Topological defects creation at fast transition: Kibble mechanism and Zurek scenario Experiments with neutrons: Vortex creation in 3He+n reaction Dark matter search Muons and electrons scintillation A-B transition in 3 He Aurora de Venice versus Baked Alaska Q-ball in 3 He-B Persistent induction signal COSLAB and TOPDIF Grenoble connection Yuriy M. Bunkov C R T B T – C N R S, Grenoble, France

E A e i  Suprconducters, 4 He, 1/4

4 He experiment: Lancaster University Fast 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 3 He experiments: Lancaster Grenoble and Helsinki fast cooling after a localise heating from 3 He neutron nuclear reaction n + 3 He = p + 3 H 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 Liquid Superfluid 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 Godfrin Eddy Collin Matty Krusius Shaun Fisher Derek J. Cousins Cristopher. Bäuerle Ann-Sophie Chen Clemens Winkelmann Johannes Elbs

Superfluid 3 He bolometry

n + 3 He = p + 3 H keV

scintillation Grenoble 1995

scintillation 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

scintillation Grenoble 2004 Grenoble 1995 Theory: V.B. Eltsov, M. Krusius, G.E. Volovik Progress Low Temp Phys 2005 Grenoble 2005

 1/√T Bolometric calibration by pulsed heating 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 Grenoble 2004 Grenoble 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 f UV (muons) ≈ 25 %

coincidence W mes (Hz) time (s) W(t) (mHz) temps (s) 10 keV Time (s)

cell A (without source) cell B (with source) Electron detection spectrum resolution of low energy emission spectrum of 57 Co Comparison to 14 keV peak with bolometric calibration  Energy deficit of f UV (e -,14keV)≈265% UV Scintillation S/B>5 Analysis LPSC, d5, B=100 mT, W0=430 mHz

The idea : Use the Bose –Einstein condensed coherent quantum state of superfluid 3 He at a limit of extremely low temperatures as a sensitive medium for the direct bolometric search of non-baryonic Dark Matter First suggestion G.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 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 Ultra Low Temperature Instrumentation for Measurements in Astrophysics

Bose – Einstein condensed coherent quantum state 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 of absolute zero of temperature. Temperature is the density of quasiparticles, that measured directly by damping of mikro vibrating wire. The deposited energy is intimately associated with the 3He nuclear. There is no isolated nuclear thermal bath, separated from electronic 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 < 0.07 Sterile neutrinos (without Standard Model weak interactions) Axions Introduced in an attempt to solve the problem of CP violation in particle physics Supersymmetric candidates Neutralinos 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 models Kaluza–Klein excitations of Standard Model fields which appear in models of universal extra dimensions Superheavy 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 3 He detector Spin dependent interaction For spin dependent interaction 100g 3 He = 30 kg Ge

scintillation Grenoble 2004 Grenoble 1995 Theory: V.B. Eltsov, M. Krusius, G.E. Volovik Progress Low Temp Phys 2005 Grenoble 2005

P T Solid Liquid Superfluid B A Helsinki Grenoble + rotation 1mK 70  m10  m 1  m p 3H-3H- Meyer, Sloan, JLTP 1998 D(0bar) = 21 cm 2 /s; R=27  m D(19bar) = 0.94 cm 2 /s; R=12  m

E A e i  Suprconducters, 4 He, A ik e i  3 He, Universe A ik ik Bunkov and Timofeevskaya modification of Kibble-Zurek theory PRL He-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

18 D manifold B P T Solid Liquid Superfluid B A A – B transition

P T Solid Liquid Superfluid B A A – B transition