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Extending superposed harmonic initial data to higher spin

Ma, Sizheng and Giesler, Matthew and Scheel, Mark A. and Varma, Vijay (2021) Extending superposed harmonic initial data to higher spin. Physical Review D, 103 (8). Art. No. 084029. ISSN 2470-0010. doi:10.1103/PhysRevD.103.084029.

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Numerical simulations of binary black holes are accompanied by an initial spurious burst of gravitational radiation (called “junk radiation”) caused by a failure of the initial data to describe a snapshot of an inspiral that started at an infinite time in the past. A previous study showed that the superposed harmonic (SH) initial data give rise to significantly smaller junk radiation. However, it is difficult to construct SH initial data for black holes with dimensionless spin χ≳0.7. We here provide a class of spatial coordinate transformations that extend SH to higher spin. The new spatial coordinate system, which we refer to as superposed modified harmonic (SMH), is characterized by a continuous parameter—Kerr-Schild and harmonic spatial coordinates are only two special cases of this new gauge. We compare SMH with the superposed Kerr-Schild initial data by evolving several binary black hole systems with χ=0.8 and 0.9. We find that the new initial data still lead to less junk radiation and only small changes of black hole parameters (e.g., mass and spin). We also find that the volume-weighted constraint violations for the new initial data converge with resolution during the junk stage (t≲700M), which means there are fewer high-frequency components in waveforms at outer regions.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Ma, Sizheng0000-0002-4645-453X
Giesler, Matthew0000-0003-2300-893X
Scheel, Mark A.0000-0001-6656-9134
Varma, Vijay0000-0002-9994-1761
Additional Information:© 2021 American Physical Society. Received 12 February 2021; accepted 2 April 2021; published 20 April 2021. We thank Maria Okounkova, Saul Teukolsky, and Harald Pfeiffer for useful discussions. M. G. is supported in part by National Science Foundation (NSF) Grant No. PHY-1912081 at Cornell. M. A. S. and S. M. are supported by NSF Grants No. PHY-2011961, No. PHY-2011968, and No. OAC-1931266 at Caltech. V. V. is supported by a Klarman fellowship at Cornell. M. G. and V. V. were supported by NSF Grants No. PHY-170212 and No. PHY-1708213 at Caltech. S. M., M. G., M. A. S., and V. V. are supported by the Sherman Fairchild Foundation. The computations presented here were conducted on the Caltech High Performance Cluster, partially supported by a grant from the Gordon and Betty Moore Foundation. This work was supported in part by NSF Grants No. PHY-1912081 and No. OAC-1931280 at Cornell.
Funding AgencyGrant Number
Cornell UniversityUNSPECIFIED
Sherman Fairchild FoundationUNSPECIFIED
Gordon and Betty Moore FoundationUNSPECIFIED
Issue or Number:8
Record Number:CaltechAUTHORS:20210406-150448157
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:108638
Deposited By: Tony Diaz
Deposited On:07 Apr 2021 17:05
Last Modified:21 Apr 2021 21:16

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