Publisher’s Note: Ideal relativistic fluid limit for a medium with polarization [Phys. Rev. D 
<b>96</b>
, 056012 (2017)]

Montenegro, David; Tinti, Leonardo; Torrieri, Giorgio

doi:10.1103/physrevd.96.079901

Cited by 60 publications

(64 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It is understood in the choice of the operator (26) that the spin density appears among densities which "slowly" evolve towards global equilibrium, just like a conserved charge density or energy density. The dissipative, entropy-increasing processes must drive the system to global equilibrium, hence (at least for systems with nonsymmetric stress-energy tensor) the spin potential Ω should converge to the thermal vorticity (see [26] for a similar discussion). Yet, this process may be slow enough so that the spin relaxation takes place on the same time scale as the typical dissipative hydrodynamic process.…”

Section: A Discussionmentioning

confidence: 99%

“…where ̟ is the thermal vorticity. Consequently, the local thermodynamic equilibrium operator (26), hence (27), is equivalent to that built directly from Belinfante's tensor, see Eq. (10) if the following conditions are met:…”

Section: Local Equilibrium Density Operatormentioning

confidence: 99%

“…where the LE subscripts stands for the mean value with the density operator (26). This vector is, however, not uniquely defined as it is possible to add vectors orthogonal to n µ to obtain the same total entropy.…”

Section: Local Equilibrium Density Operatormentioning

confidence: 99%

“…At the lowest order of approximations, the constitutive relations are obtained by calculating the mean values with the local equilibrium density operator (26). Dissipative corrections depending on gradients of β and Ω can be calculated with the same method outlined when discussing Eqs.…”

Section: B Relativistic Hydrodynamics With Spin Tensormentioning

confidence: 99%

See 3 more Smart Citations

Spin tensor and its role in non-equilibrium thermodynamics

2019

View full text Add to dashboard Cite

It is shown that the description of a relativistic fluid at local thermodynamic equilibrium depends on the particular quantum stress-energy tensor operator chosen, e.g., the canonical or symmetrized Belinfante stress-energy tensor. We argue that the Belinfante tensor is not appropriate to describe a relativistic fluid whose macroscopic polarization relaxes slowly to thermodynamic equilibrium and that a spin tensor, like the canonical spin tensor, is required. As a consequence, the description of a polarized relativistic fluid involves an extension of relativistic hydrodynamics including a new antisymmetric rank-two tensor as a dynamical field. We show that the canonical and Belinfante tensors lead to different predictions for measurable quantities such as spectrum and polarization of particles produced in relativistic heavy-ion collisions.

show abstract

Section: A Discussionmentioning

confidence: 99%

Section: Local Equilibrium Density Operatormentioning

confidence: 99%

Section: Local Equilibrium Density Operatormentioning

confidence: 99%

Section: B Relativistic Hydrodynamics With Spin Tensormentioning

confidence: 99%

See 2 more Smart Citations

Spin tensor and its role in non-equilibrium thermodynamics

2019

View full text Add to dashboard Cite

show abstract

“…(12) does not hold in general. One expects that the relation (12) is a consequence of a dissipative spin-orbit interaction, which is so far missing in our framework [22]. The spin-orbit interaction should lead also to asymmetric energy-momentum tensor [23].…”

Section: Spin Dynamicsmentioning

confidence: 99%

Relativistic hydrodynamics with spin

et al. 2019

View full text Add to dashboard Cite

A newly proposed framework of perfect-fluid relativistic hydrodynamics for particles with spin 1 /2 is briefly reviewed. The hydrodynamic equations follow entirely from the conservation laws for energy, momentum, and angular momentum. The incorporation of the angular-momentum conservation requires that the spin polarization tensor ω µν is introduced. It plays a role of a Lagrange multiplier conjugated to the spin tensor S λ, µν . The space-time evolution of the spin polarization tensor depends on the specific form chosen for the spin tensor.

show abstract