Radial oscillations of neutron stars in strong magnetic fields

The eigen frequencies of radial pulsations of neutron stars are calculated in a strong magnetic field. At low densities we use the magnetic BPS equation of state (EOS) similar to that obtained by Lai and Shapiro while at high densities the EOS obtained from the relativistic nuclear mean field theory...

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Bibliographic Details
Published in:Pramāṇa 2002-09, Vol.59 (3), p.433-443
Main Authors: Gupta, VK, Tuli, Vinita, Singh, S, Anand, JD, Goyal, Ashok
Format: Article
Language:English
Subjects:
Equations of state
Mean field theory
Neutron stars
Relativistic theory
Resonant frequencies
Stellar magnetic fields
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Summary:The eigen frequencies of radial pulsations of neutron stars are calculated in a strong magnetic field. At low densities we use the magnetic BPS equation of state (EOS) similar to that obtained by Lai and Shapiro while at high densities the EOS obtained from the relativistic nuclear mean field theory is taken and extended to include strong magnetic field. It is found that magnetized neutron stars support higher maximum mass whereas the effect of magnetic field on radial stability for observed neutron star masses is minimal.
ISSN:0304-4289
0973-7111
DOI:10.1007/s12043-002-0041-4