Shearfree axial model in massive Brans–Dicke gravity
Abstract
This paper explores the influences of dark energy on the shearfree axially symmetric evolution by considering selfinteracting Brans–Dicke gravity as a dark energy candidate. We describe energy source of the model and derive all the effective dynamical variables as well as effective structure scalars. It is found that scalar field is one of the sources of anisotropy and dissipation. The resulting effective structure scalars help to study the dynamics associated with dark energy in any axial configuration. In order to investigate shearfree evolution, we formulate a set of governing equations along with heat transport equation. We discuss consequences of shearfree condition upon different SBD fluid models like dissipative nongeodesic and geodesic models. For dissipative nongeodesic case, the rotational distribution turns out to be the necessary and sufficient condition for radiating model. The dissipation depends upon inhomogeneous expansion. The geodesic model is found to be irrotational and nonradiating. The nondissipative geodesic model leads to FRW model for positive values of the expansion parameter.
 Authors:
 Department of Mathematics, University of the Punjab, QuaideAzam Campus, Lahore54590 (Pakistan)
 (Pakistan)
 Publication Date:
 OSTI Identifier:
 22617449
 Resource Type:
 Journal Article
 Resource Relation:
 Journal Name: Annals of Physics; Journal Volume: 376; Other Information: Copyright (c) 2016 Elsevier Science B.V., Amsterdam, The Netherlands, All rights reserved.; Country of input: International Atomic Energy Agency (IAEA)
 Country of Publication:
 United States
 Language:
 English
 Subject:
 71 CLASSICAL AND QUANTUM MECHANICS, GENERAL PHYSICS; AXIAL SYMMETRY; GEODESICS; GRAVITATION; HEAT TRANSFER; NONLUMINOUS MATTER
Citation Formats
Sharif, M., Email: msharif.math@pu.edu.pk, Manzoor, Rubab, Email: rubab.manzoor@umt.edu.pk, and Department of Mathematics, University of Management and Technology, Johar Town Campus, Lahore54782. Shearfree axial model in massive Brans–Dicke gravity. United States: N. p., 2017.
Web. doi:10.1016/J.AOP.2016.10.024.
Sharif, M., Email: msharif.math@pu.edu.pk, Manzoor, Rubab, Email: rubab.manzoor@umt.edu.pk, & Department of Mathematics, University of Management and Technology, Johar Town Campus, Lahore54782. Shearfree axial model in massive Brans–Dicke gravity. United States. doi:10.1016/J.AOP.2016.10.024.
Sharif, M., Email: msharif.math@pu.edu.pk, Manzoor, Rubab, Email: rubab.manzoor@umt.edu.pk, and Department of Mathematics, University of Management and Technology, Johar Town Campus, Lahore54782. Sun .
"Shearfree axial model in massive Brans–Dicke gravity". United States.
doi:10.1016/J.AOP.2016.10.024.
@article{osti_22617449,
title = {Shearfree axial model in massive Brans–Dicke gravity},
author = {Sharif, M., Email: msharif.math@pu.edu.pk and Manzoor, Rubab, Email: rubab.manzoor@umt.edu.pk and Department of Mathematics, University of Management and Technology, Johar Town Campus, Lahore54782},
abstractNote = {This paper explores the influences of dark energy on the shearfree axially symmetric evolution by considering selfinteracting Brans–Dicke gravity as a dark energy candidate. We describe energy source of the model and derive all the effective dynamical variables as well as effective structure scalars. It is found that scalar field is one of the sources of anisotropy and dissipation. The resulting effective structure scalars help to study the dynamics associated with dark energy in any axial configuration. In order to investigate shearfree evolution, we formulate a set of governing equations along with heat transport equation. We discuss consequences of shearfree condition upon different SBD fluid models like dissipative nongeodesic and geodesic models. For dissipative nongeodesic case, the rotational distribution turns out to be the necessary and sufficient condition for radiating model. The dissipation depends upon inhomogeneous expansion. The geodesic model is found to be irrotational and nonradiating. The nondissipative geodesic model leads to FRW model for positive values of the expansion parameter.},
doi = {10.1016/J.AOP.2016.10.024},
journal = {Annals of Physics},
number = ,
volume = 376,
place = {United States},
year = {Sun Jan 15 00:00:00 EST 2017},
month = {Sun Jan 15 00:00:00 EST 2017}
}

PPN parameter {gamma} and solar system constraints of massive BransDicke theories
Previous solar system constraints of the BransDicke (BD) parameter {omega} have either ignored the effects of the scalar field potential (mass terms) or assumed a highly massive scalar field. Here, we interpolate between the above two assumptions and derive the solar system constraints on the BD parameter {omega} for any field mass. We show that for {omega}=O(1) the solar system constraints relax for a field mass m > or approx. 20xm{sub AU}=20x10{sup 27} GeV.