Efficient vectorizable PDE solvers

Schönauer, Willi; Weiβ, R.

doi:10.1016/0377-0427(89)90371-3

Cited by 167 publications

(142 citation statements)

References 4 publications

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“…The LORENE class ScalarBH used for generating GYOTO-compatible metrics from the KBHsSH raw data is publicly available in the latest version of LORENE. We remark that in preparing the framework for this study, we have compared rotating boson star solutions numerically generated by the KADATH code [39] in [31] with those generated by the code used in [13], FIDISOL/CADSOL [40], finding a very good agreement.…”

Section: Ray-tracing Setup and Shadow Computationsmentioning

confidence: 75%

Astrophysical imaging of Kerr black holes with scalar hair

et al. 2016

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We address the astrophysical imaging of a family of deformed Kerr black holes (BHs). These are stationary, asymptotically flat BH spacetimes that are solutions of general relativity minimally coupled to a massive, complex scalar field: Kerr BHs with scalar hair (KBHsSH). Such BHs bifurcate from the vacuum Kerr solution and can be regarded as a horizon within a rotating boson star. In a recent letter [P. V. P. Cunha, C. A. R. Herdeiro, E. Radu, and H. F. Rúnarsson, Phys. Rev. Lett. 115, 211102 (2015).], it was shown that KBHsSH can exhibit very distinct shadows from the ones of their vacuum counterparts. The setup therein, however, considers the light source to be a celestial sphere sufficiently far away from the BH. Here, we analyze KBHsSH surrounded by an emitting torus of matter simulating a more realistic astrophysical environment, and study the corresponding lensing of light as seen by a very faraway observer, to appropriately model ground-based observations of Sgr A Ã . We find that the differences in imaging between KBHsSH and comparable vacuum Kerr BHs remain, albeit less dramatic than those observed for the corresponding shadows in the previous setup. In particular, we highlight two observables that might allow differentiating KBHsSH and Kerr BHs. The first is the angular size of the photon ring (in a Kerr spacetime) or lensing ring (in a KBHSH spacetime), the latter being significantly smaller for sufficiently non-Kerr-like spacetimes. The second is the existence of an edge in the intensity distribution (the photon ring in Kerr spacetime). This edge can disappear for very non-Kerr-like KBHsSH. It is plausible, therefore, that sufficiently precise very long baseline interferometric observations of BH candidates can constrain this model.

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Section: Ray-tracing Setup and Shadow Computationsmentioning

confidence: 75%

Astrophysical imaging of Kerr black holes with scalar hair

et al. 2016

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“…However, errors increase dramatically when studying solutions close to central inspiralling region of the BSs curve, see Figure 4 below (left panel). A detailed description of the numerical method and explicit examples are provided in [58].…”

Section: Numerical Implementationmentioning

confidence: 99%

“…All numerical calculations have been performed by using the professional package fidisol/cadsol [58], which uses a finite difference method with an arbitrary grid and arbitrary consistency order. This package has been extensively tested in the past by recovering numerous exact solutions in general relativity and field theory.…”

Section: Numerical Implementationmentioning

confidence: 99%

Construction and physical properties of Kerr black holes with scalar hair

Herdeiro

Radu

2015

Class. Quantum Grav.

267

374

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Kerr black holes with scalar hair are solutions of the Einstein-Klein-Gordon field equations describing regular (on and outside an event horizon), asymptotically flat black holes with scalar hair [1]. These black holes interpolate continuously between the Kerr solution and rotating boson stars in D = 4 spacetime dimensions. Here we provide details on their construction, discussing properties of the ansatz, the field equations, the boundary conditions and the numerical strategy. Then, we present an overview of the parameter space of the solutions, and describe in detail the space-time structure of the black holes exterior geometry and of the scalar field for a sample of reference solutions. Phenomenological properties of potential astrophysical interest are also discussed, and the stability properties and possible generalizations are commented on. As supplementary material to this paper we make available numerical data files for the sample of reference solutions discussed, for public use. * herdeiro@ua.pt † eugen.radu@ua.pt 1 arXiv:1501.04319v2 [gr-qc] 4 May 2015

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“…This has been done using the Partial differential equation solver FIDISOL [26]. We have mapped the infinite interval of the r coordinate …”

Section: Rotating Solutionsmentioning

confidence: 99%

Symmetry breaking in (gravitating) scalar field models describing interacting boson stars andQ-balls

et al. 2009

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We investigate the properties of interacting Q-balls and boson stars that sit on top of each other in great detail. The model that describes these solutions is essentially a (gravitating)two-scalar field model where both scalar fields are complex. We construct interacting Qballs or boson stars with arbitrarily small charges but finite mass. We observe that in the interacting case -where the interaction can be either due to the potential or due to gravitytwo types of solutions exist for equal frequencies: one for which the two scalar fields are equal, but also one for which the two scalar fields differ. This constitutes a symmetry breaking in the model. While for Q-balls asymmetric solutions have always corresponding symmetric solutions and are thus likely unstable to decay to symmetric solutions with lower energy, there exists a parameter regime for interacting boson stars, where only asymmetric solutions exist. We present the domain of existence for two interacting non-rotating solutions as well as for solutions describing the interaction between rotating and non-rotating Q-balls and boson stars, respectively.

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Efficient vectorizable PDE solvers

Cited by 167 publications

References 4 publications

Astrophysical imaging of Kerr black holes with scalar hair

Astrophysical imaging of Kerr black holes with scalar hair

Construction and physical properties of Kerr black holes with scalar hair

Symmetry breaking in (gravitating) scalar field models describing interacting boson stars andQ-balls

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