Thermodynamic behavior of non-strange baryonic matter

Garpman, S.; Glendenning, Norman K.; Karant, Yasha J.

doi:10.1016/0375-9474(79)90433-0

Cited by 70 publications

(39 citation statements)

References 11 publications

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“…However, as noticed previously [3], there is a region in which three solutions exist at the same density. On the isotherms shown in Fig.…”

Section: High Temperature Propertiesmentioning

confidence: 73%

“…Being a non-linear theory in the field amplitudes, it has the possibility of possessing additional solutions to the normal state, that correspond to different field configurations [2]. In earlier work [3,4,5,6,7], a second solution was found at high temperature that is characterized by a low baryon effective mass and a high density of baryon-antibaryon pairs. Here we point out that under certain conditions there exists a temperature range over which matter in this abnormal phase can have zero pressure.…”

Section: Introductionmentioning

confidence: 99%

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Finite temperature metastable matter

Glendenning

1987

Physics Letters B

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LBL-22287Relativistic nuclear field theory possesses a solution corresponding to a hot metastable object of abnormal matter that cools by black-body radiation until a critical point is reached at which it becomes unstable, and would disassemble. IT produced in a high energy nuclear collision, a large part of the initial energy of the object is emitted in black-body radiation, so that the nuclear fragments produced in its ultimate decay would account for only a fraction of the collision energy.

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“…However, as noticed previously [3], there is a region in which three solutions exist at the same density. On the isotherms shown in Fig.…”

Section: High Temperature Propertiesmentioning

confidence: 73%

Section: Introductionmentioning

confidence: 99%

Finite temperature metastable matter

Glendenning

1987

Physics Letters B

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“…The baryon eigenvalues of momentum, k, for particle and antiparticle are, (5) (6) (7) (8) For the present application we need the finite temperature solutions. The formulation has been carried out earlier [8,9].…”

Section: · Interacting Hadron Equation Of Statementioning

confidence: 99%

“…With appropriate extensions, the theory can be used to study matter away from the normal state, matter that is under extreme conditions of temperature or density, such as is expected to be produced in relativistic nuclear collisions, and as formed in the collapse of a star just prior to the bounce that produces the supernova, and as exists in the cores of the neutron stars into which the remaining matter of the star subsides. We have studied some aspects of these problems in other papers, and refer to them for the formulation of the theory appropriate to the present application [8,9]. The new feature that we need here is the conservation of strangeness, because the time scale of nuclear collisions is so short compared to the weak interaction scale that violates strangeness conservation.…”

Section: Introductionmentioning

confidence: 99%

“…On the quark side the principle uncertainty is the bag constant and the effect of interactions due to gluon exchange. Therefore J{, B and a 8 will be the main focus as concerns uncertainties in the equation of state. We shall also investigate the role played by baryon resonances and shall include the pion polarization in the medium through the excitation of delta particle -nucleon hole excitations and the correlations introduced by the short range nuclear force.…”

Section: Introductionmentioning

confidence: 99%

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Hadron to quark—gluon phase transition in the baryon-rich domain

GLENDENNING

1990

Nuclear Physics A

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The hadron to quark-gluon phase transition is studied in charge symmetric matter. Nuclear field theory describes the hadronic phase, including baryon resonances and thermal pions and kaons. The pion dispersion in medium is computed. The other phase is described as a gas of massless u and d quarks and gluons and massive s quarks, with or without gluon exchange .. The RankineHugoniot relation is employed to estimate the initial properties of matter produced in nuclear collisions as a function of energy. It is found that signals depending on pressure or entropy are poor ones and that the most dramatic differences between the hadronic phase and mixed phase occur in the temperature and density. Di-lepton and photon signals ought therefore to be good ones. It is shown that the analogy of "melting" of hadrons in the plasma is incorrect as concerns formation of a plasma in nuclear collisions in contrast to the adiabatic heating of matter. Neither the phase diagram nor the properties of matter on the shock trajectory depend very much on the nuclear equation of state within the uncertainties with which it can be defined in terms of conventional nuclear saturation properties, because the thermal energy dominates over these. The main dependances are on the hadron spectrum, the pion dispersion in medium, the bag constant and the QCD coupling constant. Within accepted uncertainties in the nuclear and plasma equations of state, the mixed · phase could be formed in collisions with laboratory kinetic energy as low as 2.5 GeV.PACS 21.65+£, 25.70.Np, 0570.Fh tThis work was supported by the

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Neutron Stars, Fast Pulsars, Supernovae and the Equation of State of Dense Matter

Glendenning

1989

The Nuclear Equation of State

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We discuss the prospects for obtaining constraints on the equation of state from astrophysical sources. Neutron star masses although few are known at present, provide a very direct constraint in as much as the connection to the equation of state involves only the assumption that Einstein's general theory of relativity is correct at the macroscopic scale. If the millisecond pulses briefly observed in the remnant of SN1987 A can be attributed to uniform rotation of a. pulsar, then a. very severe constrajnt is placed on the equation of state. The theory again is very secure. The precise nature of the constraint is not yet understood, but it appears that the equation of state must be neither too soft nor stiff, and it may be that there is information not only on the stiffness of the equation of state but on its shape. Supernovae simulations involve such a plethora. of physical processes including those involved in the evolution of the precollapse configuration, not all of them known or understood, that they provide no constrajnt at the present time. Not even the broad category of mechanism for the explosion is agreed upon (prompt shock, delayed shock, or nuclear explosion). In connection with very fast pulsars, we include some speculations on pure quark matter stars, and on possible scenarios for understanding the disappearance of the fast pulsar in SN1987 A .

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Thermodynamic behavior of non-strange baryonic matter

Cited by 70 publications

References 11 publications

Finite temperature metastable matter

Finite temperature metastable matter

Hadron to quark—gluon phase transition in the baryon-rich domain

Neutron Stars, Fast Pulsars, Supernovae and the Equation of State of Dense Matter

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