Statistics – Computation
Scientific paper
Apr 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.219..703u&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 219, April 15, 1986, p. 703-717.
Statistics
Computation
62
Computational Astrophysics, Neutron Stars, Stellar Evolution, Stellar Magnetic Fields, Thermomagnetic Effects, Heat Transfer, Magnetic Field Configurations, Stellar Cores, Stellar Envelopes, Stellar Temperature, Toroidal Plasmas
Scientific paper
A linear stage of the magnetic field generation in outer (rho of less than about 10 to the 11th g/cu cm) layers of rather hot rotating neutron stars by thermomagnetic phenomena which accompany the heat transport from the stellar core is considered. For a neutron star with surface gravity of 10 to the 14th cm/second-squared whose envelope consists of degenerate electrons and Fe-56 ions in the fluid phase, the thermomagnetic instability is developed at surface temperatures, T(e), of more than about 3 million K and rotation periods of less than about 1 s. Axially-symmetric toroidal modes of magnetic field are unstable. In particular, at T(e) of 5 million K, the maximal instability increment equals 1/70 d and corresponds to the magnetic configuration with wavelength of about 80 m in the meridional direction and maximal field at a depth of about 40 m. At this T(e) the magnetic field modes with wavelengths of between about 30 m to 1 km are generated. If T(e) falls down to 3 million K due to the neutron star cooling, the instability increment decreases to zero, while the spectrum of wavelengths tightens to about 120 m. It is possible that at the nonlinear stage the proposed mechanism leads to the generation of strong magnetic fields of about 10 to the 10th to 10 to the 13th G present in the surface layers of neutron stars.
Iakovlev D. G.
Levshakov Sergei A.
Urpin Vadim A.
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