scholarly journals Conformal Ricci Collineations of Static Spherically Symmetric Spacetimes

2008 ◽  
Vol 49 (6) ◽  
pp. 1527-1532 ◽  
Author(s):  
Ugur Camci ◽  
Asghar Qadir ◽  
K Saifullah
Keyword(s):  
Spherically Symmetric ◽  
Ricci Collineations ◽  
Symmetric Spacetimes ◽  
Spherically Symmetric Spacetimes ◽  
Static Spherically Symmetric Spacetimes

scholarly journals Non-static spherically symmetric spacetimes and their conformal Ricci collineations

2019 ◽  
Vol 9 (2) ◽  
pp. 393-400 ◽  
Author(s):  
Fawad Khan ◽  
Tahir Hussain ◽  
Ashfaque Hussain Bokhari ◽  
Sumaira Saleem Akhtar
Keyword(s):  
Vector Field ◽  
Infinite Number ◽  
Ricci Tensor ◽  
Spherically Symmetric ◽  
Ricci Collineations ◽  
Symmetric Spacetimes ◽  
Integrability Conditions ◽  
Fluid Matter ◽  
Spherically Symmetric Spacetimes ◽  
Static Spherically Symmetric Spacetimes

Abstract For a perfect fluid matter, we present a study of conformal Ricci collineations (CRCs) of non-static spherically symmetric spacetimes. For non-degenerate Ricci tenor, a vector field generating CRCs is found subject to certain integrability conditions. These conditions are then solved in various cases by imposing certain restrictions on the Ricci tensor components. It is found that non-static spherically symmetric spacetimes admit 5, 6 or 15 CRCs. In the degenerate case, it is concluded that such spacetimes always admit infinite number of CRCs.

Homothetic Ricci collineations of non-static spherically symmetric spacetimes with perfect fluid matter

2018 ◽  
Vol 33 (34) ◽  
pp. 1850196
Author(s):  
Tahir Hussain ◽  
Sumaira Saleem Akhtar ◽  
Fawad Khan
Keyword(s):  
Perfect Fluid ◽  
Infinite Number ◽  
Ricci Tensor ◽  
Spherically Symmetric ◽  
Ricci Collineations ◽  
Symmetric Spacetimes ◽  
Fluid Matter ◽  
Spherically Symmetric Spacetimes ◽  
Static Spherically Symmetric Spacetimes

Non-static spherically symmetric spacetimes with perfect fluid matter are considered and their homothetic Ricci collineations (HRCs) are investigated for degenerate as well as non-degenerate Ricci tensor. The present analysis shows that, for non-degenerate Ricci tensor, the possible number of HRCs admitted by these spacetimes is 5, 6 or 7, while they possess 4, 11 or otherwise infinite number of HRCs when the Ricci tensor is degenerate.

Classification of Static Spherically Symmetric Spacetimes by Noether Symmetries

2013 ◽  
Vol 52 (10) ◽  
pp. 3534-3542 ◽  
Author(s):  
Ashfaque H. Bokhari ◽  
A. G. Johnpillai ◽  
A. H. Kara ◽  
F. M. Mahomed ◽  
F. D. Zaman
Keyword(s):  
Spherically Symmetric ◽  
Noether Symmetries ◽  
Symmetric Spacetimes ◽  
Spherically Symmetric Spacetimes ◽  
Static Spherically Symmetric Spacetimes

scholarly journals Bondi accretion in the spherically symmetric Johannsen–Psaltis spacetime

2019 ◽  
Vol 79 (11) ◽  
Author(s):  
Anslyn J. John ◽  
Chris Z. Stevens
Keyword(s):  
Accretion Rate ◽  
Kerr Metric ◽  
Spherically Symmetric ◽  
Gravitational Acceleration ◽  
Symmetric Spacetimes ◽  
Spherically Symmetric Spacetimes ◽  
Scalar Hair ◽  
Relativistic Analysis ◽  
Modified Theory ◽  
Static Spherically Symmetric Spacetimes

AbstractThe Johannsen–Psaltis spacetime explicitly violates the no-hair theorem. It describes rotating black holes with scalar hair in the form of parametric deviations from the Kerr metric. In principle, black hole solutions in any modified theory of gravity could be written in terms of the Johannsen–Psaltis metric. We study the accretion of gas onto a static limit of this spacetime. We utilise a recently proposed pseudo–Newtonian formulation of the dynamics around arbitrary static, spherically symmetric spacetimes. We obtain a potential that generalises the Paczyński–Wiita potential to the static Johannsen–Psaltis metric. We also perform a fully relativistic analysis of the geodesic equations in the static Johannsen–Psaltis spacetime. We find that positive (negative) values of the scalar hair parameter, $$\epsilon _{3}$$ϵ3, lower (raise) the accretion rate. Similarly, positive (negative) values of $$\epsilon _{3}$$ϵ3 reduce (increase) the gravitational acceleration of radially infalling massive particles.

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