Wormhole geometries supported by three-form fields

Barros, Bruno J.; Lobo, Francisco S. N.

doi:10.1103/physrevd.98.044012

Cited by 36 publications

(40 citation statements)

References 52 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We also should understand if the physics of a linkage between Equation (33) and Equation (34) play a role as well. 6) Finally, and not least is to see if our feed into Equation (33) to Equation (34) and linkages to Figure 1, have in their genesis, the methodologies discussed in [34], i.e. as brought up in Phase transitions and the renormalization group as brought up by Jean-Zinn-Justin, which has a very interesting discussion of the Nancy Kerrigan problem, i.e.…”

Section: )mentioning

confidence: 99%

“…4) Should there be a linkage between an initial worm hole style start to the formation of the observable universe, as a compliment to the big bank/inflation metrics, the author strongly recommends a review of the article given by Bruno J. Barros and Francisco S. N. Lobo as to relevant Wormhole geometry [33], and the question of negative energy states in a wormhole threat. If as may be the case in nonsingular starts to the expansion of the universe, negative energy states make an appearance, this may be a clue as to what is called f(R) geometries which in turn may have relevance to some of the polarization states in [32].…”

Section: And What About Polarization States Especially If We Have Mamentioning

confidence: 99%

See 1 more Smart Citation

We Begin with a “Trivial” Condition on Massive Gravitons, and Use That to Examine Nonsingular Starts to Inflation, for GW, with GW Strength and Possible Polarization States?

Beckwith¹

2020

JHEPGC

View full text Add to dashboard Cite

Our Methodology is to construct using a "trivial" solution to massive gravitons, and a nonsingular start for expansion of the universe. Our methodology has many unintended consequences, not the least is a relationship between a small time step, t, the minimum scale factor and even the tension or property values of the initial space-time wall, and that is a consequence of a "trivial" solution taking into account "massive" gravitons. I.e. this solution has a mass How to cite this paper: Beckwith, A.W.

show abstract

Section: )mentioning

confidence: 99%

Section: And What About Polarization States Especially If We Have Mamentioning

confidence: 99%

We Begin with a “Trivial” Condition on Massive Gravitons, and Use That to Examine Nonsingular Starts to Inflation, for GW, with GW Strength and Possible Polarization States?

Beckwith¹

2020

JHEPGC

View full text Add to dashboard Cite

show abstract

“…[41], to obtain spherically symmetric solutions. Some of these solutions can be interpreted as black holes by identifying the existence of event horizons (wormhole solutions were also found in [42]). The others can be interpreted as naked singularities in which there is no event horizon in the spacetime.…”

Section: Regular Black Hole Supported By 3-formmentioning

confidence: 99%

Regular black hole interior spacetime supported by three-form field

et al. 2021

View full text Add to dashboard Cite

In this paper, we show that a minimally coupled 3-form endowed with a proper potential can support a regular black hole interior. By choosing an appropriate form for the metric function representing the radius of the 2-sphere, we solve for the 3-form field and its potential. Using the obtained solution, we construct an interior black hole spacetime which is everywhere regular. The singularity is replaced with a Nariai-type spacetime, whose topology is $$\text {dS}_2 \times \text {S}^2$$ dS 2 × S 2 , in which the radius of the 2-sphere is constant. So long as the interior continues to expand indefinitely, the geometry becomes essentially compactified. The 2-dimensional de Sitter geometry appears despite the negative potential of the 3-form field. Such a dynamical compactification could shed some light on the origin of de Sitter geometry of our Universe, exacerbated by the Swampland conjecture. In addition, we show that the spacetime is geodesically complete. The geometry is singularity-free due to the violation of the null energy condition.

show abstract

“…The employment of three-form fields in gravitation was analyzed in [47], where wormhole solutions in a static and spherically symmetric spacetime continuum were explored. It was found that it is possible for the ordinary matter fields threading the wormhole to obey the classical energy conditions throughout the spacetime, while the three-form field holds the wormhole open, violating the null and weak energy conditions.…”

Section: (): V-volmentioning

confidence: 99%

Static spherically symmetric three-form stars

2021

Self Cite

View full text Add to dashboard Cite

We consider interior static and spherically symmetric solutions in a gravity theory that extends the standard Hilbert–Einstein action with a Lagrangian constructed from a three-form field $$A_{\alpha \beta \gamma }$$ A α β γ , which generates, via the field strength and a potential term, a new component in the total energy-momentum tensor of the gravitational system. We formulate the field equations in Schwarzschild coordinates and investigate their solutions numerically for different equations of state of neutron and quark matter, by assuming that the three-field potential is either a constant or possesses a Higgs-like form. Moreover, stellar models, described by the stiff-fluid, radiation-like, bag model and the Bose–Einstein condensate equations of state are explicitly obtained in both general relativity and three-form gravity, thus allowing an in-depth comparison between the astrophysical predictions of these two gravitational theories. As a general result we find that, for all the considered equations of state, three-form field stars are more massive than their general relativistic counterparts. As a possible astrophysical application, we suggest that the 2.5$$ M_{\odot }$$ M ⊙ mass compact object, associated with the GW190814 gravitational wave event, could be in fact a neutron or a quark star described by the three-form gravity theory.

show abstract

Wormhole geometries supported by three-form fields

Cited by 36 publications

References 52 publications

We Begin with a “Trivial” Condition on Massive Gravitons, and Use That to Examine Nonsingular Starts to Inflation, for GW, with GW Strength and Possible Polarization States?

We Begin with a “Trivial” Condition on Massive Gravitons, and Use That to Examine Nonsingular Starts to Inflation, for GW, with GW Strength and Possible Polarization States?

Regular black hole interior spacetime supported by three-form field

Static spherically symmetric three-form stars

Contact Info

Product

Resources

About