Boson stars in 
<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>f</mml:mi><mml:mo stretchy="false">(</mml:mo><mml:mi>T</mml:mi><mml:mo stretchy="false">)</mml:mo></mml:math>
 extended theory of gravity

Ilijić, Saša; Sossich, Marko

doi:10.1103/physrevd.102.084019

Cited by 19 publications

(17 citation statements)

References 59 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In f (T)-gravity, only few non-vacuum solutions are known. These usually are encountered in the context of anisotropic matter and Boson stars [39][40][41]. Furthermore, studies of solutions sourced by a non-linear electromagnetic field exist [42].…”

Section: Introductionmentioning

confidence: 99%

Static Spherically Symmetric Black Holes in Weak f(T)-Gravity

Pfeifer

Schuster

2021

Universe

View full text Add to dashboard Cite

With the advent of gravitational wave astronomy and first pictures of the “shadow” of the central black hole of our milky way, theoretical analyses of black holes (and compact objects mimicking them sufficiently closely) have become more important than ever. The near future promises more and more detailed information about the observable black holes and black hole candidates. This information could lead to important advances on constraints on or evidence for modifications of general relativity. More precisely, we are studying the influence of weak teleparallel perturbations on general relativistic vacuum spacetime geometries in spherical symmetry. We find the most general family of spherically symmetric, static vacuum solutions of the theory, which are candidates for describing teleparallel black holes which emerge as perturbations to the Schwarzschild black hole. We compare our findings to results on black hole or static, spherically symmetric solutions in teleparallel gravity discussed in the literature, by comparing the predictions for classical observables such as the photon sphere, the perihelion shift, the light deflection, and the Shapiro delay. On the basis of these observables, we demonstrate that among the solutions we found, there exist spacetime geometries that lead to much weaker bounds on teleparallel gravity than those found earlier. Finally, we move on to a discussion of how the teleparallel perturbations influence the Hawking evaporation in these spacetimes.

show abstract

Section: Introductionmentioning

confidence: 99%

Static Spherically Symmetric Black Holes in Weak f(T)-Gravity

Pfeifer

Schuster

2021

Universe

View full text Add to dashboard Cite

show abstract

“…1). Although other theories of gravity may also depart from this spiral pattern [36,40,44], the model considered here is peculiar because the range over which solutions are possible is relatively small, which could facilitate its observational discrimination. Though our focus was on analyzing canonical boson stars coupled to f (R) gravity, the fact is that our computational method forced us to construct boson star solutions in GR coupled to unconventional matter [see Eq.…”

Section: Discussionmentioning

confidence: 97%

“…The traditional approach assumes that the space-time is a Riemannian structure completely described by the metric tensor. But one can also consider a metric-affine ge-ometry with a priori independent metric and affine structures [33,41,42] (for an analysis of boson stars in theories with torsion of the f (T ) type, see [44]). Given that we have no compelling evidence about the kind of geometry associated to the space-time, it seems fair not to discriminate any of (at least) those options a priori.…”

Section: Introductionmentioning

confidence: 99%

Boson stars in Palatini $f(\mathcal{R})$ gravity

Masó-Ferrando,

Sanchis-Gual,

Font

et al. 2021

Preprint

View full text Add to dashboard Cite

We explore equilibrium solutions of spherically symmetric boson stars in the Palatini formulation of f (R) gravity. We account for the modifications introduced in the gravitational sector by using a recently established correspondence between modified gravity with scalar matter and general relativity with modified scalar matter. We focus on the quadratic theory f (R) = R + ξR 2 and compare its solutions with those found in general relativity, exploring both positive and negative values of the coupling parameter ξ. As matter source, a complex, massive scalar field with and without self-interaction terms is considered. Our results show that the existence curves of boson stars in Palatini f (R) gravity are fairly similar to those found in general relativity. Major differences are observed for negative values of the coupling parameter which results in a repulsive gravitational component for high enough scalar field density distributions. Adding self-interactions makes the degeneracy between f (R) and general relativity even more pronounced, leaving very little room for observational discrimination between the two theories.

show abstract

“…Notice that the above equation is just like the one of TOV GR. In [18], the authors also adopted equation ( 6) from GR. However, recall that the calculation of mass in f (T ) gravity is an open problem (see, e.g., [19] and [20]).…”

Section: Basic Equationsmentioning

confidence: 99%

Solving Tolman-Oppenheimer-Volkoff equations in f(T) gravity: a novel approach applied to some realistic equations of state

Araújo¹,

Fortes²

2021

Preprint

View full text Add to dashboard Cite

There are many ways to probe alternative theories of gravity, namely, via: experimental tests at solar system scale, cosmological data and models, gravitational waves and compact objects. In the present paper we consider a model of gravity with torsion f (T ) applied to compact objects such as neutron stars (NSs) for a couple of realistic equations of state (EOS). To do so we follow our previous articles, in which we show how to model compact stars in this f (T ) gravity by obtaining its corresponding Tolman-Oppenheimer-Volkof equations and applying this prescription to model polytropic compact stars. In these modelling of NS in f (T ) gravity presented here, we calculate, among other things, the maximum mass allowed for a given realistic EOS, which would also allow us to evaluate which models are in accordance with observations. The results already known to General Relativity must be reproduced to some extent and, eventually, we can find models that allow higher maximum masses for NSs than Relativity itself, which could explain, for example, the secondary component of the event GW190814, if this star is a massive NS.

show abstract

Boson stars in f(T) extended theory of gravity

Cited by 19 publications

References 59 publications

Static Spherically Symmetric Black Holes in Weak f(T)-Gravity

Static Spherically Symmetric Black Holes in Weak f(T)-Gravity

Boson stars in Palatini $f(\mathcal{R})$ gravity

Solving Tolman-Oppenheimer-Volkoff equations in f(T) gravity: a novel approach applied to some realistic equations of state

Contact Info

Product

Resources

About