In d-dimensional spacetime, strange quark stars gain stability with increasing dimension for ranges of central density, with the mass maximum marking the onset of radial instability, and Newtonian stability holds for adiabatic index at or above 2(d-2)/(d-1).
Hydrostatic Equilibrium of a Perfect Fluid Sphere with Exterior Higher-Dimensional Schwarzschild Spacetime
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abstract
We discuss the question of how the number of dimensions of space and time can influence the equilibrium configurations of stars. We find that dimensionality does increase the effect of mass but not the contribution of the pressure, which is the same in any dimension. In the presence of a (positive) cosmological constant the condition of hydrostatic equilibrium imposes a lower limit on mass and matter density. We show how this limit depends on the number of dimensions and suggest that $\Lambda > 0$ is more effective in 4D than in higher dimensions. We obtain a general limit for the degree of compactification (gravitational potential on the boundary) of perfect fluid stars in $D$-dimensions. We argue that the effects of gravity are stronger in 4D than in any other number of dimensions. The generality of the results is also discussed.
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UNVERDICTED 2representative citing papers
Generalized Buchdahl bounds on horizonless object compactness are derived in the presence of a cosmological constant, preserving universality while yielding method-dependent results.
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Extra dimensions' influence on the equilibrium and radial stability of strange quark stars
In d-dimensional spacetime, strange quark stars gain stability with increasing dimension for ranges of central density, with the mass maximum marking the onset of radial instability, and Newtonian stability holds for adiabatic index at or above 2(d-2)/(d-1).
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Buchdahl stars and bounds with cosmological constant
Generalized Buchdahl bounds on horizonless object compactness are derived in the presence of a cosmological constant, preserving universality while yielding method-dependent results.