Supernovae, Neutron Star Physics and Nucleosynthesis by Debades Bandyopadhyay & Kamales Kar

Author:Debades Bandyopadhyay & Kamales Kar
Language: eng
Format: epub
ISBN: 9783030951719
Publisher: Springer International Publishing

Fig. 3.10Quadrupole moment of rotating neutron star at 100 Hz is shown as a function of mass for different EoSs. This is taken from Ref. [238] and reproduced with kind permission of the European Physical Journal

3.9 Neutron Star Matter in Strongly Quantizing Magnetic Fields

Pulsars with strong surface magnetic fields ∼1012 G are normally found to exist in nature. However, it was observed that soft gamma-ray repeaters (SGRs) and anomalous x-ray pulsars (AXPs) had even stronger surface magnetic fields ≥1015 G [246, 247]. These SGRs and AXPs are believed to be the best candidates for a new class of neutron stars with very intense magnetic fields and are known as magnetars [248, 249]. It is inferred from the virial theorem that the interior magnetic field could be much higher than the surface field [250]. For a typical neutron star of mass 1.5 M⊙ and radius 15 km, the interior field could be as high as ∼1018 G. Such strong fields would quantize the motion of charged particles in the neutron star interior. Relativistic effects are important when the cyclotron energy of the charged particle is equal to its rest mass. This leads to the critical field of electrons G and that for protons G. In this section, we discuss the influence of strongly quantizing magnetic fields on the neutron star matter in the crust and the core.

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