The discovery of huge magnetic fields in the vicinity of white dwarf stars (B ≈ 102–105 T) (Kemp et al. 1970; Angel 1978; Angel et al. 1981) and neutron stars (B ≈ 107–109 T) (Trümper et al. 1977; Trümper et al. 1978) has opened the possibility of studying the properties of matter under conditions which can never be realized in terrestrial laboratories. (Rapidly time-variable magnetic fields over nuclear dimensions with peak values up to B ≈ 1011 T are assumed to occur in heavy-ion collisions, cf. Rafelski and Müller 1976). White dwarf stars and neutron stars represent final stages of stellar evolution. Neutron stars are formed from normal stars in a dramatic cosmic event, when the star has consumed its nuclear energy supply and becomes unstable against its own gravitational forces. The catastrophic collapse to a neutron star is usually accompanied by a supernova explosion, in which the star becomes almost as bright as a whole galaxy consisting of a hundred billion suns. Typical values of relevant physical parameters are listed in Table 1.1 in comparison with our sun.
KeywordsNeutron Star Magnetic Field Strength Accretion Disk Strong Magnetic Field White Dwarf
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