Slowly rotating curzon-chazy metric

Camacho, Paulo Montero; Frutos─Alfaro, Francisco; Cháves, Carlos Gutiérrez; García, Iván Cordero

doi:10.15517/rmta.v22i2.20833

Cited by 3 publications

(7 citation statements)

References 22 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…These manifolds will be called "ZVδ" for brevity. We also include the limiting configuration δ → ∞ with fixed M , which corresponds to Chazy-Curzon solution in spherical coordinates [47,[52][53][54]:…”

Section: )mentioning

confidence: 99%

Photon trapping in static axially symmetric spacetime

Gal’tsov

Kobialko

2019

Phys. Rev. D

View full text Add to dashboard Cite

Recently, several new characteristics have been introduced to describe null geodesic structure of strong gravitational field, such as photon regions, transversely trapping surfaces and some generalizations. They give an alternative and concise way to describe lensing and shadow features of compact objects with strong gravitational field without recurring to complete integration of the geodesic equations. Here we test this construction in the case of the Weyl metrics when geodesic equations are non-separable, and thus can not be integrated analytically, while the above characteristic surfaces and regions can be described in a closed form. We develop further our formalism for a class of static axially symmetric spacetimes introducing more detailed specification of transversely trapping surfaces in terms of their principal curvatures. Surprisingly, we find in the static case without spherical symmetry certain features, such as photon regions, previously known in the Kerr space. These photon regions can be regarded as photon spheres, "thickened" due to oblateness of the metric.including the dilaton field [34]).Meanwhile, in the stationary spacetimes photon surfaces generically do not exist, being, in some sense, disintegrated by rotation. The Taub-NUT metric, though belongs to this class, is an exception, whose existence is explained by local SO(3) symmetry which is preserved. In the Kerr metric the circular photon orbits exist in the equatorial plane [35]. Non-equatorial orbits with constant Boyer-Lindquist radii no longer belong to any plane, but lie on the surface of a sphere instead ("spherical photon orbits" [36]). But such surfaces are not photon spheres, which by definition should be densely filled. In the Kerr case every spherical orbit corresponds to certain value of the impact parameter defined as ratio of the angular momentum to the energy. Altogether spherical orbits now will a three-dimensional photon region (PR) [37][38][39], which can be regarded as "thickened" photon sphere. Note that the closed photon orbits may exist in more general spacetimes in which case the name of fundamental or/and spheroidal photon orbits was suggested [40][41][42].More general trapping surfaces, proposed in [43] and further studied in [44], were called transversely trapping surfaces (TTS). In Schwarzschild case TTS are the spheres with the radii r ≤ 3M . These are defined as surfaces such that initially tangent photons either remain in them or move inward; these do exist in Kerr and more general stationary axially symmetric metrics.The totality of TTSs form a three-dimensional region (TTR), which apparently will be invisible if one looks at the Schwarzschild black hole illuminated from behind. Further generalizations suggested in [44] include partial TTS (PTTS) which are non-closed surfaces (contrary to the definition in [43]) of the shape of a spherical cap. Finally, it is reasonable to introduce anti-TTS and PTTS (abbreviated as ATTS and APPTS, the corresponding regions -TTR and PTTR respoctively) replacing inward to outwa...

show abstract

Section: )mentioning

confidence: 99%

Photon trapping in static axially symmetric spacetime

Gal’tsov

Kobialko

2019

Phys. Rev. D

View full text Add to dashboard Cite

show abstract

“…Moreover, these limiting cases confirm that our metric adequately describes a mass with charge and quadrupole under rotation. We successfully applied the perturbation method developed by Frutos et al in [23,24,25,27] to obtain a new approximate metric. Notice that the main improvement of our work with respect to [24,27] is the inclusion of charge.…”

Section: Discussionmentioning

confidence: 99%

“…Here and in the following sections we will use the method developed by Frutos et al in [23,24,25] to obtain a Kerr-Newman-like metric i.e. a spacetime capable of describing a slightly deformed rotating charged mass.…”

Section: The Perturbing Methods For the Kerr Metricmentioning

confidence: 99%

See 1 more Smart Citation

Approximate Kerr-Like Metric with Quadrupole

Frutos─Alfaro¹

2016

IJAA

Self Cite

View full text Add to dashboard Cite

The Kerr metric is known to present issues when trying to find an interior solution. In this work we continue in our efforts to construct a more realistic exterior metric for astrophysical objects. A new approximate metric representing the spacetime of a charged, rotating and slightly-deformed body is obtained by perturbing the Kerr-Newman metric to include the mass-quadrupole and quadrupole-quadrupole orders. It has a simple form, because is Kerr-Newman-like. Its post-linear form without charge coincides with post-linear quadrupole-quadrupole metrics already found.

show abstract

“…Basically, our technique consists in cleverly changing the potentials of the Lewis metric while maintaining the cross term (rotational term). We have already applied this technique and obtained other approximate metrics [12,11,26]. In comparison to our previous efforts this work includes the addition of charge.…”

Section: Introductionmentioning

confidence: 99%

Approximate Kerr-Newman-like metric with quadrupole

Frutos─Alfaro

Gómez-Ovares

Montero-Camacho

2021

RMTA

View full text Add to dashboard Cite

The Kerr metric is known to have issues when trying to find a physical interior solution. In this work we continue our efforts to construct a more realistic exterior metric for astrophysical objects. A new approximate metric representing the spacetime of a charged, rotating and slightly-deformed body is obtained by perturbing the Kerr-Newman metric to include the mass-quadrupole and quadrupole-quadrupole orders. It has a simple form because it is Kerr-Newman-like.

show abstract

Slowly rotating curzon-chazy metric

Cited by 3 publications

References 22 publications

Photon trapping in static axially symmetric spacetime

Photon trapping in static axially symmetric spacetime

Approximate Kerr-Like Metric with Quadrupole

Approximate Kerr-Newman-like metric with quadrupole

Contact Info

Product

Resources

About