How Do Axisymmetric Black Holes Grow Monopole and Dipole Hair?
Abstract
We study the dynamical formation of scalar monopole and dipole hair in scalar Gauss-Bonnet theory and dynamical Chern-Simons theory. We prove that the spherically-symmetric mode of the dipole hair is completely determined by the product of the mass of the spacetime and the value of the monopole hair. We then show that the dynamics of the ℓ = 1 mode of the dipole hair is intimately tied to the appearance of the event horizon during axisymmetric collapse, which results in the radiation of certain modes that could have been divergent in the future of the collapse. We confirm these analytical predictions by simulating the gravitational collapse of a rapidly rotating neutron star in the decoupling limit, both in scalar Gauss-Bonnet and dynamical Chern-Simons theory. Our results, combined with those of Ref. [1], provide a clear physical picture of the dynamics of scalar monopole and dipole radiation in axisymmetric and spherical gravitational collapse in these theories.
Additional Information
AH and NY acknowledge support from the Simons Foundation through Award number 896696. ERM acknowledges support as John A. Wheeler Fellow at the Princeton Center for Theoretical Science, as well as postdoctoral fellowships at the Princeton Gravity Initiative, and the Institute for Advanced Study. JN is partially supported by the U.S. Department of Energy, Office of Science, Office for Nuclear Physics under Award No. DE-SC0021301. HW acknowledges support provided by NSF grants No. OAC-2004879 and No. PHY-2110416, and Royal Society (UK) Research Grant RGF\R1\180073. This work used the Extreme Science and Engineering Discovery Environment (XSEDE), through the allocation TG-PHY210114, which was supported by NSF grants No. ACI-1548562 and No. PHY-210074. This research used resources provided by the Delta research computing project, which is supported by the NSF Award No. OCI 2005572 and the State of Illinois. Delta is a joint effort of the University of Illinois at Urbana-Champaign and its National Center for Supercomputing Applications. The authors acknowledge the Texas Advanced Computing Center (TACC) at The University of Texas at Austin for providing HPC resources that have contributed to the research results reported within this paper, under LRAC grants AT21006. Part of the simulations presented in this article were performed on computational resources managed and supported by Princeton Research Computing, a consortium of groups including the Princeton Institute for Computational Science and Engineering (PICSciE) and the Office of Information Technology's High Performance Computing Center and Visualization Laboratory at Princeton University.Attached Files
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Additional details
- Eprint ID
- 121193
- Resolver ID
- CaltechAUTHORS:20230501-296691000.3
- 896696
- Simons Foundation
- Princeton University
- Institute for Advanced Study
- DE-SC0021301
- Department of Energy (DOE)
- OAC-2004879
- NSF
- PHY-2110416
- NSF
- RGF\R1\180073
- Royal Society
- TG-PHY210114
- NSF
- ACI-1548562
- NSF
- PHY-210074
- NSF
- OAC-2005572
- NSF
- State of Illinois
- AST-21006
- NSF
- Created
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2023-05-02Created from EPrint's datestamp field
- Updated
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2023-05-02Created from EPrint's last_modified field