Simulations of inspiraling and merging double neutron stars using the Spectral Einstein Code
Abstract
We present results on the inspiral, merger, and postmerger evolution of a neutron star-neutron star (NSNS) system. Our results are obtained using the hybrid pseudospectral-finite volume Spectral Einstein Code (SpEC). To test our numerical methods, we evolve an equal-mass system for ≈22 orbits before merger. This waveform is the longest waveform obtained from fully general-relativistic simulations for NSNSs to date. Such long (and accurate) numerical waveforms are required to further improve semianalytical models used in gravitational wave data analysis, for example, the effective one body models. We discuss in detail the improvements to SpEC's ability to simulate NSNS mergers, in particular mesh refined grids to better resolve the merger and postmerger phases. We provide a set of consistency checks and compare our results to NSNS merger simulations with the independent bam code. We find agreement between them, which increases confidence in results obtained with either code. This work paves the way for future studies using long waveforms and more complex microphysical descriptions of neutron star matter in SpEC.
Additional Information
© 2016 American Physical Society. Received 7 April 2016. Received 7 April 2016; published 24 June 2016. We acknowledge helpful discussions with Sebastiano Bernuzzi, Michael Boyle [123], Alessandra Buonanno, M. Brett Deaton, Sarah Gossan, Tanja Hinderer, Kenta Kiuchi, Luis Lehner, Geoffrey Lovelace, Maria Okounkova, David Radice, Jocelyn Read, Masaru Shibata, Nick Tacik, and members of our Simulating eXtreme Spacetimes (SXS) collaboration (http://www.black‑holes.org). This research is partially supported by NSF Grants No. PHY-1068881, No. CAREER PHY-1151197, No. PHY-1306125, No. PHY-1404569, No. PHY-1402916, No. AST- 1205732, No. AST-1333129, and No. AST-1333520; by the Alfred P. Sloan Foundation; by the Max-Planck Society; by the Sherman Fairchild Foundation; and by the International Research Unit of Advanced Future Studies, Kyoto University. Support for F. F. was provided by NASA through Einstein Postdoctoral Fellowship Grant No. PF4-150122 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under Contract No. NAS8- 03060. The simulations were performed on the Caltech compute cluster Zwicky (NSF MRI Grant No. PHY- 0960291), on the Datura cluster of the AEI, on machines of the Louisiana Optical Network Initiative under Grant No. loni_numrel07, and on Stampede at TACC under NSF XSEDE allocations No. TG-PHY990007N and No. TG-PHY100033. All 2D graphs were generated with the PYTHON-based MATPLOTLIB [124] and IPYTHON [125] packages. VISIT [126,127] was used for 3D and 2D sliced plots. This paper has been assigned Yukawa Institute for Theoretical Physics Report No. YITP-16-39.Attached Files
Published - PhysRevD.93.124062.pdf
Submitted - 1604.00782v1.pdf
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Additional details
- Eprint ID
- 68695
- Resolver ID
- CaltechAUTHORS:20160627-150704335
- PHY-1068881
- NSF
- PHY-1151197
- NSF CAREER
- PHY-1306125
- NSF
- PHY-1404569
- NSF
- PHY-1402916
- NSF
- AST- 1205732
- NSF
- AST-1333129
- NSF
- AST-1333520
- NSF
- Alfred P. Sloan Foundation
- Max-Planck Society
- Sherman Fairchild Foundation
- International Research Unit of Advanced Future Studies
- Kyoto University
- PF4-150122
- NASA Einstein Postdoctoral Fellowship
- NAS8- 03060
- NASA
- PHY- 0960291
- NSF MRI
- loni_numrel07
- Louisiana Optical Network Initiative
- TG-PHY990007N
- NSF XSEDE
- TG-PHY100033
- NSF XSEDE
- Created
-
2016-06-28Created from EPrint's datestamp field
- Updated
-
2021-11-11Created from EPrint's last_modified field
- Caltech groups
- TAPIR