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QCD matter

(Redirected fromQuark matter)

Quark matterorQCD matter(quantum chromodynamic) refers to any of a number of hypotheticalphasesof matter whosedegrees of freedomincludequarksandgluons,of which the prominent example isquark-gluon plasma.[1]Several series of conferences in 2019, 2020, and 2021 were devoted to this topic.[2][3][4]

Quarks are liberated into quark matter at extremely high temperatures and/or densities, and some of them are still only theoretical as they require conditions so extreme that they cannot be produced in any laboratory, especially not at equilibrium conditions. Under these extreme conditions, the familiar structure ofmatter,where the basic constituents arenuclei(consisting ofnucleonswhich are bound states of quarks) and electrons, is disrupted. In quark matter it is more appropriate to treat the quarks themselves as the basic degrees of freedom.

In thestandard modelof particle physics, thestrong forceis described by the theory ofQCD.At ordinary temperatures or densities this force justconfinesthe quarks into composite particles (hadrons) of size around 10−15m = 1femtometer= 1 fm (corresponding to the QCD energy scale ΛQCD≈ 200MeV) and its effects are not noticeable at longer distances.

However, when the temperature reaches the QCD energy scale (Tof order 1012kelvins) or the density rises to the point where the average inter-quark separation is less than 1 fm (quarkchemical potentialμ around 400 MeV), the hadrons are melted into their constituent quarks, and the strong interaction becomes the dominant feature of the physics. Such phases are called quark matter or QCD matter.

The strength of the color force makes the properties of quark matter unlike gas or plasma, instead leading to a state of matter more reminiscent of a liquid. At high densities, quark matter is aFermi liquid,but is predicted to exhibitcolor superconductivityat high densities and temperatures below 1012K.

Unsolved problem in physics:
QCD in the non-perturbativeregime:quark matter.The equations of QCD predict that asea of quarks and gluonsshould be formed at high temperature and density. What are the properties of thisphase of matter?
(more unsolved problems in physics)

Occurrence

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Natural occurrence

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  • According to theBig Bangtheory, in the early universe at high temperatures when the universe was only a few tens of microseconds old, the phase of matter took the form of a hot phase of quark matter called thequark–gluon plasma(QGP).[5]
  • Compact stars(neutron stars). A neutron star is much cooler than 1012K, but gravitational collapse has compressed it to such high densities, that it is reasonable to surmise that quark matter may exist in the core.[6]Compact stars composed mostly or entirely of quark matter are calledquark starsorstrange stars.
  • QCD matter may exist within thecollapsarof agamma-ray burst,where temperatures as high as 6.7 × 1013K may be generated.

At this time no star with properties expected of these objects has been observed, although some evidence has been provided for quark matter in the cores of large neutron stars.[7]

  • Strangelets.These are theoretically postulated (but as yet unobserved) lumps ofstrange mattercomprising nearly equal amounts of up, down and strange quarks. Strangelets are supposed to be present in the galactic flux of high energy particles and should therefore theoretically be detectable incosmic rayshere on Earth, but no strangelet has been detected with certainty.[8][9]
  • Cosmic rayimpacts. Cosmic rays comprise a lot of different particles, including highly accelerated atomic nuclei, particularly that ofiron.

Laboratory experiments suggests that the inevitable interaction with heavynoble gasnuclei in theupper atmospherewould lead to quark–gluon plasma formation.

Laboratory experiments

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Particle debris trajectories from one of the first lead-ion collisions with the LHC, as recorded by theALICEdetector. The extremely brief appearance of quark matter in the point of collision is inferred from the statistics of the trajectories.

Even though quark-gluon plasma can only occur under quite extreme conditions of temperature and/or pressure, it is being actively studied atparticle colliders,such as the Large Hadron ColliderLHCatCERNand the Relativistic Heavy Ion ColliderRHICatBrookhaven National Laboratory.

In these collisions, the plasma only occurs for a very short time before it spontaneously disintegrates. The plasma's physical characteristics are studied by detecting the debris emanating from the collision region with large particle detectors[11][12]

Heavy-ion collisionsat very high energies can produce small short-lived regions of space whose energy density is comparable to that of the20-micro-second-old universe.This has been achieved by colliding heavy nuclei such asleadnuclei at high speeds, and a first time claim of formation ofquark–gluon plasmacame from theSPSaccelerator atCERNin February 2000.[13]

This work has been continued at more powerful accelerators, such as RHIC in the US, and as of 2010 at the European LHC at CERN located in the border area of Switzerland and France. There is good evidence that the quark–gluon plasma has also been produced at RHIC.[14]

Thermodynamics

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The context for understanding the thermodynamics of quark matter is thestandard modelof particle physics, which contains six differentflavorsof quarks, as well asleptonslikeelectronsandneutrinos.These interact via thestrong interaction,electromagnetism,and also theweak interactionwhich allows one flavor of quark to turn into another. Electromagnetic interactions occur between particles that carry electrical charge; strong interactions occur between particles that carrycolor charge.

The correct thermodynamic treatment of quark matter depends on the physical context. For large quantities that exist for long periods of time (the "thermodynamic limit" ), we must take into account the fact that the only conserved charges in the standard model are quark number (equivalent tobaryonnumber), electric charge, the eight color charges, and lepton number. Each of these can have an associated chemical potential. However, large volumes of matter must be electrically and color-neutral, which determines the electric and color charge chemical potentials. This leaves a three-dimensionalphase space,parameterized by quark chemical potential, lepton chemical potential, and temperature.

In compact stars quark matter would occupy cubic kilometers and exist for millions of years, so the thermodynamic limit is appropriate. However, the neutrinos escape, violating lepton number, so the phase space for quark matter in compact stars only has two dimensions, temperature (T) and quark number chemical potential μ. Astrangeletis not in the thermodynamic limit of large volume, so it is like an exotic nucleus: it may carry electric charge.

A heavy-ion collision is in neither the thermodynamic limit of large volumes nor long times. Putting aside questions of whether it is sufficiently equilibrated for thermodynamics to be applicable, there is certainly not enough time for weak interactions to occur, so flavor is conserved, and there are independent chemical potentials for all six quark flavors. The initial conditions (theimpact parameterof the collision, the number of up and down quarks in the colliding nuclei, and the fact that they contain no quarks of other flavors) determine the chemical potentials. (Reference for this section:[15][16]).

Phase diagram

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Conjectured form of the phase diagram of QCD matter, with temperature on the vertical axis and quarkchemical potentialon the horizontal axis, both in mega-electron volts.[15]

Thephase diagramof quark matter is not well known, either experimentally or theoretically. A commonly conjectured form of the phase diagram is shown in the figure to the right.[15]It is applicable to matter in a compact star, where the only relevant thermodynamic potentials are quarkchemical potentialμ andtemperatureT.

For guidance it also shows the typical values of μ andTin heavy-ion collisions and in the early universe. For readers who are not familiar with the concept of a chemical potential, it is helpful to think of μ as a measure of the imbalance between quarks and antiquarks in the system. Higher μ means a stronger bias favoring quarks over antiquarks. At low temperatures there are no antiquarks, and then higher μ generally means a higher density of quarks.

Ordinary atomic matter as we know it is really a mixed phase, droplets of nuclear matter (nuclei) surrounded by vacuum, which exists at the low-temperature phase boundary between vacuum and nuclear matter, at μ = 310 MeV andTclose to zero. If we increase the quark density (i.e. increase μ) keeping the temperature low, we move into a phase of more and more compressed nuclear matter. Following this path corresponds to burrowing more and more deeply into aneutron star.

Eventually, at an unknown critical value of μ, there is a transition to quark matter. At ultra-high densities we expect to find thecolor-flavor-locked(CFL) phase ofcolor-superconductingquark matter. At intermediate densities we expect some other phases (labelled "non-CFL quark liquid" in the figure) whose nature is presently unknown.[15][16]They might be other forms of color-superconducting quark matter, or something different.

Now, imagine starting at the bottom left corner of the phase diagram, in the vacuum where μ =T= 0. If we heat up the system without introducing any preference for quarks over antiquarks, this corresponds to moving vertically upwards along theTaxis. At first, quarks are still confined and we create a gas of hadrons (pions,mostly). Then aroundT= 150 MeV there is a crossover to the quark gluon plasma: thermal fluctuations break up the pions, and we find a gas of quarks, antiquarks, and gluons, as well as lighter particles such as photons, electrons, positrons, etc. Following this path corresponds to travelling far back in time (so to say), to the state of the universe shortly after the big bang (where there was a very tiny preference for quarks over antiquarks).

The line that rises up from the nuclear/quark matter transition and then bends back towards theTaxis, with its end marked by a star, is the conjectured boundary between confined and unconfined phases. Until recently it was also believed to be a boundary between phases where chiral symmetry is broken (low temperature and density) and phases where it is unbroken (high temperature and density). It is now known that the CFL phase exhibits chiral symmetry breaking, and other quark matter phases may also break chiral symmetry, so it is not clear whether this is really a chiral transition line. The line ends at the "chiralcritical point",marked by a star in this figure, which is a special temperature and density at which striking physical phenomena, analogous tocritical opalescence,are expected. (Reference for this section:[15][16][17]).

For a complete description of phase diagram it is required that one must have complete understanding of dense, strongly interacting hadronic matter and strongly interacting quark matter from some underlying theory e.g. quantum chromodynamics (QCD). However, because such a description requires the proper understanding of QCD in its non-perturbative regime, which is still far from being completely understood, any theoretical advance remains very challenging.

Theoretical challenges: calculation techniques

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The phase structure of quark matter remains mostly conjectural because it is difficult to perform calculations predicting the properties of quark matter. The reason is that QCD, the theory describing the dominant interaction between quarks, is strongly coupled at the densities and temperatures of greatest physical interest, and hence it is very hard to obtain any predictions from it. Here are brief descriptions of some of the standard approaches.

Lattice gauge theory

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The only first-principles calculational tool currently available islattice QCD,i.e. brute-force computer calculations. Because of a technical obstacle known as the fermionsign problem,this method can only be used at low density and high temperature (μ <T), and it predicts that the crossover to the quark–gluon plasma will occur aroundT= 150 MeV[18]However, it cannot be used to investigate the interesting color-superconducting phase structure at high density and low temperature.[19]

Weak coupling theory

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Because QCD isasymptotically freeit becomes weakly coupled at unrealistically high densities, and diagrammatic methods can be used.[16]Such methods show that the CFL phase occurs at very high density. At high temperatures, however, diagrammatic methods are still not under full control.

Models

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To obtain a rough idea of what phases might occur, one can use a model that has some of the same properties as QCD, but is easier to manipulate. Many physicists useNambu–Jona-Lasinio models,which contain no gluons, and replace the strong interaction with afour-fermion interaction.Mean-field methods are commonly used to analyse the phases. Another approach is thebag model,in which the effects of confinement are simulated by an additive energy density that penalizes unconfined quark matter.

Effective theories

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Many physicists simply give up on a microscopic approach, and make informed guesses of the expected phases (perhaps based on NJL model results). For each phase, they then write down an effective theory for the low-energy excitations, in terms of a small number of parameters, and use it to make predictions that could allow those parameters to be fixed by experimental observations.[17]

Other approaches

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Main article:AdS/QCD

There are other methods that are sometimes used to shed light on QCD, but for various reasons have not yet yielded useful results in studying quark matter.

1/N expansion

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Treat the number of colorsN,which is actually 3, as a large number, and expand in powers of 1/N.It turns out that at high density the higher-order corrections are large, and the expansion gives misleading results.[15]

Supersymmetry

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Adding scalar quarks (squarks) and fermionic gluons (gluinos) to the theory makes it more tractable, but the thermodynamics of quark matter depends crucially on the fact that only fermions can carry quark number, and on the number of degrees of freedom in general.

Experimental challenges

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Experimentally, it is hard to map the phase diagram of quark matter because it has been rather difficult to learn how to tune to high enough temperatures and density in the laboratory experiment using collisions of relativistic heavy ions as experimental tools. However, these collisions ultimately will provide information about the crossover fromhadronic matterto QGP. It has been suggested that the observations of compact stars may also constrain the information about the high-density low-temperature region. Models of the cooling, spin-down, and precession of these stars offer information about the relevant properties of their interior. As observations become more precise, physicists hope to learn more.[15]

One of the natural subjects for future research is the search for the exact location of the chiral critical point. Some ambitious lattice QCD calculations may have found evidence for it, and future calculations will clarify the situation. Heavy-ion collisions might be able to measure its position experimentally, but this will require scanning across a range of values of μ and T.[20]

Evidence

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In 2020, evidence was provided that the cores of neutron stars with mass ~2M⊙were likely composed of quark matter.[7][21]Their result was based on neutron-startidal deformabilityduring aneutron star mergeras measured bygravitational-wave observatories,leading to an estimate of star radius, combined with calculations of the equation of state relating the pressure and energy density of the star's core. The evidence was strongly suggestive but did not conclusively prove the existence of quark matter.

See also

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Sources and further reading

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  • Aronson, S. and Ludlam, T.:"Hunting the quark gluon plasma",U.S. Dept. of Energy (2005)
  • Letessier, Jean:Hadrons and quark-gluon plasma,Cambridge monographs on particle physics, nuclear physics, and cosmology (Vol. 18), Cambridge University Press (2002)
  • S. Hands (2001). "The phase diagram of QCD".Contemporary Physics.42(4): 209–225.arXiv:physics/0105022.Bibcode:2001ConPh..42..209H.doi:10.1080/00107510110063843.S2CID16835076.
  • K. Rajagopal (2001)."Free the quarks"(PDF).Beam Line.32(2): 9–15.

References

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  1. ^Letessier, Jean; Rafelski, Johann (2002).Hadrons and Quark–Gluon Plasma(1 ed.). Cambridge University Press.doi:10.1017/cbo9780511534997.ISBN978-0-521-38536-7.
  2. ^"Quark Matter 2021: The 29th International Conference on Ultrarelativistic Nucleus-Nucleus Collisions".Indico.Retrieved2020-06-26.
  3. ^"CPOD2020 - International Conference on Critical Point and Onset of Deconfinement".Indico.4 May 2020.Retrieved2020-06-26.
  4. ^"Strangeness in Quark Matter 2019".Indico.9 June 2019.Retrieved2020-06-26.
  5. ^See"Hadrons and quark-gluon plasma"for example.
  6. ^Shapiro and Teukolsky:Black Holes, White Dwarfs and Neutron Stars: The Physics of Compact Objects,Wiley 2008
  7. ^abAnnala, Eemeli; Gorda, Tyler; Kurkela, Aleksi; Nättilä, Joonas; Vuorinen, Aleksi (2020-06-01)."Evidence for quark-matter cores in massive neutron stars".Nature Physics.16(9): 907–910.arXiv:1903.09121.Bibcode:2020NatPh..16..907A.doi:10.1038/s41567-020-0914-9.ISSN1745-2481.
  8. ^Biswas, Sayan; et al. (2016)."A production scenario of Galactic strangelets and an estimation of their possible flux in solar neighborhood".Proceedings: A production scenario of Galactic strangelets and an estimation of their possible flux in solar neighborhood.Vol. ICRC2015. inSpire. p. 504.doi:10.22323/1.236.0504.Retrieved11 October2016.
  9. ^Madsen, Jes (18 November 2004). "Strangelet propagation and cosmic ray flux".Phys. Rev. D.71(1): 014026.arXiv:astro-ph/0411538.Bibcode:2005PhRvD..71a4026M.doi:10.1103/PhysRevD.71.014026.S2CID119485839.
  10. ^Holdom, Bob; Ren, Jing; Zhang, Chen (31 May 2018). "Quark Matter May Not Be Strange".Physical Review Letters.120(22): 222001.arXiv:1707.06610.Bibcode:2018PhRvL.120v2001H.doi:10.1103/PhysRevLett.120.222001.PMID29906186.S2CID49216916.
  11. ^"ALICE".CERN.Retrieved16 December2015.
  12. ^See"Hunting the quark gluoan plasma"as an example of the research at RHIC.
  13. ^Heinz, Ulrich; Jacob, Maurice (2000). "Evidence for a New State of Matter: An Assessment of the Results from the CERN Lead Beam Programme".arXiv:nucl-th/0002042.
  14. ^Heinz, Ulrich; Jacob, Maurice (2005). "Quark Matter 2005 – Theoretical Summary".arXiv:nucl-th/0508062.
  15. ^abcdefgAlford, Mark G.; Schmitt, Andreas; Rajagopal, Krishna; Schäfer, Thomas (2008). "Color superconductivity in dense quark matter".Reviews of Modern Physics.80(4): 1455–1515.arXiv:0709.4635.Bibcode:2008RvMP...80.1455A.doi:10.1103/RevModPhys.80.1455.S2CID14117263.
  16. ^abcdRischke, D (2004). "The quark–gluon plasma in equilibrium".Progress in Particle and Nuclear Physics.52(1): 197–296.arXiv:nucl-th/0305030.Bibcode:2004PrPNP..52..197R.CiteSeerX10.1.1.265.4175.doi:10.1016/j.ppnp.2003.09.002.S2CID119081533.
  17. ^ab T. Schäfer (2004). "Quark matter". In A. B. Santra (ed.).Mesons and Quarks.14th National Nuclear Physics Summer School. Alpha Science International.arXiv:hep-ph/0304281.Bibcode:2003hep.ph....4281S.ISBN978-81-7319-589-1.
  18. ^P. Petreczky (2012). "Lattice QCD at non-zero temperature".J. Phys. G.39(9): 093002.arXiv:1203.5320.Bibcode:2012JPhG...39i3002P.doi:10.1088/0954-3899/39/9/093002.S2CID119193093.
  19. ^Christian Schmidt (2006)."Lattice QCD at Finite Density".PoS LAT2006.2006(21): 021.arXiv:hep-lat/0610116.Bibcode:2006slft.confE..21S.doi:10.22323/1.032.0021.S2CID14890549.
  20. ^Rajagopal, K (1999). "Mapping the QCD phase diagram".Nuclear Physics A.661(1–4): 150–161.arXiv:hep-ph/9908360.Bibcode:1999NuPhA.661..150R.doi:10.1016/S0375-9474(99)85017-9.S2CID15893165.
  21. ^"A new type of matter discovered inside neutron stars".ScienceDaily.Retrieved2020-06-01.
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