The Bhatia – Hazarika Limit for Magnetized Rotating Neutron Stars with viscosity and collisional effect

A B RAJIB HAZARIKA

doi:10.36948/ijfmr.2025.v07i06.63578

The Bhatia – Hazarika Limit for Magnetized Rotating Neutron Stars with viscosity and collisional effect

Author(s)	Dr. A B RAJIB HAZARIKA
Country	India
Abstract	The Tolman–Oppenheimer–Volkoff (TOV) limit represents the maximum mass a non-rotating, cold neutron star can sustain against gravitational collapse. However, in realistic astrophysical environments, neutron stars often possess intense magnetic fields (up to 10^15 G) and rapid rotation (up to millisecond periods), both of which significantly modifies the equilibrium structure and stability conditions. This paper is presented with the TOV limit by incorporating magnetic pressure, rotational effect with viscosity and collisional effect, and general relativistic corrections, aiming to estimate the upper mass threshold of a magnetized rotating neutron star (MRS). We derive the modified hydrostatic equilibrium equations; discuss numerical models based on General Relativity Magneto Hydro Dynamics (GRMHD), Navier-Stoke equation (for stress tensor consisting of bulk viscosity (collision effect) and shear viscosity) and present scaling relations between rotation rate, magnetic field strength, and the effective TOV mass. Recently GW170817 gravitational wave observed on 17 August 2017,the merger of two neutrons resulting into increased mass of 2.82 M☉[15] as reported is in complimenting results of Bhatia Hazarika limit (2.82 M☉ ) .Which definitely occurs due to collision of two neutron stars and also some effect shear viscosity is there .So our new model shows results in compliment with the observed data and Bhatia Hazarika Limit .The results suggest that the combined effects of rotation and magnetic field along with viscosity and collision support can increase the canonical TOV limit (~2.1 M☉) by up to 20–30% as Bhatia-Hazarika limit (~2.82 M☉) as observed [14] depending on field topology and equation of state (EOS).
Keywords	Neutron stars, stellar stability, general relativity, rotation, magnetic field, viscosity, collision, pulsar, gravitational wave.
Field	Mathematics > Maths + Physics
Published In	Volume 7, Issue 6, November-December 2025
Published On	2025-12-17
DOI	https://doi.org/10.36948/ijfmr.2025.v07i06.63578

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The Bhatia – Hazarika Limit for Magnetized Rotating Neutron Stars with viscosity and collisional effect

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