Quartically self-interacting massive boson stars are stable only up to the first mass maximum; their head-on mergers yield a boson-star remnant, a black hole at contact, or two black holes formed before contact, with radiated energy varying non-monotonically at strong coupling.
Gravitational wave extraction in higher dimensional numerical relativity using the Weyl tensor
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abstract
Gravitational waves are one of the most important diagnostic tools in the analysis of strong-gravity dynamics and have been turned into an observational channel with LIGO's detection of GW150914. Aside from their importance in astrophysics, black holes and compact matter distributions have also assumed a central role in many other branches of physics. These applications often involve spacetimes with $D>4$ dimensions where the calculation of gravitational waves is more involved than in the four dimensional case, but has now become possible thanks to substantial progress in the theoretical study of general relativity in $D>4$. Here, we develop a numerical implementation of the formalism by Godazgar and Reall (Ref.[1]) -- based on projections of the Weyl tensor analogous to the Newman-Penrose scalars -- that allows for the calculation of gravitational waves in higher dimensional spacetimes with rotational symmetry. We apply and test this method in black-hole head-on collisions from rest in $D=6$ spacetime dimensions and find that a fraction $(8.19\pm 0.05)\times 10^{-4}$ of the Arnowitt-Deser-Misner mass is radiated away from the system, in excellent agreement with literature results based on the Kodama-Ishibashi perturbation technique. The method presented here complements the perturbative approach by automatically including contributions from all multipoles rather than computing the energy content of individual multipoles.
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gr-qc 3representative citing papers
Chain-like transients in boson star collisions are controlled by a timing window set by matching binary collision time to the isolated breathing clock rather than excitation level alone.
Using an existing numerical-relativity catalogue, the paper builds a branch-conditioned neural reconstruction model that infers boson-star merger outcomes from waveform morphology by comparing reconstruction quality across candidate hypotheses.
citing papers explorer
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Massive boson stars: Stability and GW emission in head-on mergers
Quartically self-interacting massive boson stars are stable only up to the first mass maximum; their head-on mergers yield a boson-star remnant, a black hole at contact, or two black holes formed before contact, with radiated energy varying non-monotonically at strong coupling.
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Timing-Window Mechanism for Chain-Like Transients in Collisions of Radially Excited Boson Stars
Chain-like transients in boson star collisions are controlled by a timing window set by matching binary collision time to the isolated breathing clock rather than excitation level alone.
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Massive boson stars: Waveform-based branch diagnosis with neural reconstruction
Using an existing numerical-relativity catalogue, the paper builds a branch-conditioned neural reconstruction model that infers boson-star merger outcomes from waveform morphology by comparing reconstruction quality across candidate hypotheses.