Astronomy and Astrophysics – Astrophysics
Scientific paper
Oct 1988
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...205..335s&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 205, no. 1-2, Oct. 1988, p. 335-346. Research supported by the Max-Planck-Inst
Astronomy and Astrophysics
Astrophysics
13
Conductive Heat Transfer, Magnetic Field Configurations, Neutron Stars, Stellar Magnetic Fields, Electron Plasma, Magnetic Stars, Relativistic Plasmas, Transport Theory
Scientific paper
The author presents heat conduction coefficients longitudinal and transverse to a quantizing magnetic field of strength B = 1011, 1012 and 1013G. The coefficients describe the heat conduction behaviour of a relativistic electron gas in the state of partial degeneracy (T ≠ 0). The electron gas may coexist with a solid or liquid ion matter of any degree of ionisation. The conduction coefficients are easy to handle since they are calculated as analytic expressions. Their validity is restricted to densities in the range of 10-2 ≤ ρ/(g cm-3) ≤ 1011. This density regime covers the outer part of neutron stars where non-isotropic two-dimensional heat flow phenomena occur.
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