Pith. sign in

REVIEW 1 cited by

Numerical evolution of shocks in the interior of Kerr black holes

Not yet reviewed by Pith; the record is open.

Re-run · record.json Download PDF Read on arXiv ↗

This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.

SPECIMEN: schema-true, not a live event

T0 review · schema-true

One-sentence machine reading of the paper's core claim.

pith:XXXXXXXX · record.json · timestamp

arxiv 1808.07502 v3 pith:2J3GOFSW submitted 2018-08-22 gr-qc

Paul M. Chesler , Erik Curiel , Ramesh Narayan This is my paper · ORCID
classification gr-qc
keywords exponentiallyshocksblackholesinteriorkerracceleratedamplitude
verification ladder T0 review T1 audit T2 compute T3 formal

Signed reviews

No signed human review yet.

0 comments
read the original abstract

We numerically solve Einstein's equations coupled to a scalar field in the interior of Kerr black holes. We find shock waves form near the inner horizon. The shocks grow exponentially in amplitude and need not be axisymmetric. Observers who pass through the shocks experience exponentially large tidal forces and are accelerated exponentially close to the speed of light.

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Excision and avoiding the use of boundary conditions in numerical relativity

    gr-qc 2019-08 accept novelty 5.0 of 10

    A numerical method that excises the outer computational boundary along the ingoing light cone makes boundary conditions unnecessary, at the cost of limiting evolution to about one light-crossing time of the initial grid.

Pith tools