Topological defects creation at fast transition: Kibble mechanism and Zurek scenario
Experiments with neutrons:Vortex creation in 3He+n reaction
Dark matter searchMuons and electrons scintillation
A-B transition in 3HeAurora de Venice versus Baked Alaska
Q-ball in 3He-BPersistent induction signal
COSLAB and TOPDIFCOSLAB and TOPDIFGrenoble connectionGrenoble connection
Yuriy M. Bunkov C R T B T – C N R S, Grenoble, France
E
A ei
Suprconducters,
4He,
1/4
4He experiment: Lancaster UniversityFast pressure release. P.C.Hendry, N.S Lawson, R.A.M. Lee, P.V.E. McClintock, C.H.D. Williams, Nature, 368, 315 (1994)
T
P
Superfluid
Solid
Liquid
No conformation at better prepared experiments
2K
3He experiments: Lancaster Grenoble and Helsinki fast cooling after a localise heating from 3He neutron nuclear reaction
n + 3He = p + 3H + 764 keV
C. Bauerle, Yu.M.Bunkov, S.N.Fisher, H. Godfrin, G.R.Pickett, Nature, 382, 332 (1996)
V.M.H. Ruutu, V.B.Eltsov, A.J.Gill, T.W.B. Kibble, M. Krusius, Yu.G. Makhlin, B. Placcais, G.E. Volovik, W. Xu, Nature , 382, 334, (1996)
P
T
Solid
LiquidSuperfluid B A
Helsinki
Grenoble
+ rotation
1mK
D.I. Bradley, Yu.M.Bunkov, D.J.Cousins, M.P.Enrico,S.N.Fisher, M.R.Follows, A.M.Guénault, W.M.Hayes, G.R.Pickett, T.Sloan, Phys. Rev. Lett., v. 75. p. 1887, (1995)
Yuriy M. Bunkov Henri GodfrinEddy Collin
Matty Krusius
Shaun FisherDerek J. Cousins
Cristopher. Bäuerle Ann-Sophie ChenClemens WinkelmannJohannes Elbs
Superfluid 3He bolometry
60 µm hole
Sintered silverCopper box
Vibrating Wires (5 µm and 13 µm)
4.5
5
5.5
6
6.5
12:00 12:10 12:20 12:30 12:40 12:50 13:00
Neutrons detection
Time
760 keV
13,1
13,15
13,2
13,25
13,3
6:00:00 6:12:00 6:24:00 6:36:00 6:48:00 7:00:00
Particle-Background Detection
TIME
100 keV
n + 3He = p + 3H + 764 keV
scintillation0
40
80
120
160
200
240
0 5 10 15 20 25 30
En
erg
y d
efic
ite
(keV
)
Pressure (bar)
Grenoble 1995
scintillation0
40
80
120
160
200
240
0 5 10 15 20 25 30
En
erg
y d
efic
ite
(keV
)
Pressure (bar)
Grenoble 1995
Theory: V.B. Eltsov, M. Krusius, G.E. Volovik Progress Low Temp Phys 2005
scintillation
Grenoble 1995
Theory: V.B. Eltsov, M. Krusius, G.E. Volovik Progress Low Temp Phys 2005
Grenoble 2004
0
40
80
120
160
200
240
0 5 10 15 20 25 30
En
erg
y d
efic
ite
(keV
)
Pressure (bar)
scintillation0
40
80
120
160
200
240
0 5 10 15 20 25 30
En
erg
y d
efic
ite
(keV
)
Pressure (bar)
Grenoble 2004Grenoble 1995
Theory: V.B. Eltsov, M. Krusius, G.E. Volovik Progress Low Temp Phys 2005
Grenoble 2005
1/√T
Bolometric calibration by pulsed heating
-0.05
0
0.05
478 480 482 484 486
V (V
)
fréquence (Hz)
W(T)
Signal en phase
Signal en quadrature
0.41
0.43
0.45
0.47
0 10 20 30
Wre
t (H
z)
temps (s)
y = 0.414+m1*(m3/(m3-0.77))*...
ErrorValue
9.0417e-050.054976m1
0.00429560.057101m2
0.0122635.1739m3
NA1.5681e-05Chisq
NA0.99978R
H
A
G.M.SeidelG. R. Pickett
H. Godfrin
In 3He + n reaction 9% +- 1%of energy going for scintillation
From the fit, the energy emitted into a solid angle of 4 steradians is 87 keV, or 24% of the total energy of the 364 keV electron. In contrast, for an alpha particle stopped in helium we found, upon correcting for reflectivity, that only 10% of the initial energy of the particle is emitted as uv radiation.Journal of Low Temperature Physics, Vol. 113, 5/6, 1998
scintillation
0
40
80
120
160
200
240
0 5 10 15 20 25 30
En
erg
y d
efic
ite
(keV
)
Pressure (bar)
Grenoble 2004Grenoble 1995
Theory: V.B. Eltsov, M. Krusius, G.E. Volovik Progress Low Temp Phys 2005
Grenoble 2005
Analysis and simulation
LPSC (GEANT4)
• Detection of cosmic muons: good agreement experience/simulation if
fUV(muons) ≈ 25 %
coincidence
Wm
es(
Hz)
time (s)
260
262
264
266
0 100 200 300
W(t
) (m
Hz)
temps (s)
10 keV
Time (s)
cell A (without source)cell B (with source)
Electron detection spectrum
• resolution of low energy emission spectrum of 57Co
• Comparison to 14 keV peak with bolometric calibration Energy deficit of fUV(e-,14keV)≈265%
UV Scintillation
S/B>5Analysis LPSC, d5, B=100 mT, W0=430 mHz
The idea : Use the Bose –Einstein condensed coherent quantum state of superfluid 3He at
a limit of extremely low temperatures as a sensitive medium for the direct bolometric search of non-baryonic Dark Matter
First suggestionG.R.Pickett in Proc. «Second european worshop on neutrinos and dark matters detectors», ed by L.Gonzales-Mestres and D.Perret-Gallix, Frontiers, 1988, p. 377.
Yu.Bunkov, S.Fisher, H.Godfrin, A.Guenault, G.Pickett. in Proc. « International Workshop Superconductivity and Particles Detection (Toledo, 1994)», ed. by T.Girard, A.Morales and G.Waysand. World Scientific, p. 21-26.
Ultra Low Temperature Ultra Low Temperature Instrumentation for Measurements Instrumentation for Measurements
in Astrophysicsin Astrophysics
Bose – Einstein condensed coherent quantum state Bose – Einstein condensed coherent quantum state with rear gas of collective excitations.with rear gas of collective excitations.
At about 100 mK at 0.1 cm3 remains At about 100 mK at 0.1 cm3 remains only 10 keV from the level only 10 keV from the level of absolute zero of temperature. of absolute zero of temperature.
Temperature is the density of Temperature is the density of quasiparticles, that measured quasiparticles, that measured directly by damping of mikro directly by damping of mikro vibrating wire.vibrating wire.
The deposited energy is intimatelyThe deposited energy is intimatelyassociated with the 3He nuclear. associated with the 3He nuclear. There is no isolated nuclear thermal There is no isolated nuclear thermal bath, separated from electronic bath, separated from electronic and phononic subsystems!and phononic subsystems!
Candidates What is the dark matter made of ?
The non-baryonic candidate zoo Gianfranco Bertonea, Dan Hooperb, Joseph Silkb, Physics Reports 405 (2005) 279–390
Standard Model neutrinos < 0.07Sterile neutrinos (without Standard Model weak interactions)Axions Introduced in an attempt to solve the problem of CP violation in particle physics
Supersymmetric candidatesNeutralinos WIMP Sneutrinos (superpartners of the Standard Model neutrinos in supersymmetric models) Gravitinos (superpartners of the graviton in supersymmetric models.)Axinos (superpartner of the axion,)
Light scalar dark matter (fermionic dark matter candidates)Dark matter from little Higgs modelsKaluza–Klein excitations of Standard Model fields which appear in models of universal extra dimensionsSuperheavy dark matter called Wimpzillas,Q-balls, mirror particles, CHArged Massive Particles (CHAMPs), self interacting dark matter, D-matter, cryptons, superweakly interacting dark matter, brane world dark matter, heavy fourth generation neutrinos, etc.
100g 100g 33He detectorHe detector
Spin dependent interactionSpin dependent interaction
For spin dependent interaction 100g 3He = 30 kg Ge
scintillation
0
40
80
120
160
200
240
0 5 10 15 20 25 30
En
erg
y d
efic
ite
(keV
)
Pressure (bar)
Grenoble 2004Grenoble 1995
Theory: V.B. Eltsov, M. Krusius, G.E. Volovik Progress Low Temp Phys 2005
Grenoble 2005
P
T
Solid
LiquidSuperfluid B A
Helsinki
Grenoble
+ rotation
1mK
70 m10 m
1 m
p
3H- Meyer, Sloan, JLTP 1998
D(0bar) = 21 cm2/s; R=27mD(19bar) = 0.94 cm2/s; R=12m
E
A ei
Suprconducters,
4He,
Aik ei3He, Universe Aik
ik
Bunkov and Timofeevskaya modification of Kibble-Zurek theory PRL 1998
3He-A
Inflation of B phase in the space of A phase
Transition triggered by radiation (Osheroff)
“Baked Alaska” due to Leggett does not work
Volovik suggestion, LT, Praga, 1996
40
45
50
55
60
65
70
-0.05
0.00
0.05
0.10
0.0 5.0 10 15 20 25 30 35
F, (B-A)
Pressure, (bar)
-0.35
-0.30
-0.25
-0.20
-0.15
-0.10
-0.05
0.00
0.05
0.0 0.050 0.10 0.15 0.20 0.25
214347
Time, (s)
A
B
Figure 1
18 D manifold
B
P
T
Solid
LiquidSuperfluid B
A
A – B transition
P
T
Solid
LiquidSuperfluid B
A
A – B transition