## Magnetization of High Density Hadronic Fluid

Publication: Research - peer-review › Journal article – Annual report year: 2012

### Standard

**Magnetization of High Density Hadronic Fluid.** / Bohr, Henrik; Providencia, Constanca; da Providencia, João.

Publication: Research - peer-review › Journal article – Annual report year: 2012

### Harvard

*Brazilian Journal of Physics*, vol 42, no. 1-2, pp. 68-76., 10.1007/s13538-012-0060-7

### APA

*Brazilian Journal of Physics*,

*42*(1-2), 68-76. 10.1007/s13538-012-0060-7

### CBE

### MLA

*Brazilian Journal of Physics*. 2012, 42(1-2). 68-76. Available: 10.1007/s13538-012-0060-7

### Vancouver

### Author

### Bibtex

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### RIS

TY - JOUR

T1 - Magnetization of High Density Hadronic Fluid

A1 - Bohr,Henrik

A1 - Providencia,Constanca

A1 - da Providencia,João

AU - Bohr,Henrik

AU - Providencia,Constanca

AU - da Providencia,João

PB - Sociedade Brasileira de Fisica

PY - 2012

Y1 - 2012

N2 - In the present paper the magnetization of a high density relativistic fluid of elementary particles is studied. At very high densities, such as may be found in the interior of a neutron star, when the external magnetic field is gradually increased, the energy of the normal phase of the fluid remains practically constant before extremely high magnetic fields are reached. However, if pion condensation occurs, the energy decreases linearly while the magnetic field strength increases, so that a non vanishing magnetization, independent of the magnetic field, is present. The expression of the magnetization is derived by first considering and solving the Dirac equation of a fermion in interaction with a magnetic field and with a chiral sigma-pion pair. The solution provides the energies of single-particle states. The energy of the system is found by summing up contributions from all particles in the particle fluid. For nuclear densities above 2 to 3 rho(0), where rho(0) is the equilibrium nuclear density, the resulting magnetic field turns out to be rather huge, of the order of 10(17) Gauss.

AB - In the present paper the magnetization of a high density relativistic fluid of elementary particles is studied. At very high densities, such as may be found in the interior of a neutron star, when the external magnetic field is gradually increased, the energy of the normal phase of the fluid remains practically constant before extremely high magnetic fields are reached. However, if pion condensation occurs, the energy decreases linearly while the magnetic field strength increases, so that a non vanishing magnetization, independent of the magnetic field, is present. The expression of the magnetization is derived by first considering and solving the Dirac equation of a fermion in interaction with a magnetic field and with a chiral sigma-pion pair. The solution provides the energies of single-particle states. The energy of the system is found by summing up contributions from all particles in the particle fluid. For nuclear densities above 2 to 3 rho(0), where rho(0) is the equilibrium nuclear density, the resulting magnetic field turns out to be rather huge, of the order of 10(17) Gauss.

KW - Physics

KW - Gamma-ray bursts

KW - Pion-condensation

KW - Neutron matter

KW - Chiral model

KW - Fields

KW - Stars

U2 - 10.1007/s13538-012-0060-7

DO - 10.1007/s13538-012-0060-7

JO - Brazilian Journal of Physics

JF - Brazilian Journal of Physics

SN - 0103-9733

IS - 1-2

VL - 42

SP - 68

EP - 76

ER -