Ritam Mallick

Deformation of a magnetized neutron star

Magnetars are compact stars which are observationally determined to have very strong surface magnetic fields of the order of

Maximum mass of a hybrid star having a mixed-phase region based on constraints set by the pulsar PSR J1614-2230

10^{14}-10^{15}

Nonequilibrium phase transition in compact stars through a violent shock

G. The centre of the star can potentially have a magnetic field several orders of magnitude larger. We study the effect of the field on the mass and shape of such a star. In general, we assume a non-uniform magnetic field inside the star which varies with density. The magnetic energy and pressure as well as the metric are expanded as multipoles in spherical harmonics up to the quadrupole term. Solving the Einstein equations for the gravitational potential, one obtains the correction terms as functions of the magnetic field. Using a nonlinear model for the hadronic EoS the excess mass and change in equatorial radius of the star due to the magnetic field are quite significant if the surface field is

On the possibility of rho-meson condensation in neutron stars

10^{15}

GENERAL RELATIVISTIC EFFECT ON THE ENERGY DEPOSITION RATE FOR NEUTRINO PAIR ANNIHILATION ABOVE THE EQUATORIAL PLANE ALONG THE SYMMETRY AXIS NEAR A ROTATING NEUTRON STAR

G and the central field is about

Possible conversion of a neutron star to a quark star in the presence of high magnetic field: Neutron star-quark star conversion

10^{18}

Effect of magnetic field on the burning of a neutron star

G. For a value of the central magnetic field strength of

Oblique magnetohydrodynamic shocks: Space-like and time-like characteristics

1.75\times10^{18}

Oblique MHD shocks: space-like and time-like

G, we find that both the excess mass and the equatorial radius of the star changes by about

Taub adiabat: a tool to study astrophysical phase transition

3-4\%