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PreprintCC BY 4.0arXiv

An exact Kerr-like rotating Morris--Thorne wormhole: throat, ergoregion and equatorial shadow slice

  • Mark Sukaiti
  • Davide Batic
  • Denys Dutykh
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Abstract

We construct an exact Kerr-like rotating extension of the zero-redshift Morris--Thorne wormhole in a Teo-type stationary, axisymmetric ansatz. The Einstein equations for an anisotropic source comoving with zero angular momentum observers fix 𝒦(r)=r2+a2 and reduce frame dragging to a radial quadrature. For b(r)=r02/r, this is evaluated using incomplete elliptic integrals and normalised by the ADM angular momentum. The spacetime is asymptotically flat with zero ADM mass, so a=JADM/MADM does not apply. The oblateness length a and angular momentum JADM remain independent, yielding a family (r0,a,JADM). The choice JADM=ar0 selects only a one-parameter slice for numerical ergoregion and equatorial-capture illustrations; it is not a field-equation constraint. We find rth=√(r02βˆ’a2), with reality bound |a|≀ r0 and regular range 0≀ |a|<r0. In the canonical stationary foliation, the throat is defined quasi-locally as the unique closed surface S0 in the family Sβ„“ with zero mean curvature and positive area second variation. Moreover, r=rth and β„“=0 are coordinate representations. A signed throat-adapted coordinate reveals two asymptotically flat ends, excludes closed timelike curves, and establishes that the throat is timelike, not a horizon. These conclusions hold independently of JADM=ar0. The supporting stress tensor, reconstructed from the Einstein tensor, is an effective phenomenological source. We do not claim any microscopic matter Lagrangian or realistic equation of state. We also determine the ergoregion onset. Since the full Hamilton--Jacobi equation is nonseparable, we limit ourselves to derive the optical result for a one-dimensional equatorial capture interval.

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Cite

BibTeXRIS
BibTeX
@misc{sukaiti2026exact,
  title = {{An exact Kerr-like rotating Morris--Thorne wormhole: throat, ergoregion and equatorial shadow slice}},
  author = {Mark Sukaiti and Davide Batic and Denys Dutykh},
  howpublished = {arXiv},
  year = {2026},
  month = sep,
  doi = {10.48550/arxiv.2609.22823},
  eprint = {2609.22823},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2609.22823},
  note = {CC BY 4.0},
}
RIS
TY  - UNPB
TI  - An exact Kerr-like rotating Morris--Thorne wormhole: throat, ergoregion and equatorial shadow slice
AU  - Mark Sukaiti
AU  - Davide Batic
AU  - Denys Dutykh
PY  - 2026
DA  - 2026/09/19
PB  - arXiv
DO  - 10.48550/arxiv.2609.22823
UR  - https://arxiv.org/abs/2609.22823
AB  - We construct an exact Kerr-like rotating extension of the zero-redshift Morris--Thorne wormhole in a Teo-type stationary, axisymmetric ansatz. The Einstein equations for an anisotropic source comoving with zero angular momentum observers fix 𝒦(r)=r^2+a^2 and reduce frame dragging to a radial quadrature. For b(r)=r_0^2/r, this is evaluated using incomplete elliptic integrals and normalised by the ADM angular momentum. The spacetime is asymptotically flat with zero ADM mass, so a=J_ADM/M_ADM does not apply. The oblateness length a and angular momentum J_ADM remain independent, yielding a family (r_0,a,J_ADM). The choice J_ADM=ar_0 selects only a one-parameter slice for numerical ergoregion and equatorial-capture illustrations; it is not a field-equation constraint. We find r_th=√(r_0^2βˆ’a^2), with reality bound |a|≀ r_0 and regular range 0≀ |a|<r_0. In the canonical stationary foliation, the throat is defined quasi-locally as the unique closed surface S_0 in the family S_β„“ with zero mean curvature and positive area second variation. Moreover, r=r_th and β„“=0 are coordinate representations. A signed throat-adapted coordinate reveals two asymptotically flat ends, excludes closed timelike curves, and establishes that the throat is timelike, not a horizon. These conclusions hold independently of J_ADM=ar_0. The supporting stress tensor, reconstructed from the Einstein tensor, is an effective phenomenological source. We do not claim any microscopic matter Lagrangian or realistic equation of state. We also determine the ergoregion onset. Since the full Hamilton--Jacobi equation is nonseparable, we limit ourselves to derive the optical result for a one-dimensional equatorial capture interval.
ER  -