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Radial oscillations of neutron stars in strong magnetic fields

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Abstract

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.

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Authors and Affiliations

  1. Department of Physics and Astrophysics, University of Delhi, 110 007, Delhi, India

    VK Gupta, Vinita Tuli, S Singh, JD Anand & Ashok Goyal

  2. Inter University Centre for Astronomy and Astrophysics, 411 007, Ganeshkhind, Pune, India

    VK Gupta, Vinita Tuli, S Singh, JD Anand & Ashok Goyal

Authors
  1. VK Gupta
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  2. Vinita Tuli
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  3. S Singh
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  4. JD Anand
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  5. Ashok Goyal
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Gupta, V., Tuli, V., Singh, S. et al. Radial oscillations of neutron stars in strong magnetic fields. Pramana - J Phys 59, 433–443 (2002). https://doi.org/10.1007/s12043-002-0041-4

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  • DOI: https://doi.org/10.1007/s12043-002-0041-4

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