Newtonian analogue of Schwarzschild–de Sitter spacetime: Influence on the local kinematics in galaxies

Sarkar, Tamal; Ghosh, Shubhrangshu; Bhadra, Arunava

doi:10.1103/physrevd.90.063008

Cited by 17 publications

(31 citation statements)

References 60 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Here, we present an approach to "pseudo-Newtonization" which is systematic, taking only the space-time metric in a convenient set of coordinates and giving a pseudo-Newtonian prescription without prior knowledge of the structure of orbits which are supposed to be mimicked by the pseudo-Newtonian dynamics. This approach is inspired by previous works of Tejeda & Rosswog (2013, 2015, Sarkar et al (2014), and Ghosh et al (2014), but expands the stated works in generality and elucidates the pattern and theoretical foundation of these pseudo-Newtonian prescriptions. The following is only an overview of the results and a full description can be found in Witzany & Lämmerzahl (2016).…”

Section: Introductionmentioning

confidence: 84%

A pseudo-Newtonian description of any stationary space-time

Witzany

Lämmerzahl

2016

Proc. IAU

View full text Add to dashboard Cite

Since the first investigations into accretion onto black holes, astrophysicists have proposed effective Newtonian-like potentials to mimic the strong-field behavior of matter near a Schwarzschild or Kerr black hole. On the other hand, the fields of neutron stars or black holes in many of the alternative gravity theories differ from the idealized Schwarzschild or Kerr field which would require a number of new potentials. To resolve this, we give a Newtonian-like Hamiltonian which almost perfectly mimics the behavior of test particles in any given stationary space-time. The properties of the Hamiltonian are excellent in static space-times such as the Schwarzschild black hole, but become worse for space-times with gravito-magnetic or dragging effects such as near the Kerr black hole.

show abstract

Section: Introductionmentioning

confidence: 84%

A pseudo-Newtonian description of any stationary space-time

Witzany

Lämmerzahl

2016

Proc. IAU

View full text Add to dashboard Cite

show abstract

“…Moreover, here we have also assumed the criteria of 'low energy limit' to derive the said potential. The low energy limit criteria may be suitable to describe static geometries, for which, the results would be precisely exact and the GR features in its entirety would be reproduced with remarkable accuracy (Sarkar et al 2014). For axially symmetric Kerr geometry, it provides more limitations.…”

Section: Discussionmentioning

confidence: 99%

Newtonian analogue of corresponding space–time dynamics of rotating black holes: implication for black hole accretion

Ghosh

Sarkar

Bhadra

2014

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

Based on the conserved Hamiltonian for a test particle, we have formulated a Newtonian analogue of Kerr spacetime in the 'low energy limit of the test particle motion' that, in principle, can be comprehensively used to describe general relativistic (GR) features of Kerr spacetime, however, with less accuracy for high spin. The derived potential, which has an explicit velocity dependence, contains the entire relativistic features of corresponding spacetime including the frame dragging effect, unlike other prevailing pseudo-Newtonian potentials (PNPs) for the Kerr metric where such an effect is either totally missing or introduced in a ad hoc manner. The particle dynamics with this potential precisely reproduce the GR results within a maximum ∼ 10% deviation in energy for a particle orbiting circularly in the vicinity of a rapidly corotating black hole. GR epicyclic frequencies are also well reproduced with the potential, though with a relatively higher percentage of deviation. For counterrotating cases, the obtained potential replicate the GR results with precise accuracy. The KerrNewtonian potential also approximates the radius of marginally stable and marginally bound circular orbits with reasonable accuracy for a < 0.7. Importantly, the derived potential can imitate the experimentally tested GR effects like perihelion advancement and bending of light with reasonable accuracy. The formulated Kerr-Newtonian potential thus can be useful to study complex accreting plasma dynamics and its implications around rotating BHs in the Newtonian framework, avoiding GR gas dynamical equations.

show abstract

“…For any arbitrary physical quantity G, the relative deviation (ξ) is defined as ξ = 2| GDS−GSW GDS+GSW |, 52 where subscripts "DS" and "SW" represent corresponding quantities in "SDS" and "Schwarzschild" backgrounds, respectively. In Fig.…”

Section: Adiabatic Casementioning

confidence: 99%

“…One of them, called LERGs, a more generalization of low luminous AGNs (LLAGNs), which are often massive ellipticals 37 plausibly harboring SMBHs, are believed to be powered by hot mode accretion which is radiatively inefficient, accreting gaseous plasma directly from the hot X-ray emitting phase S. Ghosh and P. Banik large scales, plausibly around and beyond the central kiloparsecs-scale structure in local-galaxies, owing to its small value. 52 A very likely local scenario where a significant influence of cosmological constant may occur is the relativistic accretion phenomena around supermassive BHs (SMBHs), involving length-scales of the order of hundreds of parsecs or even more.…”

Section: Introductionmentioning

confidence: 99%

Characteristics of transonic spherical symmetric accretion flow in Schwarzschild-de Sitter and Schwarzschild anti-de Sitter backgrounds, in pseudo-general relativistic paradigm

Ghosh

Banik

2015

Int. J. Mod. Phys. D

Self Cite

View full text Add to dashboard Cite

In this paper, we present a complete work on steady state spherically symmetric Bondi type accretion flow in the presence of cosmological constant (Λ) in both Schwarzschildde Sitter (SDS) and Schwarzschild anti-de Sitter (SADS) backgrounds considering an isolated supermassive black hole (SMBH), with the inclusion of a simple radiative transfer scheme, in the pseudo-general relativistic paradigm. We do an extensive analysis on the transonic behavior of the Bondi type accretion flow onto the cosmological BHs including a complete analysis of the global parameter space and the stability of flow, and do a complete study of the global family of solutions for a generic polytropic flow. Bondi type accretion flow in SADS background renders multiplicity in its transonic behavior with inner "saddle" type and outer "center" type sonic points, with the transonic solutions forming closed loops or contours. There is always a limiting value for |Λ| up to which we obtain valid stationary transonic solutions, which correspond to both SDS and SADS geometries; this limiting value moderately increases with the increasing radiative efficiency of the flow, especially correspond to Bondi type accretion flow in SADS background. Repulsive Λ suppresses the Bondi accretion rate by an order of magnitude for relativistic Bondi type accretion flow for a certain range in temperature, and with a marginal increase in the Bondi accretion rate if the corresponding accretion flow occurs in SADS background. However, for a strongly radiative Bondi type accretion flow with high mass accretion rate, the presence of cosmological constant do not much influence the corresponding Bondi accretion rate of the flow. Our analysis show that the relic cosmological constant has a substantial effect on Bondi type accretion flow onto isolated SMBHs and their transonic solutions beyond length-scale of kiloparsecs, especially if the Bondi type accretion occurs onto the host supergiant ellipticals or central dominant (CD) galaxies directly from ambient intercluster medium (ICM). However, for high mass accretion rate, the influence of cosmological constant on Bondi accretion dynamics, generically, diminishes. As active galactic nuclei (AGN)/ICM feedback can be advertently linked to Bondi type spherical accretion, any proper modeling of AGN feedback or megaparsecs-scale jet dynamics or accretion flow from ICM onto the central regions of host galaxies should take into account the relevant information of 1550084-1 Int. J. Mod. Phys. D Downloaded from www.worldscientific.com by THE UNIVERSITY OF NEW SOUTH WALES on 08/10/15. For personal use only. S. Ghosh and P. Banikrepulsive Λ, especially in context to supergiant elliptical galaxies or CD galaxies present in rich galaxy clusters. This could also explore the feasibility to limit the value of Λ, from the kinematics in local galactic-scales.

show abstract

Newtonian analogue of Schwarzschild–de Sitter spacetime: Influence on the local kinematics in galaxies

Cited by 17 publications

References 60 publications

A pseudo-Newtonian description of any stationary space-time

A pseudo-Newtonian description of any stationary space-time

Newtonian analogue of corresponding space–time dynamics of rotating black holes: implication for black hole accretion

Characteristics of transonic spherical symmetric accretion flow in Schwarzschild-de Sitter and Schwarzschild anti-de Sitter backgrounds, in pseudo-general relativistic paradigm

Contact Info

Product

Resources

About