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PreprintCC BY 4.0arXiv

Relativistic stellar collapse of initially static configurations

  • Keshlan S. Govinder
  • Megandhren Govender
  • Sunil Maharaj
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Abstract

We study the dynamics of a radiating relativistic star in the presence of the electromagnetic field and the cosmological constant. The evolution of the model originates from an initially static configuration. The temporal behaviour of the system is governed by a nonlinear second order equation which is studied using a phase plane analysis. We show that in the general case, with all physical parameters present, fold bifurcations arise which are related to nonzero charge and cosmological constant. Our treatment clarifies earlier results and we extend our study to the general solution space. We obtain a more comprehensive understanding of the temporal evolution for a shear-free configuration during collapse.

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Cite

BibTeXRIS
BibTeX
@misc{govinder2026relativistic,
  title = {{Relativistic stellar collapse of initially static configurations}},
  author = {Keshlan S. Govinder and Megandhren Govender and Sunil Maharaj},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.02655},
  eprint = {2609.02655},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.02655},
  note = {CC BY 4.0},
}
RIS
TY  - UNPB
TI  - Relativistic stellar collapse of initially static configurations
AU  - Keshlan S. Govinder
AU  - Megandhren Govender
AU  - Sunil Maharaj
PY  - 2026
DA  - 2026/09/02
PB  - arXiv
DO  - 10.48550/arxiv.2609.02655
UR  - https://arxiv.org/abs/2609.02655
AB  - We study the dynamics of a radiating relativistic star in the presence of the electromagnetic field and the cosmological constant. The evolution of the model originates from an initially static configuration. The temporal behaviour of the system is governed by a nonlinear second order equation which is studied using a phase plane analysis. We show that in the general case, with all physical parameters present, fold bifurcations arise which are related to nonzero charge and cosmological constant. Our treatment clarifies earlier results and we extend our study to the general solution space. We obtain a more comprehensive understanding of the temporal evolution for a shear-free configuration during collapse.
ER  -