattice)
Gibbs-Duhem Relation: !µn = Enn !nn + Enp!np
!µn = !"t#! Enpnp"i$i
Velocities and current-current coupling :
Ln = P (µn) +!P
!µn"µn +
12
!2P
!µn!µn"µ2
n + · · ·
!µn = ! ("i#)2
2m+
12$ m (%vn ! %vp)2
!vn ="i#
m!vp = m "t$i
density-density interaction
current-current interaction
Tuesday, July 6, 2010
Coupling Neutrons and Protons. (or the superfluid and the lattice)
Gibbs-Duhem Relation: !µn = Enn !nn + Enp!np
!µn = !"t#! Enpnp"i$i
Velocities and current-current coupling :
Ln = P (µn) +!P
!µn"µn +
12
!2P
!µn!µn"µ2
n + · · ·
!µn = ! ("i#)2
2m+
12$ m (%vn ! %vp)2
!vn ="i#
m!vp = m "t$i
density-density interaction
current-current interaction
Ln = P (µn) + nn !µn +12"n! µ2
n + · · ·
Tuesday, July 6, 2010
The Coupled SystemLn+p =
12(!t")2 ! 1
2v2
s (!i")2 +12(!t#i)2 !
12(c2
l ! g2) (!i#i)2
v2s =
nf
m!nc2l =
K + 4µs/3m(np + nb)
nb = ! nnBound neutrons:Free neutrons: nf = nn (1! !){Entrainment: protons
drag neutrons.
Velocities :
Tuesday, July 6, 2010
The Coupled SystemLn+p =
12(!t")2 ! 1
2v2
s (!i")2 +12(!t#i)2 !
12(c2
l ! g2) (!i#i)2
v2s =
nf
m!nc2l =
K + 4µs/3m(np + nb)
nb = ! nnBound neutrons:Free neutrons: nf = nn (1! !){Entrainment: protons
drag neutrons.
Velocities :
+ g !t" !i#i + $̃ !i" !t#i
Longitudinal lattice phonons and superfluid phonons are coupled:
g = np Enp
!!n
m(np + nb)"̃ =
!nb vs"(np + nb)nf
Tuesday, July 6, 2010
The Coupled SystemLn+p =
12(!t")2 ! 1
2v2
s (!i")2 +12(!t#i)2 !
12(c2
l ! g2) (!i#i)2
v2s =
nf
m!nc2l =
K + 4µs/3m(np + nb)
nb = ! nnBound neutrons:Free neutrons: nf = nn (1! !){Entrainment: protons
drag neutrons.
Velocities :
+ g !t" !i#i + $̃ !i" !t#i
Longitudinal lattice phonons and superfluid phonons are coupled:
g = np Enp
!!n
m(np + nb)"̃ =
!nb vs"(np + nb)nf
Lt =12(!t"i)2 !
12c2t (!i"j + !j"i)2
Transverse lattice phonons:
c2t =
µs
m(np + nb)⇒
Tuesday, July 6, 2010
List of low energy constants
Thermodynamic Derivatives: Enn =
!2E
!nn!nnEpp =
!2E
!np!npEnp =
!2E
!nn!np
cl ct vs g !̃
K µs Enn Enp nb
g ! 10!3 " 10!2
Coupling between superfluid and lattice: !̃ ! 10!3 " 10!2
Tuesday, July 6, 2010
Two Applications
• Superfluid heat conduction.
• Effects of mixing and entrainment on the sound speeds.
Tuesday, July 6, 2010
Mixing and DissipationMixing of sound modes
Dissipation of lPh leads to dissipation of sPh
1011 1012 1013 1014
ρ (g/cm3)
0.01
0.1
Spee
d (in
uni
ts o
f c=3
x1010
cm
/s)
Longitudinal Lattice PhononSuperfluid PhononTransverse Lattice Phonons
Tuesday, July 6, 2010
Mixing and DissipationMixing of sound modes
Dissipation of lPh leads to dissipation of sPh
Tuesday, July 6, 2010
Mixing and DissipationMixing of sound modes
Dissipation of lPh leads to dissipation of sPh
Tuesday, July 6, 2010
Mixing and DissipationMixing of sound modes
Dissipation of lPh leads to dissipation of sPh
sPh mean free path
lPh mean free path
Tuesday, July 6, 2010
g̃mix = g + !̃ " =cl
vs
!lPh = cl "lPh
Mixing and DissipationMixing of sound modes
Dissipation of lPh leads to dissipation of sPh
sPh mean free path
lPh mean free path
Tuesday, July 6, 2010
g̃mix = g + !̃ " =cl
vs
!lPh = cl "lPh
Mixing and DissipationMixing of sound modes
Dissipation of lPh leads to dissipation of sPh
sPh mean free path
lPh mean free path
Away from resonance
Tuesday, July 6, 2010
Thermal Conductivity
107 K
108 K
109 K
neutron-drip
! =1
3Cv ! v ! "
Typically electrons dominate heat conduction.Processes:•Electron-phonon•Electron-impurity
Flowers & Itoh (1976)Uripin & Yakovlev (1980)
Tuesday, July 6, 2010
Thermal Conductivity
107 K
108 K
109 K
109 K
108 K
107 K
For T>108 K superfluid phonons play a role.
neutron-drip
! =1
3Cv ! v ! "
Typically electrons dominate heat conduction.Processes:•Electron-phonon•Electron-impurity
Flowers & Itoh (1976)Uripin & Yakovlev (1980)
Tuesday, July 6, 2010
Conductivity in Magnetized Neutron StarsMagnetic field suppresses transverse conduction
= Collision time
=Gyrofrequency
Canuto and Ventura (1977)Uripin & Yakovlev (1980)
Tuesday, July 6, 2010
Conductivity in Magnetized Neutron StarsMagnetic field suppresses transverse conduction
= Collision time
=Gyrofrequency
Canuto and Ventura (1977)Uripin & Yakovlev (1980)
Aguilera et al. (2009)
1013 G
1013 G1014 G
1014 G
Tuesday, July 6, 2010
Shear Mode Velocity:
Lowest energy modes dominate the specific heat.
c2t =
µs
m(np + nb)
Entrainment effects
µs !Z2e2
a4i
nb = ! nn
CV ! 4!2
15
T 3
c3t(T < TDebye)
Specific Heat
Chamel, Pethick, Reddy (in prep)Tuesday, July 6, 2010
Specific Heat at 1012 g/cm3
electronssh
ear m
ode
long
itudin
al m
ode
supe
rfluid
mod
e
107 108 109
T (K)
0.0001
0.001
0.01
0.1
1C
v (in
units
of n
i) Normal Neutrons !
Tuesday, July 6, 2010
Specific Heat at 1012 g/cm3
electronssh
ear m
ode
long
itudin
al m
ode
supe
rfluid
mod
e
107 108 109
T (K)
0.0001
0.001
0.01
0.1
1C
v (in
units
of n
i) Normal Neutrons !
Tuesday, July 6, 2010
Specific Heat at 1012 g/cm3
electronssh
ear m
ode
long
itudin
al m
ode
supe
rfluid
mod
e
107 108 109
T (K)
0.0001
0.001
0.01
0.1
1C
v (in
units
of n
i) Normal Neutrons !
CV ! CnormalV exp ("!
T)
Tuesday, July 6, 2010
Shear Mode Velocity & Magnetar QPOs
Duncan (1998)Watts & Strohmayer (2006)
!n=0,l=2 ! 2 ctR
!n=1 ! " ctR
!R
R
Tuesday, July 6, 2010
Conclusions
!Cool !CV
"(!R)2
Astronomy (Observations) Astrophysics
( Theory)
Nuclear Physics& Many-body
Theory
Insights about the nature of matter at extreme density
Tuesday, July 6, 2010
Back up slides
Tuesday, July 6, 2010
MixingMixing leads to oscillations
1011 1012 1013 1014
ρ (g/cm3)
0.01
0.1
Spee
d (in
uni
ts o
f c=3
x1010
cm
/s)
Longitudinal Lattice PhononSuperfluid PhononTransverse Lattice Phonons
Tuesday, July 6, 2010
Dissipative Processes
Electrons lPhs sPhs
Electron-phononprocesses
Impurity (Rayleigh)scattering
Multi electron and phonon processes
Tuesday, July 6, 2010
Dissipative Processes
Electrons lPhs sPhs
Electron-phononprocesses
Impurity (Rayleigh)scattering
Multi electron and phonon processes
Tuesday, July 6, 2010
Coupling to Electrons - Landau Damping
Electron particle-hole excitations damp collective modesand vice-versa.
Lel!lph =1
fel!ph!i"i #†
e #e
Lel!sPh !g̃mix
v2s(1" !2)
1fel!ph
"t# $†e $e
Induced coupling between superfluid phonons and electrons:
g̃mix = g + !̃ " =cl
vswhere
Tuesday, July 6, 2010
Heating in an Accreting Crust
Haensel & Zdunik (2003,2008) Gupta et al. (2007 & 2009)
Non-equilibrium reactions:Electron capture: Neutron transfers:Pycno-nuclear fusion:
e! + [A,Z] ! [A,Z " 1] + !e + Heat
n + [A,Z] ! [A+ 1, Z] + Heat
Tuesday, July 6, 2010