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2019

Bootstrapped Newtonian stars and black holes

Casadio, Roberto, Lenzi, Michele, Micu, Octavian

Understand

We study equilibrium configurations of a homogenous ball of matter in a bootstrapped description of gravity which includes a gravitational self-interaction term beyond the Newtonian coupling.

Both matter density and pressure are accounted for as sources of the gravitational potential for test particles.
Unlike the general relativistic case, no Buchdahl limit is found and the pressure can in principle support a star of arbitrarily large compactness.
By defining the horizon as the location where the escape velocity of test particles equals the speed of light, like in Newtonian gravity, we find a minimum value of the compactness for which this occurs.

Built on

K. Schwarzschild, Sitzungsber. Preuss. Akad. Wiss. Berlin (Math. Phys. ) 1916
1916
Earlier work this paper cites.
P. Nicolini, Int. J. Mod. Phys. A 24
Original
1939
Earlier work this paper cites.
R.L. Arnowitt, S. Deser and C.W. Misner, Phys. Rev. 116
1959
Earlier work this paper cites.
H. A. Buchdahl, Phys. Rev. 116
1959
Earlier work this paper cites.
R. Gaines, J. Differential Equations 12
1970
Earlier work this paper cites.
S. W. Hawking and G. F. R. Ellis, “The Large Scale Structure of Space-Time,” (Cambridge University Press, Cambridge, 1973)
1973
Earlier work this paper cites.
R. M. Wald, “General Relativity,” (Chicago University Press, Chicago, 1984)
1984
Earlier work this paper cites.
R. P. Geroch and J. H. Traschen, Phys. Rev. D 36
1993
Earlier work this paper cites.
J. F. Donoghue, Phys. Rev. D 50
1994
Earlier work this paper cites.
A.C. King, J. Billingham, and S.R. Otto, “Differential equations: linear, nonlinear, ordinary, partial,” (Cambridge University Press, Cambridge, 2003)
2003
Earlier work this paper cites.