Collider to Cosmology- Mini Bang to the Big Bang

1. Collider to Cosmology- Mini Bang to the Big Bang Bikash Sinha INSA Emeritus Scientist Variable Energy Cyclotron Centre Festschrift, Professor Pijushpani Bhattacharya 13th October, 2015

2. Four basic forces United Infinitely small universe ? BIG BANG DAWN OF TIME Physics as we know it does not exist

3. HUBBLE’S DISCOVERY Universe is expanding. The expansion follows specific mathematical relation. This implies universe was much smaller in the past and hence it was much denser and hotter. In the early universe matter existed in the form of fundamental particles. UNIVERSE STARTED WITH A BIG BANG !!

4. Big Bang Universe was born 14 billion years ago through a massive explosion called Big Bang. At that moment, all matter was compressed into a space billions of times smaller than a proton. Beginning of space and time. Since that moment the cosmic bodies are moving away from each other, and the universe is expanding.

5. Cosmic Time Line Arrow of Time 12-14 Billion years 1 Billion years 100 Million years 1 Million years BIG BANG Emission of cosmic background radiation Dark ages First stars First supernovae and black holes Modern galaxies

6. Cosmic Time Line Arrow of Time 12-14 Billion years 1 Billion years 100 Million years 1 Million years BIG BANG Emission of cosmic background radiation Dark ages First stars First supernovae and black holes Modern galaxies

9. The cosmological big bang is played out at LHC albeit in a miniature scale, with the little bangs between two nuclei. As is well known the big bang is a display of gravity, space and time where as the little bang is essentially to do with confinement and subsequently to deconfinement in extreme conditions. On the other extreme end of the phase diagramme lies a domain of very high baryonic density but at rather low temperature, a scenario for neutron star matter, of compressed baryonic matter and a temperature, very near zero.

10. It is widely conjectured that the quark gluon sector of such matter may indeed consist of “colour super conductors” and high density hadronic (neutron) matter or hybrid matter in the hadronic sector. We study the spin down behaviour of a rotating neutron star with the realisation that changes in the internal structure as the star spins down, will be reflected in the moment of inertia and hence the deceleration. In this letter we are not considering the “recycling” scenario of binary system. During the spin down of a (say) millisecond neutron star, the central density increases with decreasing centrifugal force; leading to a phase transition from the somewhat incompressible nuclear matter to the highly compressible, perfect fluid, quark matter in the stellar core.

11. Indeed as the bulge of quark matter in the stellar core increases in dimension, a perfect fluid of QCD colour will set in, and, the perfect colour fluid will splash into hadronic matter transforming more of hadronic matter to colour superconducting quark matter. After the quark gluon matter dominates in the core, the star would contract significantly and its moment of inertia decreases sharply, a common signature of phase transition from confined to deconfined matter.

12. The nature of the phase transition from hadrons to quarks in a neutron star, thus is unique and very different; from the experiments carried out on our earth. The continuous process of phase transition closely resembles cross over but not exactly identical. It is felt that by means of designing ingenious experiments conducted by ”CBM” type of detector this novel matter can be discovered; one possibility of course is to study ”CBM” but at cooler environment, analogous to the core of neutron star.

15. Possible existence of quark- matter in dense neutron- stars is discussed using Quantum Chromo-dynamical equation of state for cold degenerate quark- matter.

16. Radiation at CERN-SPS

17. WA98 Experiment at CERN-SPS • Observation of collective flow • Phys. Lett. B403 (1997) 390. • Scaling of particle production: • Phys. Lett. B458 (1999) 422. • DCC Search: • Phys. Lett. B420 (1998) 169 • Phys.Rev.C64:011901,2001, • Phys. Rev. C 2003 • Fluctuations: • Phys. Rev. C, May 2002 • DIRECT PHOTONS

18. PMD in WA98 Experiment

19. Brookhaven National Laboratory, New York STAR PHENIX BARC & BHU  STAR h STAR IOP Bhubaneswar Panjab U., Chandigarh Rajasthan U., Jaipur Jammu U., Jammu VECC, Kolkata 1 km PHOBOS RHIC PHENIX BRAHMS

20. STAR experiment at RHIC, BNL

21. CERN, Geneva • ALICE @ LHC: • Photon Multiplicity Detector • IOP Bhubaneswar • Panjab U. Chandigarh • Rajasthan U. Jaipur • Jammu U. Jammu • VECC Kolkata • Muon Arm Project • SINP Kolkata • AMU Aligarh LHC 9km SPS WA93 & WA98 @ SPS: IOP Bhubaneswar Panjab U., Chandigarh Rajasthan U., Jaipur Jammu U., Jammu VECC, Kolkata

22. ALICE Experiment at LHC Muon chambers PMD Modules MUON arm m-pairs PMD photons

25. (nucl-th/0508043, J. Alam, J. Nayak, P.Roy, A. Dutt-Mazumder, B.S.) Radiation at RHIC

26. J.K. Nayak, B. Sinha / Physics Letters B 719 (2013) 110–115 26

27. FROM THE TERRESTRIAL LIGHT to THE COSMIC LIGHT, NO ORDINARY LIGHT Light from large Megellanic clouds – 150,000 light years away

29. Survivability of Cosmological Quark Nuggets: (Chromoelectric flux-tube fission model): First order phase transition (q-h) E. Witten Phys. Rev. D 30 (1984) P. Bhattacharya, J. Alam, B.Sinha, Sibaji Raha: Phys Rev.D 48 (1993)

30. Chromo electric Flux-tube fission P. Bhattacharya J. Alam S. Raha B.S. (PRD ’93) [dNB/dt]abs = -2π2 [ nN υN / mN T2] exp [mN - μNq / T ] [ dNB / dt ] ev The net charge of baryon number of the QN is dNB /dt = [dNB/dt ]ev + [dNB/dt]abs

32. Strange quark nuggets (SQN) H L H L L L L H L L Isolated expanding bubbles of low temp In high temp phase Expanding bubbles meet H L L L H Isolated shrinking bubbles of High temp phase

33. • • o • • • o o CEFT MODEL Glendenning & matsui -1983 meson evaporation Sumiyoshi et al 1990 Baryon evaporation

34. QN with a baryon number NB at the time t will stop evaporating further (thus survive) if the “time scale” of evaporation >> Hubble expansion (Cooling time scale)

35. [Source: P. Bhattacharjee, J. Alam, B. Sinha and S. Raha, 1993, Phys. Rev. D 48, 10, 4630-4638

36. [Source: P. Bhattacharjee, J. Alam, B. Sinha and S. Raha, 1993, Phys. Rev. D 48, 10, 4630-4638

37. [Source: P. Bhattacharjee, J. Alam, B. Sinha and S. Raha, 1993, Phys. Rev. D 48, 10, 4630-4638

38. So, Quark Nuggets with NB , in ≥ 1043. 5 are stable and survive forever!!

39. MACHO , Relics of Q-H phase transition Sibaji Banerjee A. Bhattacharya S. Ghose S. Raha, B.Sinha Mon. Not. R. Astronomical Society (2002)

40. Gravitational Lensing : (13-17) Milky Way halo MACHOs, detected in the direction of Large Magellanic cloud Mass range (0.15-0.95) Mסּ Most probable ~ 0.5 Mסּ Suttherland (1999) Alocock (2000)

41. Above the threshold for Nuclear fusion => evolution of metastable (TFVD) (Strange Quark Nuggets, SQN) Entire Cold Dark Matter (CDM) (ΩCDM~0.3-0.35) can be comfortably explained by stable SQN’s Alam, Raha & B.S. Astrophysical journal (1999) S. Banerjee et. al. PLB 611 (2005) Nucl. Phys A774(2006)

42. Cold Dark Matter and the Cosmic Phase Transition

43. It is entirely plausible that during the primordial quark hadron phase transition in the universe, microseconds after the Big Bang, supercooling takes place, accompanied by mini inflation. With μ/T ∼ 1 (μ is chemical potential), leading to a first order phase transition, there will be relics in the form of quark nuggets, and, that they consist of Strange Quark Matter. The possibility that these SQM nuggets may well be the candidates of cold dark matter is critically examined. A cursory comparison with the neutron star is presented at the end. …to be published in Journal of Physics: Conference Series

44. Ref: Boeckel T and Schaner- Bielich J 2010 Phys. Rev. Lett. 105 041301

45. - η b/ ηγ ~ 10 -10 - expansion time scale ~ 10 –5 sec ____ Mini Bang = Big Bang ? Turbulance Inflation Gravitation Horizon

46. LITTLE BANGVS.BIG BANG(B.B) 1. B.B expanding against the pull of Gravity (G) L.B expanding against the pull of the Bag (B) Both Very Violent

47. Anisotropy isotropy 2. Entropy is mysteriously produced at some early stage t Approximately conserved later v B.B. H(t) : time dependent “Hubble’’ Const v L.B. HT : Tensor ; anisotropic as time t ~ Freeze out ~ Hubble like

48. QGP Hadrons ( Zero density & Pressure ) “B” deccelerate 3. B.B : Eq. Of state, Gravity DARK MATTERS Even “shocking” DARK Energy ~ 73% (-ve) pressure Accl Universe (Non Zero Cosmological Const)

49. Are seen at the moment of their last interaction (decouple) freeze out Ω- hyperons decouple earlier and/or Leptons & photons Fluctuation : 5. 4. L.B. : ( Observed Hadrons ) Analogous to the microwave cosmic radiation of B.B : ∆ (Microwave heat both) (L.B) QGP Hadrons ( Fluctuation ) B. B is much better studied