Three-body problem at finite temperature and density

Kvinikhidze, A. N.; Blankleider, B.

doi:10.1103/physrevc.72.054001

Cited by 3 publications

(4 citation statements)

References 28 publications

(51 reference statements)

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“…Therefore, we focus on the region where E 0 3 M  . We briefly note that similar in-medium three-body equations were employed in nuclear physics [80][81][82][83][84][85][86][87]. Figure 3 shows the ground-state trimer energy E 3 M with the medium effects, which can be obtained numerically from equation (11) as a dimensionless function…”

Section: In-medium Stm Equationmentioning

confidence: 99%

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Quantum chromodynamics (QCD)-like phase diagram with Efimov trimers and Cooper pairs in resonantly interacting SU(3) Fermi gases

Tajima

Naidon

2019

New J. Phys.

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We investigate color superfluidity and trimer formation in resonantly interacting SU(3) Fermi gases with a finite interaction range. The finite range is crucial to avoid the Thomas collapse and treat the Efimov effect occurring in this system. Using the Skorniakov-Ter-Martirosian equation with medium effects, we show the effects of the atomic Fermi distribution on the Efimov trimer energy at finite temperature. We show the critical temperature of color superfluidity within the many-body T-matrix approximation. In this way, we can provide a first insight into the phase diagram as a function of the temperature T and the chemical potential μ. This phase diagram consists of trimer, normal, and colorsuperfluid phases, and is similar to that of quantum chromodynamics at finite density and temperature.

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Section: In-medium Stm Equationmentioning

confidence: 99%

“…( 12) (see Appendix A) does not allow such solutions and we focus on the region where E M 3 ≤ 0. We briefly note that similar in-medium three-body equations were employed in nuclear physics [78][79][80][81][82][83][84][85].…”

Section: In-medium Skorniakov-ter-martirosian Equationmentioning

confidence: 99%

Quantum chromodynamics (QCD)-like phase diagram with Efimov trimers and Cooper pairs in resonantly interacting SU(3) Fermi gases

Tajima

Naidon

2019

New J. Phys.

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“…The counterparts of these equations in the many-body theory were first formulated by Bethe [70] to access the three-hole-line contributions to the nucleon self-energy and the binding of nuclear matter (Bethe's approach is discussed in Subsection 2.3). More recently, alternative forms of the three-body equations in a background medium have been developed that use either an alternative driving force (the particle-hole interaction or scattering T -matrix) [29,71,72,73] or/and adopt an alternative version of the free-space three-body equations, known as the Alt-Grassberger-Sandhas form [74,75,76]. The resummation series for three-body scattering amplitudes can be written down in terms of the three-body interaction V as [29] where G 0 and G are the free and full three-particle Green's functions (we use the operator form for notational simplicity; each operator, as in the two-particle case, is ordered on the contour).…”

Section: Three-body T -Matrix and Bound Statesmentioning

confidence: 99%

The physics of dense hadronic matter and compact stars

Sedrakian

2007

Progress in Particle and Nuclear Physics

125

109

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This review describes the properties of hadronic phases of dense matter in compact stars. The theory is developed within the method of real-time Green's functions and is applied to study of baryonic matter at and above the saturation density. The non-relativistic and covariant theories based on continuum Green's functions and the T -matrix and related approximations to the selfenergies are reviewed. The effects of symmetry energy, onset of hyperons and meson condensation on the properties of stellar configurations are demonstrated on specific examples. Neutrino interactions with baryonic matter are introduced within a kinetic theory. We concentrate on the classification, analysis and first principle derivation of neutrino radiation processes from unpaired and superfluid hadronic phases. We then demonstrate how neutrino radiation rates from various microscopic processes affect the macroscopic cooling of neutron stars and how the observed X-ray fluxes from pulsars constrain the properties of dense hadronic matter. Contents IntroductionNeutron stars are born in a gravitational collapse of luminous stars whose core mass exceeds the Chandrasekhar limit for a self-gravitating body supported by degeneracy pressure of electron gas [1]. Being the densest observable bodies in our universe they open a window on the physics of matter under extreme conditions of high densities, pressures and strong electromagnetic and gravitational fields. Most of the known pulsars are isolated objects which emit radio-waves at frequencies 10 8 − 10 10 Hz, which are pulsed at the rotation frequency of the star. Young objects, like the pulsar in the Crab nebula, are also observed through X-rays that are emitted from their surface as the star radiates away its thermal energy. Relativistic magnetospheres of young pulsars emit detectable non-thermal optical and gamma radiation; they could be sources of high-energy elementary particles. Neutron stars in the binaries are powered by the energy of matter accreted from companion star.The radio observations of pulsars stretch back to 1967 when the first pulsar was discovered. Since then, the observational pulsar astronomy has been extremely important to the fundamental physics and 2 astrophysics, which is evidenced by two Nobel awards, one for the discovery of pulsars (Hewish 1974) [2], the other for the discovery of the first neutron star -neutron star binary pulsar (Hulse and Taylor, 1993) [3] whose orbital decay confirmed the gravitational radiation in full agreement with Einstein's General Theory of Relativity. The measurements of neutron star (NS) masses in binaries provide one of the most stringent constraint on properties of the superdense matter. The timing observations of the millisecond pulsars set an upper limit on the angular momentum that can be accommodated by a stable NS -a limit that can potentially constrains the properties of dense matter. Noise and rotational anomalies that are superimposed on the otherwise highly stable rotation of these objects provide a clue to the ...

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“…In this approach, the Brueckner G-matrix is employed as the driving term in the three-body equations [20]. More recently, alternative forms of the three-body equations in a background medium have been developed that either (i) use an alternative driving force (the particle-hole interaction or scattering T -matrix) [21,22,23] or/and (ii) adopt an alternative version of the free-space threebody equations, known as the Alt-Grassberger-Sandhas form [24,25]. Our initial task will be to derive the homogeneous integral equations that determine the in-matter bound-state wave-function and the corresponding eigenstates using the real-time Green's functions formulation of the in-matter three-body equations [22].…”

Section: Introductionmentioning

confidence: 99%

Pair condensation and bound states in fermionic systems

Sedrakian

Clark

2006

Phys. Rev. C

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We study the finite temperature-density phase diagram of an attractive fermionic system that supports two-body (dimer) and three-body (trimer) bound states in free space. Using interactions characteristic for nuclear systems, we obtain the critical temperature Tc2 for the superfluid phase transition and the limiting temperature Tc3 for the extinction of trimers. The phase diagram features a Cooper-pair condensate in the high-density, low-temperature domain which, with decreasing density, crosses over to a Bose condensate of strongly bound dimers. The high-temperature, low-density domain is populated by trimers whose binding energy decreases toward the density-temperature domain occupied by the superfluid and vanishes at a critical temperature Tc3 > Tc2.

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Three-body problem at finite temperature and density

Abstract: We derive practical three-body equations for the equal-time three-body Green's function in matter. Our equations describe both bosons and fermions at finite density and temperature and take into account all possible two-body subprocesses allowed by the underlying Hamiltonian.

Cited by 3 publications

References 28 publications

Quantum chromodynamics (QCD)-like phase diagram with Efimov trimers and Cooper pairs in resonantly interacting SU(3) Fermi gases

Quantum chromodynamics (QCD)-like phase diagram with Efimov trimers and Cooper pairs in resonantly interacting SU(3) Fermi gases

The physics of dense hadronic matter and compact stars

Pair condensation and bound states in fermionic systems

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