Bulletin of the Astronomical Society of India
Debades Bandyopadhyay*
Astroparticle Physics and Cosmology Division, Saha Institute of Nuclear Physics,
1/AF Bidhannagar, Kolkata-700064, India
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Recently neutron star masses have been estimated to very high degree
of accuracy. The accurately measured highest neutron star mass is
2.01±0.04M⊙. This puts a strong constraint on the β-equilibrated equation
of state (EoS) for neutron stars. Observed neutron star masses are also direct
probes of compositions of dense matter. Novel phases of matter such
as hyperons, Bose-Einstein condensates of (anti)-kaons and quarks might
exist in neutron star interior. The theoretical mass-radius relationship of
neutron stars including exotic forms of matter is calculated and it is shown
to be compatible with massive neutron stars. Unlike neutron star masses,
measurements of their radii are not accurate. The moments of inertia of
pulsars could be used as a tool for the determination of neutron star radii.
On the other hand, the compositions and EoS of magnetized neutron
star crusts might be probed using asteroseismology. The role of magnetized
crusts on quasi periodic oscillations (QPOs) in giant flares of magnetars
identified as torsional shear modes is discussed in this article.
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Keywords : equation of state - magnetic fields - stars:neutron