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  Black-Hole Neutron Star Simulations with the BAM code: First Tests and Simulations

Chaurasia, S. V., Dietrich, T., & Rosswog, S. (2021). Black-Hole Neutron Star Simulations with the BAM code: First Tests and Simulations. Physical Review D, 104: 084010. doi:10.1103/PhysRevD.104.084010.

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 Creators:
Chaurasia, Swami Vivekanandji, Author
Dietrich, Tim1, 2, Author              
Rosswog, Stephan, Author
Affiliations:
1Multi-messenger Astrophysics of Compact Binaries, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_3329942              
2Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, Golm, DE, ou_1933290              

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Free keywords: General Relativity and Quantum Cosmology, gr-qc, Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE, Physics, Computational Physics, physics.comp-ph
 Abstract: The first detections of black hole - neutron star mergers (GW200105 and GW200115) by the LIGO-Virgo-Kagra Collaboration mark a significant scientific breakthrough. The physical interpretation of pre- and post-merger signals requires careful cross-examination between observational and theoretical modelling results. Here we present the first set of black hole - neutron star simulations that were obtained with the numerical-relativity code BAM. Our initial data are constructed using the public LORENE spectral library which employs an excision of the black hole interior. BAM, in contrast, uses the moving-puncture gauge for the evolution. Therefore, we need to ``stuff'' the black hole interior with smooth initial data to evolve the binary system in time. This procedure introduces constraint violations such that the constraint damping properties of the evolution system are essential to increase the accuracy of the simulation and in particular to reduce spurious center-of-mass drifts. Within BAM we evolve the Z4c equations and we compare our gravitational-wave results with those of the SXS collaboration and results obtained with the SACRA code. While we find generally good agreement with the reference solutions and phase differences $\lesssim 0.5$ rad at the moment of merger, the absence of a clean convergence order in our simulations does not allow for a proper error quantification. We finally present a set of different initial conditions to explore how the merger of black hole neutron star systems depends on the involved masses, spins, and equations of state.

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 Dates: 2021-07-192021
 Publication Status: Published in print
 Pages: 14 pages, 10 figures
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 Table of Contents: -
 Rev. Type: -
 Identifiers: arXiv: 2107.08752
DOI: 10.1103/PhysRevD.104.084010
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Title: Physical Review D
  Other : Phys. Rev. D.
Source Genre: Journal
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Publ. Info: Lancaster, Pa. : American Physical Society
Pages: - Volume / Issue: 104 Sequence Number: 084010 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: https://pure.mpg.de/cone/journals/resource/111088197762258