Numerical Relativity Simulations of the Neutron Star Merger GW170817: Long-Term Remnant Evolutions, Winds, Remnant Disks, and Nucleosynthesis

We release outflow data extracted at a fixed coordinate sphere with a radius 294km. 
Material unbound according to the geodesic criterion is located in the dir 
'dynamical_ejecta/'
Material unbound according to the Bernoulli criterion, computed from the 
moment the dynamical ejecta saturates is located in the folder `spiral_wave_wind/`
Part of the `spiral_wave_wind` confined to the polar region, above 60~deg 
from the binary plane is located in `neutrino_wind/`

See [1] for more details. See also [2] for more details on 'spiral wave wind' 
and [3] for more details on dynamical ejecta.

Included data:

• `Table1.txt`: Table 1 of the paper in a machine-readable format
• `[model].tar`: ejecta data for individual simulations. The name reads as following.
  "EOS_GravMassesOfStars_NeutrinoScheme_Viscosity(LK)_Resolution".
  Simulations without viscosity do not have LK in their name. 
  Neutrino scheme is consistent in all simulations and is Leackage+M0.
  Resolutions available are: LR, SR, and HR that correspond to 246 m, 158 m and 123 m. 
• EOS tables used for the evolution (Except BLh which is not public)

For each model we provide

• Initial data generated with LORENE
• Parameter file

Additionally, we provide ejecta properties (for all ejecta types) as:

• `total_flux.dat`: angle integrated outflow rate and cumulated ejecta mass.
  Time is in seconds, masses are in solar masses.
• `hist_entropy.dat`: histogram of the ejecta as a function of the entropy (in kb)
• `hist_vel_inf.dat`: histogram of the ejecta as a function of the asymptotic velocity (in units of c)
• `hist_Y_e.dat`: histogram of the ejecta as a function of the electron fraction Ye.
• `ejecta_profile.dat`: time-integrated ejecta profiles as a function of the polar angle.
• `hist_vinf_theta.h5`: histograms of the ejecta as a function of the asymptotic velocity and the polar angle.
• `corr_Y_e_theta.h5`: histograms of the ejecta as a function of the asymptotic velocity and the polar angle.
• `ejecta.h5`: histograms of the ejecta as a function of Ye,  entropy, and expansion timescale tau.

For nucleosynthesis yields from pre-computed parametrized trajectories see [4]

[1] V. Nedora, S. Bernuzzi, D. Radice, B. Daszuta, A. Endrizzi, A. Perego, A. Prakash, M. Safarzadeh, F. Schianchi, D. Logoteta Numerical Relativity Simulations of the Neutron Star Merger GW170817: Long-Term Remnant Evolutions, Winds, Remnant Disks, and Nucleosynthesis, arXiv:2008.04333 
[2] V. Nedora, S. Bernuzzi, D. Radice, A. Perego, A. Endrizzi, N. Ortiz, Spiral-wave wind for the blue kilonova, Astrophys.J.Lett. 886 (2019), arXiv:1907.04872 
[3] S. Bernuzzi, M. Breschi, B. Daszuta, A. Endrizzi, D. Logoteta, V. Nedora, A. Perego, F. Schianchi, D. Radice, F. Zappa, I. Bombaci, N. Ortiz, Accretion-induced prompt black hole formation in asymmetric neutron star mergers, dynamical ejecta and kilonova signals, Mon.Not.Roy.Astron.Soc. 497 (2020),  arXiv:2003.06015 
[4] D. Radice, A. Perego, K. Hotokezaka, S. A. Fromm, S. Bernuzzi, and L. F. Roberts, Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis, ApJ 869:130 (2018), arXiv:1809.11161, Released data