Quark Deconfinement As Supernova Explosion Engine for Massive Blue
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Surprises from the Search for Quark-Gluon Plasma?* When Was Quark-Gluon Plasma Seen?
Surprises from the search for quark-gluon plasma?* When was quark-gluon plasma seen? Richard M. Weiner Laboratoire de Physique Théorique, Univ. Paris-Sud, Orsay and Physics Department, University of Marburg The historical context of the recent results from high energy heavy ion reactions devoted to the search of quark-gluon plasma (QGP) is reviewed, with emphasis on the surprises encountered. The evidence for QGP from heavy ion reactions is compared with that available from particle reactions. Keywords: Quark-Gluon plasma in particle and nuclear reactions, hydrodynamics, equation of state, confinement, superfluidity. 1. Evidence for QGP in the Pre-SPS Era Particle Physics 1.1 The mystery of the large number of degrees of freedom 1.2 The equation of state 1.2.1 Energy dependence of the multiplicity 1.2.2 Single inclusive distributions Rapidity and transverse momentum distributions Large transverse momenta 1.2.3 Multiplicity distributions 1.3 Global equilibrium: the universality of the hadronization process 1.3.1 Inclusive distributions 1.3.2 Particle ratios -------------------------------------------------------------------------------------- *) Invited Review 1 Heavy ion reactions A dependence of multiplicity Traces of QGP in low energy heavy ion reactions? 2. Evidence for QGP in the SPS-RHIC Era 2.1 Implications of observations at SPS for RHIC 2.1.1 Role of the Equation of State in the solutions of the equations of hydrodynamics 2.1.2 Longitudinal versus transverse expansion 2.1.3 Role of resonances in Bose-Einstein interferometry; the Rout/Rside ratio 2.2 Surprises from RHIC? 2.2.1 HBT puzzle? 2.2.2 Strongly interacting quark-gluon plasma? Superfluidity and chiral symmetry Confinement and asymptotic freedom Outlook * * * In February 2000 spokespersons from the experiments on CERN’s Heavy Ion programme presented “compelling evidence for the existence of a new state of matter in which quarks, instead of being bound up into more complex particles such as protons and neutrons, are liberated to roam freely…”1. -
Deconfinement and Chiral Transition in Ads/QCD Wall Models
EPJ Web of Conferences 137, 03006 (2017) DOI: 10.1051/ epjconf/201713703006 XIIth Quark Confinement & the Hadron Spectrum Deconfinement and chiral transition in AdS/QCD wall models supplemented with a magnetic field David Dudal1;2;a, Diego R. Granado3;b, and Thomas G. Mertens4;2;c 1KU Leuven Campus Kortrijk - KULAK, Department of Physics, Etienne Sabbelaan 51 bus 7800, 8500 Kor- trijk, Belgium 2Ghent University, Department of Physics and Astronomy, Krijgslaan 281-S9, 9000 Gent, Belgium 3Departamento de Física, Universidade Federal Rural do Rio de Janeiro, BR 465-07, 23890-971, Seropédica, RJ, Brasil 4Joseph Henry Laboratories, Princeton University, Princeton, NJ 08544, USA Abstract. We discuss the phenomenon of (inverse) magnetic catalysis for both the de- confinement and chiral transition. We discriminate between the hard and soft wall model, which we suitably generalize to include a magnetic field. Our findings show a critical de- confinement temperature going down, in contrast with the chiral restoration temperature growing with increasing magnetic field. This is at odds with contemporary lattice data, so the quest for a holographic QCD model capable of capturing inverse magnetic catalysis in the chiral sector remains open. 1 Introduction The ongoing heavy ion collision programs (ALICE or RHIC) provide a fertile testing ground for novel experimental, phenomenological and theoretical features of strongly coupled QCD. During the early stages after the collision, a sufficiently hot heat bath is created that leads to the creation of a quark- gluon plasma, an exotic state of deconfined QCD matter. In units of the fundamental QCD scale, ΛQCD, the transition temperature Tdecon f ∼ ΛQCD, so the relevant physics is still strongly coupled. -
Supernova Neutrinos in the Proto-Neutron Star Cooling Phase and Nuclear Matter
TAUP 2019 IOP Publishing Journal of Physics: Conference Series 1468 (2020) 012089 doi:10.1088/1742-6596/1468/1/012089 Supernova neutrinos in the proto-neutron star cooling phase and nuclear matter Ken’ichiro Nakazato1 and Hideyuki Suzuki2 1 Faculty of Arts and Science, Kyushu University, 744 Motooka, Nishi-ku, Fukuoka 819-0395, Japan 2 Faculty of Science & Technology, Tokyo University of Science, 2641 Yamazaki, Noda, Chiba 278-8510, Japan E-mail: [email protected] Abstract. A proto-neutron star (PNS) is a newly formed compact object in a core collapse supernova. Using a series of phenomenological equations of state (EOS), we have systematically investigated the neutrino emission from the cooling phase of a PNS. The numerical code utilized in this study follows a quasi-static evolution of a PNS solving the general-relativistic stellar structure with neutrino diffusion. As a result, the cooling timescale evaluated from the neutrino light curve is found to be long for the EOS models with small neutron star radius and large effective mass of nucleons. It implies that extracting properties of a PNS (such as mass and radius) and the nuclear EOS is possible by a future supernova neutrino observation. 1. Introduction Core collapse supernovae, which are the spectacular death of massive stars, emit an enormous amount of neutrinos. In the case of SN1987A, a few tens of events were actually detected [1, 2, 3] and contributed to confirm the standard scenario for supernova neutrino emission. Although the neutron star formed in SN1987A has not yet been observed, its mass estimations had been attempted by using the neutrino event number [4, 5]. -
Excited Hadron States and the Deconfinement Transition
Excited Hadron States and the Deconfinement Transition Concluding Discussion Berndt Müller (Duke University) Workshop*) JLab - February 23-25, 2011 Friday, February 25, 2011 If we would hold a follow-up workshop in 2 years from now, which questions would we like to be answered? 2 Friday, February 25, 2011 Which QCD model describes the hadron (meson, baryon) spectrum best? E.g.: Constituent quark model MIT bag model Flux-tube model Holographic dual models Large Nc expansion Is there a “constituent gluon” model? If yes, how do we understand the large gluon mass? Scale breaking by the trace anomaly? Additional spontaneous scale invariance breaking? Is the constituent gluon a flux tube excitation? 3 Friday, February 25, 2011 What is the relation between the deconfinement transition and the chiral transition? Is it a well defined question? Are they at the “same” temperature? Do they drive each other? Where (at what T) and why does the hadron resonance gas model fail? Do unknown hadron states (hybrids, tetraquarks, glueballs) contribute significantly in the range of validity? If yes, which ones? 4 Friday, February 25, 2011 What are the requirements for a valid description of the hadronic break-up of the quark-gluon plasma? How must viscous hydrodynamics be matched to a kinetic description of the hadron gas? What are the minimal matching conditions? In which temperature range can the matching be performed? What are the most sensitive experimental tests? Where does the hot glue in the quark-gluon plasma go? Does it fragment into quark pairs? Does it initially end up in gluonic excitations? Is it possible to measure the average amount of excited glue in hadrons for a given mass or temperature on the lattice? 5 Friday, February 25, 2011 Can finite temperature lattice calculations determine average aspects of the hadron spectrum? Analogy with the Monte-Carlo shell model of Koonin, Ormand, Dean, Langanke, et al, who used MC methods to obtain level densities and Gamov-Teller strengths in the shell model for complex nuclei (e.g. -
Neutrinos from Core-Collapse Supernovae and Binary Neutron Star Mergers
Neutrinos from core-collapse supernovae and binary neutron star mergers Maria Cristina Volpe Astroparticules et Cosmologie (APC), Paris, France Sun core-collapse Supernovae McLaughlin Perego et al, 2014 accretion disks around black holes or neutron star mergers remnants Solar neutrino observations Vacuum averaged oscillations pep MSW solution 7Be 8B ν Survival Probability e Borexino, Nature 512 (2014) ν Neutrino Energy (MeV) Vacuum-averaged oscillations versus MSW suppression of high energy 8B neutrinos. Energy production of low mass main sequence stars confirmed — pp reaction chain. Future measurement of CNO neutrinos - main energy production in massive main sequence stars. The Mikheev-Smirnov-Wolfenstein effect Neutrinos interact with matter and undergo resonant adiabatic flavor conversion. Wolfenstein PRD (1978) Mikheev, Smirnov(1985) hmat = p2GF ⇢e mean-field approximation matter basis flavour basis ~ ν2 =νe ν , ν ν ν ~ ν2 µ τ e 2 ~ ν 1 =νµ ν~ 1 Effective mass Effective vacuum ν1 MSW resonance DENSITY 2 ∆m˜ /4E i✓˙M h⌫ = − − neutrino hamiltonian in the matter basis i✓˙ ∆m˜ 2/4E ✓ M ◆ ✓˙M Resonance condition : Adiabaticity : γ = | 2 | << 1 h h 0 ∆m˜ /4E ⌫,11 − ⌫,22 ⇡ Also in supernovae, in accretion disks around compact objects, in the Earth and in the Early Universe (BBN epoch) Heavy elements nucleosynthesis Two main mechanisms at the origin of elements heavier than iron : s-process (s-slow) and r-process (r-rapid). Double peak structures at the first A=90, the second A=130 and third A=190 peaks due to both the s-process and the r-process. The r-process sites : a longstanding question The r-process : neutron-capture is fast compared to half-lives of neutron-rich unstable nuclei. -
Nora Brambilla Quark Confinement and the Hadron Spectrum
Quark Confinement and the Hadron Spectrum XII Nora Brambilla Nora Brambilla Thessaloniki, 28 TU MUNICH August-4 September TU Munich 2016 4el Much of the way in which we develop science Aristotele’s apprehension of reality Aristotele’ school TIMES changed …… Conf12 venue but other things resisted the time the beauty of the place but other things resisted the time the temper, the determination and the ambition of the “locals” Modern Heros that organised 10 days of conference(s) with 400 participants, hundreds of talks, 7 sessions running in parallel , a social event each night and…. almost NO FUNDS ! and what allowed to surpass any difficulty was.. to have as Chair a true descendant of Cleopatra with the same inherited personality We can say that the Quark Confinement Conference shares some of the important Macedonian footprints • “Many different nations, cultures, languages.... “Macedoin” now means “a mix” We have the ambition to bring together all the people dealing with strong interactions from one perspective or the other Scientific Sessions of the conference Section A: Vacuum Structure and Confinement Mechanisms of quark confinement (vortices, monopoles, calorons...) and the structure of the vacuum in non-Abelian gauge theories. Chiral symmetry breaking, and the Dirac spectrum in the low-momentum region. Studies of ghost and gluon propagators. Confining strings and flux tubes, their effective actions. Renormalons and power corrections. Interface between perturbative and non-perturbative physics. Conveners: D. Antonov (Heidelberg), M. Faber (TU Vienna), J. Greensite (San Francisco State U) Focus Subsection: Emergent gauge fields and chiral fermions Chiral Fermions and anomalous hydrodynamic effects in condensed matter systems, quantum simulators of QCD, topological phenomena in condensed matter systems. -
Arxiv:2011.01466V2 [Hep-Lat] 28 Dec 2020
Deconfinement and Hadron Resonance Gas for Heavy ∗ Quarks Peter Petreczky Physics Deparment, Brookhaven National Laboratory, Upton, NY 11973, USA I discuss the deconfinement transition in 2+1 flavor QCD in terms of Polyakov loops as well as the hadron resonance gas for hadrons containing static quarks and charm quarks. PACS numbers: 12.38.Gc,12.38.Mh,25.75.Nq 1. Introduction Heavy quarks and infinitely heavy (static) quarks play an important role when discussing deconfinement transition in strongly interacting matter at high temperatures. The early works on deconfinement considered the free energy of static quark Q as well as the free energy of static quark antiquark (QQ¯) pair [1, 2, 3] and the lattice calculations of these quantities was a focus of many works, see Ref. [4] for a historic review. Deconfinement is closely related to color screening. The production rate of quarkonia, bound states of a heavy quark and anti-quark, was suggested as a probe of deconfinement in heavy ion collisions [5]. The basic idea behind this proposal was that the color screening in the deconfined medium effects the binding of heavy quarks (see also Ref. [6] for a review). Recent lattice QCD studies, however, mostly focus on the chiral aspects of the transition at high temperature, see e.g. Refs. [7, 8] for recent reviews. In this contribution I will discuss the deconfinement in 2+1 flavor QCD with (almost) physical quark masses in arXiv:2011.01466v2 [hep-lat] 28 Dec 2020 terms of Polyakov loops in different renormalization schemes. The Hadron Resonance Gas (HRG) model has been used to understand the thermodynamics below the cross-over temperature for many years [9, 10, 11, 12, 12, 13, 14, 15, 16]. -
Gigantic Japanese Detector Seeks Supernova Neutrinos Tracing the History of Exploding Stars Is a Goal of the Revamped Super-Kamiokande
NEWS IN FOCUS ASAHI SHIMBUN/GETTY Observations by the Super-Kamiokande neutrino detector have forced theorists to amend the standard model of particle physics. PHYSICS Gigantic Japanese detector seeks supernova neutrinos Tracing the history of exploding stars is a goal of the revamped Super-Kamiokande. BY DAVIDE CASTELVECCHI weight. These data will help astronomers to detector much better at distinguishing between better understand the history of supernovae different types, or ‘flavours’, of neutrino, as well leven thousand giant orange eyes in the Universe — but the neutrinos that the as their antiparticles, antineutrinos. confront the lucky few who have explosions emit have been difficult to detect. In 1987, the Kamiokande detector, Super-K’s entered the Super-Kamiokande under- “Every 2–3 seconds, a supernova goes off smaller predecessor, detected the first neutri- Eground neutrino observatory in Japan — by somewhere in the Universe, and it produces nos from a supernova. The dozen neutrinos far the largest neutrino detector of its kind in 1058 neutrinos,” says Masayuki Nakahata, came from Supernova 1987A, which occurred the world. A chance to see these light sensors who heads the Super-K, an international col- in the Large Magellanic Cloud, a small galaxy is rare because they are usually submerged in laboration led by Japan and the United States. that orbits the Milky Way. Head experimenter 50,000 tonnes of purified water. But a major With the upgrade, the detector should be able Masatoshi Koshiba shared the 2002 Nobel revamp of Super-K that was completed in to count a few of these ‘relic’ neutrinos every physics prize partly for that discovery. -
Astroparficle,Physics,, With,Mev,Neutrinos
University(of(Virginia,(HEP(Seminar,(April(21st(2015( Astropar(cle,physics,, with,MeV,neutrinos, Shunsaku(Horiuchi(( (Center(for(Neutrino(Physics,(Virginia(Tech)( Image(credit:(NASA/ESA( Contents, • IntroducJon:(why(astrophysical(neutrinos(now?( • Topic(1:(Supernova(neutrinos( – GalacJc(events:(rich(physics(and(astronomy( – Detectability(beyond(GalacJc(events( • Topic(2:(Dark(maPer(neutrinos( – Two(searches,(two(constraints( • Summary( UVa,(April(21st(2015( Shunsaku(Horiuchi((Virginia(Tech)( 2( Neutrinos,as,messenger,par(cles Neutrinos(are(great(messenger(parJcles:( • allow(us(to(see(opJcally(thick((to(photons)(regions( • experience(liPle(aPenuaJon(through(cosmic(space( • travel(in(straight(lines( Source Neutrinos gamma(rays( Cosmic(raysCosmic(rays( MagneJc(field UVa,(April(21st(2015 Shunsaku(Horiuchi((Virginia(Tech) 3( Neutrino,detec(on:,Cherenkov,, Use(the(Cherenkov(light(to(reconstruct(the(original(neutrino( ν" IceCube( Eν >(10(GeV( Muon(range(increases( the(effecJve(volume(( lepton( e( Du>a,et,al,,PRD,(2001),, SuperVKamiokande( Eν(>(few(MeV(( Volume(~(50(kton(of(water( Volume(~(1(Gton(of(ice( UVa,(April(21st(2015( Shunsaku(Horiuchi((Virginia(Tech)( 4( Neutrino,sources, RadioacJve(decay( Sun((x1)( Nuclear( Supernova((x1)( reactors( ParJcle( Astrophysical( accelerator( accelerator( Likely' Cosmic(background( Atmospheric( +(others?( UVa,(April(21st(2015(Shunsaku(Horiuchi((IPMU)((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((((Shunsaku(Horiuchi((Virginia(Tech)( -
QUARK DECONFINEMENT and HIGH Energf I9 NUCLEAR COLLISIONS
BNL—38530 BROOKHAVIN NATIONAL LABORATORY DE87 001374 July 1986 BNL- ' >••> QUARK DECONFINEMENT AND HIGH ENERGf I9 NUCLEAR COLLISIONS H. Satz Fakultat fur Physik Universitat Bielefeld, D-48 Bielefeld, F.R. Germany and Physics Department Brookltaven National Laboratory, Upton, NY 11973, USA ABSTRACT Statistical QCD predicts that with increasing density, strongly inter- acting matter will undergo a transition to a plasma of deconfined quarks and gluons. High energy heavy ion collisions are expected to permit exper- imental studies of this transition and of the predicted new state of matter. Talk given at the XXIII International Conference on High Energy Physics, 1C-23 July 1980, Berkeley, California, USA. This manuscript has been authored under contract number D10-ACO2-7OCIIOUU1C with the U.S. Depn.rt.- ment of Energy. Accordingly, the U.S. Government retains a non-exclusive, royalty-free license to publish or reproduce the published form of this contribution, or allow others to do so, for U.S. Government purposes. DISTRIBUTION OF THIS DOCUMEKT !S UNLIMITED yfi 1. Introduction High energy hadron collisions have provided the empirical basis for strong interaction dynamics. It is our hope that high energy heavy ion collisions will do the same for strong interaction thermodynamics, that they will become the tool with which we can carry out the experimental analysis of strongly interacting matter. We recall that thermodynamics, in studying the collective behaviour of many components, may well lead to new physics, beyond the known dynamics. In solid state physics, ferromagnetism and superconductivity are just two striking examples of this. We shall see shortly that the statistical mechanics obtained with QCD as dynamical input in fact does predict new states of matter. -
Gravitating Bubbles of Gluon Plasma Above Deconfinement Temperature
S S symmetry Article Gravitating Bubbles of Gluon Plasma above Deconfinement Temperature Yves Brihaye 1 and Fabien Buisseret 2,3,∗ 1 Service de Physique de l’Univers, Champs et Gravitation, UMONS Research Institute for Complex Systems, Université de Mons, Place du Parc 20, 7000 Mons, Belgium; [email protected] 2 Service de Physique Nucléaire et Subnucléaire, UMONS Research Institute for Complex Systems, Université de Mons, Place du Parc 20, 7000 Mons, Belgium 3 CeREF, Chaussée de Binche 159, 7000 Mons, Belgium * Correspondence: [email protected] Received: 2 September 2020; Accepted: 8 October 2020; Published: 13 October 2020 Abstract: The equation of state of SU(3) Yang–Mills theory can be modelled by an effective Z3−symmetric potential depending on the temperature and on a complex scalar field f. Allowing f to be dynamical opens the way to the study of spatially localized classical configurations of the scalar field. We first show that spherically symmetric static Q-balls exist in the range (1 − 1.21) × Tc, Tc being the deconfinement temperature. Then we argue that Q-holes solutions, if any, are unphysical within our framework. Finally, we couple our matter Lagrangian to Einstein gravity and show that spherically symmetric static boson stars exist in the same range of temperature. The Q-ball and boson-star solutions we find can be interpreted as “bubbles” of deconfined gluonic matter; their mean radius is always smaller than 10 fm. Keywords: deconfinement; Matter-gravity coupling; Yang–Mills theory; Q-ball; boson star 1. Introduction A fascinating feature of Yang–Mills theory is the existence of a deconfinement temperature, Tc, above which free color charges (free gluons) may propagate without being confined into color singlets [1,2]. -
Neutrinos from Supernovae Detecting the Diffuse Supernova Neutrino Background
Neutrino Probes of Supernovae Shunsaku Horiuchi (Uni of Tokyo, IPMU) IPMU ACP Seminar, 14th May 2009 Introduction Thermal neutrinos from supernovae Detecting the diffuse supernova neutrino background Non-thermal neutrinos from supernovae Gamma-ray burst context (Magnetic stars) Summary Shunsaku Horiuchi (IPMU) 2 The Dream of Neutrino Astronomy “If [there are no new forces] -- one can conclude that there is no practically possible way of observing the neutrino.” Bethe&Peierls, Nature (1934) “The title is more of an expression of hope than a description of the book’s contents....the observational horizon of neutrino astrophysics may grow...perhaps in a time as short as one or two decades.” Bahcall, Neutrino Astrophysics (1989) We now have the technology to detect neutrinos! And we know neutrino sources exist. Neutrinos are unique messengers in astrophysics. It is timely to study astrophysical neutrinos Shunsaku Horiuchi (IPMU) 3 Some neutrino sources Radioactive Sun (x1) decay Nuclear Supernova (x1) reactors Particle Astrophysical accelerator soon accelerator Cosmic Atmospheric background Shunsaku Horiuchi (IPMU) 4 Supernova neutrinos are Many MeV neutrinos [thermal] Core-collapse of massive star (x1) How are neutron stars and black holes formed? GeV – TeV neutrinos [non-thermal] Supernova, supernova remnants, and gamma-ray bursts Particle acceleration and hadronic interactions? > TeV neutrinos [non-thermal] Gamma-ray bursts? What are the origins of high-energy cosmic rays? Each gives us valuable information Shunsaku