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| Main Authors: | , , |
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| Format: | Preprint |
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2025
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| Online Access: | https://arxiv.org/abs/2505.02871 |
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| _version_ | 1866916720288989184 |
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| author | Herrera, L. Di Prisco, A. Ospino, J. |
| author_facet | Herrera, L. Di Prisco, A. Ospino, J. |
| contents | We present a model of an evolving spherically symmetric dissipative self-gravitating fluid distribution which tends asymptotically to a ghost star, meaning that the end state of such a system corresponds to a static fluid distribution with vanishing total mass, and energy-density distribution which is negative in some regions of the fluid. The model is inspired in a solution representing a fluid evolving quasi-homologously and with vanishing complexity factor. However in order to satisfy the asymptotic behavior mentioned above, the starting solution has to be modified, as a consequence of which the resulting model only satisfies the two previously mentioned conditions, asymptotically. Additionally a condition on the variation of the infinitesimal proper radial distance between two neighboring points per unit of proper time is imposed, which implies the presence of a cavity surrounding the center. Putting together all these conditions we are able to obtain an analytical model depicting the emergence of a ghost star. Some potential observational consequences of this phenomenon are briefly discussed at the last section. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2505_02871 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The birth of a ghost star Herrera, L. Di Prisco, A. Ospino, J. General Relativity and Quantum Cosmology We present a model of an evolving spherically symmetric dissipative self-gravitating fluid distribution which tends asymptotically to a ghost star, meaning that the end state of such a system corresponds to a static fluid distribution with vanishing total mass, and energy-density distribution which is negative in some regions of the fluid. The model is inspired in a solution representing a fluid evolving quasi-homologously and with vanishing complexity factor. However in order to satisfy the asymptotic behavior mentioned above, the starting solution has to be modified, as a consequence of which the resulting model only satisfies the two previously mentioned conditions, asymptotically. Additionally a condition on the variation of the infinitesimal proper radial distance between two neighboring points per unit of proper time is imposed, which implies the presence of a cavity surrounding the center. Putting together all these conditions we are able to obtain an analytical model depicting the emergence of a ghost star. Some potential observational consequences of this phenomenon are briefly discussed at the last section. |
| title | The birth of a ghost star |
| topic | General Relativity and Quantum Cosmology |
| url | https://arxiv.org/abs/2505.02871 |