Bhatia Hazarika Limit

In astrophysics, the Chandrasekhar Limit is the maximum mass of a stable white dwarf star, defined as 1.4 times the mass of the sun, before gravitational collapse occurs. However, when a neutron star escapes to become 2.8 times its solar mass, it reaches what is called its Bhatia Hazarika limit, to become a bigger neutron star or a black hole due to gravitational collapse. It was observed in gravitational wave of GW170817 to have a 2.82 time solar mass. The formula is:

M _star = 2 ^3/2 M _sun

As the velocity of the neutron star, along with the rotation increases, gravitational collapse may or may not occur. If it does collapse it converts into a black hole after exceeding the Bhatia Hazarika Limit of 2.8 times solar mass. The formula is described again theoretically and mathematically, A neutron star smash breaks universe showing 2.8 times solar mass shown in a lecture at Niels Bohr Institute of University of Copenhagen.

A new discovery has been made by LIGO for GW190425 which have 2.8 times solar mass A book Seeing God through Science exploring the science narrates that gravitational collapse occurs at 2.8 solar mass. The complex life of Star cluster also shows 2.8 solar mass for neutron star, NASA, the book "The Hundred Greatest Stars", the book "Extreme stars". All exclaimed about the gravitational collapse at 2.8 times of solar mass.

References

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