| Full text | |
| Author(s): |
Total Authors: 2
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| Affiliation: | [1] Univ Lisbon, IST, Dept Fis, Ctr Multidisciplinar Astrofis CENTRA, P-1049001 Lisbon - Portugal
[2] Univ Fed ABC, Ctr Ciencias Nat & Humanas, BR-09210580 Santo Andre, SP - Brazil
Total Affiliations: 2
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| Document type: | Journal article |
| Source: | Classical and Quantum Gravity; v. 32, n. 13 JUL 9 2015. |
| Web of Science Citations: | 7 |
| Abstract | |
Buchdahl, by imposing a few reasonable physical assumptions on matter, i.e., its density is a nonincreasing function of the radius and the fluid is a perfect fluid, and on the configuration, such as the exterior is the Schwarzschild solution, found that the radius r(0) to mass m ratio of a star would obey the bound r0 m. 9 4, the Buchdahl bound. He also noted that the bound was saturated by the Schwarzschild interior solution, i.e., the solution with rho(m)(r) = constant where rho(m)(r) m is the energy density of the matter at r, when the central central pressure blows to infinity. Generalizations of this bound in various forms have been studied. An important generalization was given by Andreasson, by including electrically charged matter and imposing a different set of conditions, namely, p + 2p(T) <= rho m where p is the radial pressure and p(T) the tangential pressure. His bound is sharp and given by r(0)/m >= 9/(1 +root 1+ 3q(2)/r(0)(2))(2), the Buchdahl-Andreasson bound, with q being the total electric charge of the star. For q = 0 one recovers the Buchdahl bound. However, following Andreasson's proof, the configuration that saturates the Buchdahl bound is an uncharged shell, rather than the Schwarzschild interior solution. By extension, the configurations that saturate the electrically charged Buchdahl-Andreasson bound are charged shells. One could expect then, in turn, that there should exist an electrically charged equivalent to the interior Schwarzschild limit. We find here that this equivalent is provided by the equation rho(m)(r) + Q(2)(r)(8 pi r(4)) constant where Q(r) is the electric charge at r. This equation was put forward by Cooperstock and de la Cruz, and Florides, and realized in Guilfoyle's stars. When the central pressure goes to infinity, Guilfoyle's stars are configurations that also saturate the Buchdahl-Andreasson bound. A proof in Buchdahl's manner, such that these configurations are the limiting configurations of the bound, remains to be found. (AU) | |
| FAPESP's process: | 12/08041-5 - Regular black holes, quasiblack holes and other compact objects in general relativity |
| Grantee: | Vilson Tonin Zanchin |
| Support Opportunities: | Scholarships abroad - Research |