Geodesic motion in the space-time of a noncompact boson star

Diemer, Valeria; Eilers, Keno; Hartmann, Betti; Schaffer, Isabell; Toma, Catalin

doi:10.1103/physrevd.88.044025

Cited by 34 publications

(32 citation statements)

References 69 publications

(92 reference statements)

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“…For instance, there may also be solutions which mimic compact astrophysical objects like neutron stars or black holes. These solutions could be studied in the context of gravitational lensing [28][29][30], with respect to their light curves [22], their geodesics [31], etc.…”

Section: Discussionmentioning

confidence: 99%

Spontaneous symmetry breaking in wormholes spacetimes with matter

et al. 2017

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When bosonic matter in the form of a complex scalar field is added to Ellis wormholes, the phenomenon of spontaneous symmetry breaking is observed. Symmetric solutions possess full reflection symmetry with respect to the radial coordinate of the two asymptotically flat spacetime regions connected by the wormhole, whereas asymmetric solutions do not possess this symmetry. Depending on the size of the throat, at bifurcation points pairs of asymmetric solutions arise from or merge with the symmetric solutions. These asymmetric solutions are energetically favoured. When the backreaction of the boson field is taken into account, this phenomenon is retained. Moreover, in a certain region of the solution space both symmetric and asymmetric solutions exhibit a transition from single throat to double throat configurations.

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Section: Discussionmentioning

confidence: 99%

Spontaneous symmetry breaking in wormholes spacetimes with matter

et al. 2017

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“…We remark that boson stars have been suggested as BH mimickers, and studies in this context, including of the comparative phenomenology, have been report in, e.g. [53][54][55][56][57][58][59][60][61][62][63][64].…”

Section: Introductionmentioning

confidence: 99%

Iron Kα line of boson stars

Cao

Cárdenas-Avendaño

Zhou

et al. 2016

J. Cosmol. Astropart. Phys.

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Abstract. The present paper is a sequel to our previous work [Y. Ni et al., JCAP 1607, 049 (2016] in which we studied the iron Kα line expected in the reflection spectrum of Kerr black holes with scalar hair. These metrics are solutions of Einstein's gravity minimally coupled to a massive, complex scalar field. They form a continuous bridge between a subset of Kerr black holes and a family of rotating boson stars depending on one extra parameter, the dimensionless scalar hair parameter q, ranging from 0 (Kerr black holes) to 1 (boson stars). Here we study the limiting case q = 1, corresponding to rotating boson stars. For comparison, spherical boson stars are also considered. We simulate observations with XIS/Suzaku. Using the fact that current observations are well fit by the Kerr solution and thus requiring that acceptable alternative compact objects must be compatible with a Kerr fit, we find that some boson star solutions are relatively easy to rule out as potential candidates to explain astrophysical black holes, while other solutions, which are neither too dilute nor too compact are more elusive and we argue that they cannot be distinguished from Kerr black holes by the analysis of the iron line with current X-ray facilities.

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“…5). However, as mentioned before this is never the case in boson-star metrics [Diemer et al, 2013, Grandclément et al, 2014. On the right panel of Fig.…”

Section: Orbits With L = 1 Mmentioning

confidence: 57%

Comparing timelike geodesics around a Kerr black hole and a boson star

Grould

Méliani

Vincent

et al. 2017

Class. Quantum Grav.

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Abstract. The second-generation beam combiner at the Very Large Telescope (VLT), GRAVITY, observes the stars orbiting the compact object located at the center of our galaxy, with an unprecedented astrometric accuracy of 10 µas. The nature of this compact source is still unknown since black holes are not the only candidates explaining the four million solar masses at the Galactic center. Boson stars are such an alternative model to black holes. This paper focuses on the study of trajectories of stars orbiting a boson star and a Kerr black hole. We put in light strong differences between orbits obtained in both metrics when considering stars with sufficiently close pericenters to the compact object, typically 30 M . Discovery of closer stars to the Galactic center than the S2 star by the GRAVITY instrument would thus be a powerful tool to possibly constrain the nature of the central source.

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Geodesic motion in the space-time of a noncompact boson star

Cited by 34 publications

References 69 publications

Spontaneous symmetry breaking in wormholes spacetimes with matter

Spontaneous symmetry breaking in wormholes spacetimes with matter

Iron Kα line of boson stars

Comparing timelike geodesics around a Kerr black hole and a boson star

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