Static Orbits in Rotating Spacetimes

Collodel, Lucas G.; Kleihaus, Burkhard; Kunz, Jutta

doi:10.1103/physrevlett.120.201103

Cited by 32 publications

(33 citation statements)

References 26 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For a distant observer, this shell would look like a shadow similar to that of a black hole. The existence of static degenerated orbits in other spacetimes is considered in [38][39][40][41]. We note also that in SFNS spacetimes, as opposed to black holes, a freely moving massive particle with E ≥ 1 will inevitably escape to infinity, while such a particle with E < 1 will move on a bound geodesic; thus the value E = 1 separates bound and unbound orbits.…”

Section: Bound Orbitsmentioning

confidence: 95%

“…Thus, a bound orbit of the general type oscillates near a stable circular orbit (an oscillation is the motion from pericentre to apocentre and back) and ϕ osc is the angle between any two successive pericentre points of the orbit. The relativistic precession of pericentres of bound orbits is considered in [1,5,11,[40][41][42][43][44] both from a purely theoretical point of view and in the context of observations of S-stars in the Galactic Centre. If a massive test particle moves radially in some nonstatic degenerate orbit, which will be the case if J = 0 and A(r 0 ) < E 2 < 1, then ∆ ϕ = −2π.…”

Section: Bound Orbitsmentioning

confidence: 99%

See 1 more Smart Citation

Bound orbits near scalar field naked singularities

2019

View full text Add to dashboard Cite

We study bound orbits near the centres of static, spherically symmetric, asymptotically flat configurations of a self-gravitating scalar field minimally coupled to gravity. In our approach, a nonlinear scalar field is considered as an idealized model of dark matter, and the main examples that we have in mind are the centres of galaxies. We consider both scalar field black holes (SFBHs) and scalar field naked singularities (SFNSs). It turns out that the shape and parameters of a bound orbit depend crucially on the type of configuration. The lapse metric function of a SFNS and, consequently, the effective potential of a massive test particle with zero angular momentum have a global minimum. A SFNS has a static degenerated orbit on which a test particle, having zero angular momentum and the minimum of its energy, remains at rest at all times. This implies that there exists a spherical shell consisting of cold gas or dust, which for a distant observer can look like the shadow of a black hole. We also study the shape of noncircular bound orbits close to the centres of SFNSs and show that their angles of precession are negative.

show abstract

Section: Bound Orbitsmentioning

confidence: 95%

Section: Bound Orbitsmentioning

confidence: 99%

Bound orbits near scalar field naked singularities

2019

View full text Add to dashboard Cite

show abstract

“…In [58] is was shown that in stationary rotating spacetimes static orbits in the equatorial plane may exist. On this kind of orbit a particle stays at rest relative to an observer in the asymptotic region when it was at rest initially.…”

Section: G Ergosurface and Static Orbitsmentioning

confidence: 99%

“…The necessary and sufficient condition for a static orbit is that g tt possesses a local maximum (stable) or a local minimum (unstable) in some region where g tt < 0. It was demonstrated in [58] that static orbits exist for rotating boson stars and wormholes immersed in rotating matter. For symmetric wormhole solutions considered in this work g tt always is extremal at the throat.…”

Section: G Ergosurface and Static Orbitsmentioning

confidence: 99%

Rotating wormhole solutions with a complex phantom scalar field

et al. 2019

Self Cite

View full text Add to dashboard Cite

show abstract

“…One of the most impressive recent examples in this context represents the discovery of hairy black holes based on boson stars [16,17]. Another recent surprise was the realization that rotating boson stars allow for static orbits [18].…”

Section: Introductionmentioning

confidence: 99%

Phase diagrams of charged compact boson stars

Kumar

Kulshreshtha

et al. 2019

Eur. Phys. J. C

Self Cite

View full text Add to dashboard Cite

Compact boson stars, whose scalar field vanishes identically in the exterior region, arise in a theory involving a massless complex scalar field with a conical potential, when coupled to gravity. Their charged compact generalizations, obtained in the presence of a U(1) gauge field, exhibit further interesting features. On the one hand, charged compact boson shells can arise, whose scalar field vanishes also in the central region, while on the other hand, the domain of existence of charged compact boson stars exhibits bifurcation points. First 2D phase diagrams have been studied before. Here we extend these earlier studies to a larger range of the variables and study additional phase diagrams. We then extend these studies to obtain 3D phase diagrams and present these with a detailed discussion of their various regions with respect to the bifurcation points and argue, that there is an infinite series of such bifurcation points. Thus the theory is seen to contain rich physics in a particular domain of the phase diagrams. We also discuss the dependence of the fields on the dimensionless radial coordinate for some representative points of the phase trajectories in the phase diagrams of the theory.

show abstract

Static Orbits in Rotating Spacetimes

Cited by 32 publications

References 26 publications

Bound orbits near scalar field naked singularities

Bound orbits near scalar field naked singularities

Rotating wormhole solutions with a complex phantom scalar field

Phase diagrams of charged compact boson stars

Contact Info

Product

Resources

About