SACRA Gravitational Waveform Data Bank

This repository contains all publicly available SACRA gravitational waveforms for binary neutron star mergers. All the waveforms for Ψ4 are provided at several fixed extraction radii and those for h are extrapolated to future null infinity. For all the runs, waveforms are provided at 6 grid resolutions, e.g., N=182, 150, 130, 110, 102, and 90. N=182 is a higher resolution than N = 90.

Reference paper

Our most recent paper is available at arxiv:1907.03790. This paper illustrates our methods, parameter space of binary neutron stars, and estimation of our waveform accuracies. See also arxiv:1708.08926 and 1802.06518.

Caveats

  1. All the waveforms are provided with c=G=Msun=1 unit.
  2. All the waveforms are provided for the l=2, m=2 mode.
The data in this catalog are free for anyone to use, but we request that you please acknowledge the first scientific publication of each simulation. We may provide the simulation data for the ejecta, the remnant, and etc. Please contact to the first author of the corresponding papers.

Proceed to Data Bank

File format

  1. Ψ4 data
    2. Ψ4 data are provided with file names in the format of psi4_*_l2m2, where * denotes the extraction radius in the unit of Msun.
    Data are contained in files in the next format:
    • The 1st column: the simulation time
    • The 2nd column: the real part of Ψ4,22
    • The 3rd column: the imaginary part of Ψ4,22
  2. h data
    3. h data are provided with file names in the format of h_*l2m2, where * denotes the extraction radius in the unit of Msun. h is calculated from Ψ4 data employing fixed frequency method [1] and are extrapolated to future null infinity employing the method of [2] (please see arxiv:1708.08926, 1802.06518, or 1907.03790 for more details).
    Data are contained in files in the next format:
    • The 1st column: the retarded time
    • The 2nd column: the real part of h22 D
    • The 3rd column: the imaginary part of h22 D
    Here, D is an approximate proper area of the extraction radius (please see arxiv :1907.03790 for more details).

references

  1. C. Reisswig and D. Pollney, Class. Quant. Grav. 28,195015 (2011); arXiv:1006.1632
  2. H. Nakano, Class. Quantum. Grav. 32, 177002 (2015); arXiv:1501.02890