Critical collapse of a rotating scalar field in dimensions
Feb 15, 201717 pages
Published in:
- Phys.Rev.D 95 (2017) 8, 084001
- Published: Apr 3, 2017
e-Print:
- 1702.04601 [gr-qc]
View in:
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Abstract: (APS)
We carry out numerical simulations of the collapse of a complex rotating scalar field of the form Ψ(t,r,θ)=eimθΦ(t,r), giving rise to an axisymmetric metric, in 2+1 spacetime dimensions with cosmological constant Λ<0, for m=0, 1, 2, for four one-parameter families of initial data. We look for the familiar scaling of black hole mass and maximal Ricci curvature as a power of |p-p*|, where p is the amplitude of our initial data and p* some threshold. We find evidence of Ricci scaling for all families, and tentative evidence of mass scaling for most families, but the case m>0 is very different from the case m=0 we have considered before: the thresholds for mass scaling and Ricci scaling are significantly different (for the same family); scaling stops well above the scale set by Λ, and the exponents depend strongly on the family. Hence, in contrast to the m=0 case, and to many other self-gravitating systems, there is only weak evidence for the collapse threshold being controlled by a self-similar critical solution and no evidence for it being universal.Note:
- Version accepted for publication in PRD
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