Condensed matter in a very strong magnetic field, at high pressure and zero temperature

Details Condensed matter in a very strong magnetic field, at high pressure and zero temperature Condensed matter in a very strong magnetic field, at high pressure and zero temperature

Mar 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976ncimb..32..177c&link_type=abstract

Nuovo Cimento, Sezione B, vol. 32B, Mar. 11, 1976, p. 177-194.

Physics

Atomic Physics

9

Atomic Physics, High Pressure, Magnetic Flux, Pulsars, Stellar Models, Astronomical Models, Condensed Matter Physics, Density (Mass/Volume), Equations Of State, Fermions, Mathematical Models, Neutron Stars, Pressure Effects, Statistical Analysis, Virial Theorem

Scientific paper

A statistical model describing condensed matter under conditions found at pulsar surfaces is developed on the assumptions that a very strong magnetic field is present, the motion of electrons perpendicular to the magnetic field is determined by that field alone, only the lowest magnetic level contributes to this motion, and the electrons may be treated locally as free fermions. The differential formulation of this model is reviewed and used to derive the equations of state for the condensed matter. Numerical results are given for a large range of atomic numbers, magnetic-field intensities, and a dimensionless parameter proportional to the cube root of density. It is shown that since the statistical model does not take account of cohesion forces within the condensed matter, it cannot predict the off-diagonal elements of the stress tensor or the arbitrary Lame coefficients, thus excluding its application to shear deformations. Possible applications to the outer crust of magnetic neutron stars are briefly noted.

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