Existence of Black Neutron Star

ABSTRACT

A sufficiently large star will collapse to form a Black Hole Singularity due to Gravitational Pressure beyond Neutron Degeneracy. A Black Hole exhibits extremely strong Gravitational attraction that no particle or electromagnetic radiation can escape from it. The boundary of the region from which no escape is possible is called Event Horizon. In this work it is proposed that there exists a Neutron star smaller than Event Horizon, which is termed as Black Neutron Star. Furthermore an alternative method is proposed to ascertain the maximum permissible mass limit of the Neutron Star and the minimum mass limit of the naturally occurring gravitationally collapsed Black hole.

A sufficiently large star will collapse to form a Black Hole Singularity due to Gravitational Pressure beyond Neutron Degeneracy. A Black Hole exhibits extremely strong Gravitational attraction that no particle or electromagnetic radiation can escape from it. The boundary of the region from which no escape is possible is called Event Horizon. In this work it is proposed that there exists a Neutron star smaller than Event Horizon, which is termed as Black Neutron Star. Furthermore an alternative method is proposed to ascertain the maximum permissible mass limit of the Neutron Star and the minimum mass limit of the naturally occurring gravitationally collapsed Black hole.

Cite this paper

Rajesh, T. (2015) Existence of Black Neutron Star.*International Journal of Astronomy and Astrophysics*, **5**, 11-14. doi: 10.4236/ijaa.2015.51002.

Rajesh, T. (2015) Existence of Black Neutron Star.

References

[1] Chandrasekhar, S. (1935) The Highly Collapsed Configurations of a Stellar Mass. Monthly Notices of the Royal Astronomical Society, 95, 207-225.

http://dx.doi.org/10.1093/mnras/95.3.207

[2] Bombaci, I. (1996) The Maximum Mass of a Neutron Star. Astronomy and Astrophysics, 305, 871-877.

[3] Carroll, B.W. and Ostlie, D.A. (2006) §16.3. The Physics of Degenerate Matter. In: An Introduction to Modern Astrophysics, 2nd Edition, Addison-Wesley, Boston.

[4] Oppenheimer, J.R. and Volkoff, G.M. (1939) On Massive Neutron Cores. Physical Review Letters, 55, 374.

http://dx.doi.org/10.1103/PhysRev.55.374

[5] Sloane, N.J.A. (1998) The Sphere-Packing Problem. Documenta Mathematika, 3, 387-396.

[6] Hales, T.C. (1998) The Kepler Conjecture.

http://front.math.ucdavis.edu/math.MG/9811078

[1] Chandrasekhar, S. (1935) The Highly Collapsed Configurations of a Stellar Mass. Monthly Notices of the Royal Astronomical Society, 95, 207-225.

http://dx.doi.org/10.1093/mnras/95.3.207

[2] Bombaci, I. (1996) The Maximum Mass of a Neutron Star. Astronomy and Astrophysics, 305, 871-877.

[3] Carroll, B.W. and Ostlie, D.A. (2006) §16.3. The Physics of Degenerate Matter. In: An Introduction to Modern Astrophysics, 2nd Edition, Addison-Wesley, Boston.

[4] Oppenheimer, J.R. and Volkoff, G.M. (1939) On Massive Neutron Cores. Physical Review Letters, 55, 374.

http://dx.doi.org/10.1103/PhysRev.55.374

[5] Sloane, N.J.A. (1998) The Sphere-Packing Problem. Documenta Mathematika, 3, 387-396.

[6] Hales, T.C. (1998) The Kepler Conjecture.

http://front.math.ucdavis.edu/math.MG/9811078