Mass Limit of Neutron Star

Author(s)
Jehangir Ahmad Dar

Affiliation(s)

Inventor at Department of USIC/EDC, University of Kashmir, Hazratbal, Srinagar, India.

Inventor at Department of USIC/EDC, University of Kashmir, Hazratbal, Srinagar, India.

ABSTRACT

The mass limit of neutron star has still remained a mystery. The
existing Tolman-Oppenheimer-Volkoff (TOV) equation for calculating the limit
always gives different values, by introducing different assumptions and having
been predicted like 0.7 Mo, 3.2 Mo, 3.6 Mo, where Mo = 1.98 × 10^{30} Kg.
There is a need of some better technique to adopt other than TOV relation to
seek out the value. In this paper, a new relation between the mass of the collapsing star and its
average density *ρ*′ has been derived and used to calculate the limit of neutron
star. The conditions in radii between Schwarz Child’s radius and the actual
radius of the collapsing star have been introduced to calculate the mass of
star above which it will transform into a black hole and below it to a neutron
star. A new constant, *J _{N}* = 8.53707554 × 1039 N

KEYWORDS

Black Hole, Neutron Star, Schwarz Child’s Radius Relation, Degeneracy Pressure, Event Horizon, FCC and HCP Lattices and TOV Equation

Black Hole, Neutron Star, Schwarz Child’s Radius Relation, Degeneracy Pressure, Event Horizon, FCC and HCP Lattices and TOV Equation

Cite this paper

Dar, J. (2014) Mass Limit of Neutron Star.*International Journal of Astronomy and Astrophysics*, **4**, 414-418. doi: 10.4236/ijaa.2014.42036.

Dar, J. (2014) Mass Limit of Neutron Star.

References

[1] Srinivasan, G. (2002) The Maximum Mass of Neutron Stars. Bulletin of Astronomic Society of India, 30, 523-547.

[2] Brill, D. (2012) Black Hole Horizons and How They Begin. Astronomical Review.

[3] Oppenheimer, J.R. and Volkoff, G.M. (1939) Physical Review Letters, 55, 374.

[4] Rhoades, C.E. and Ruffini, J.R. (1974) Physical Review Letters, 32, 3240.

http://dx.doi.org/10.1103/PhysRevLett.32.324

[5] Hales, T.C. The Kepler Conjecture. http://front.math.ucdavis.edu/math.MG/9811078

[6] Hales, T.C. (1992) The Spherical Packing Problem. Journal of Computing and Applied Mathematics, 44, 41-76. http://dx.doi.org/10.1016/0377-0427(92)90052-Y

[7] Llanes-Estrada, F.J. and Navarro, G.M. (2011) Cubic Neutrons.

[1] Srinivasan, G. (2002) The Maximum Mass of Neutron Stars. Bulletin of Astronomic Society of India, 30, 523-547.

[2] Brill, D. (2012) Black Hole Horizons and How They Begin. Astronomical Review.

[3] Oppenheimer, J.R. and Volkoff, G.M. (1939) Physical Review Letters, 55, 374.

[4] Rhoades, C.E. and Ruffini, J.R. (1974) Physical Review Letters, 32, 3240.

http://dx.doi.org/10.1103/PhysRevLett.32.324

[5] Hales, T.C. The Kepler Conjecture. http://front.math.ucdavis.edu/math.MG/9811078

[6] Hales, T.C. (1992) The Spherical Packing Problem. Journal of Computing and Applied Mathematics, 44, 41-76. http://dx.doi.org/10.1016/0377-0427(92)90052-Y

[7] Llanes-Estrada, F.J. and Navarro, G.M. (2011) Cubic Neutrons.