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