2019-07-16T00:35:36Z
https://zenodo.org/oai2d
oai:zenodo.org:201145
2019-04-10T03:55:22Z
openaire_data
user-nrgw-opendata
Richers, Sherwood
Ott, Christian David
Abdikamalov, Ernazar
O'Connor, Evan
Sullivan, Chris
2016-12-15
Gravitational waveforms from 1824 fiducial and detailed electron capture simulations, sampled at 65535 Hz. The file is in HDF5 format, using the flags {dtype="f4",compression="gzip",shuffle=True,fletcher32=True}. Each group is contained in the "waveforms" top-level group and is named with the "A" and "omega_0" values from Equation 5 and the EOS. In each sub-group is a dataset containing timestamps in seconds (t=0 is core bounce) and a dataset containing the strain multiplied by the distance in centimeters. The values of A in kilometers, omega_0 in radians/s, and the EOS are stored as attributes of each group.
In addition, the Ye(rho) profiles are stored in the "yeofrho" top-level group. Each sub-group is labeled by the EOS used to generate the profile.
Finally, select reduced data is stored in the "reduced_data" top-level group. The following quantities are each stored as a 1824-element array, where elements of the same index from different datasets correspond to the same 2D simulation.
A(km) -- differential rotation parameter in Equation 5
D*bounce_amplitude_1(cm) -- The minimum of the first (negative) GW strain peak, multiplied by distance.
D*bounce_amplitude_2(cm) -- The maximum of the second (positive) GW strain peak, multiplied by distance.
EOS -- the equation of state used in the simulation
MbarICgrav(Msun) -- gravitational mass of the inner core, averaged over time after core bounce
Mgrav1_IC_b(Msun) -- gravitational mass of the inner core at bounce
Mrest_IC_b(Msun) -- rest mass of the inner core at bounce
SNR(aLIGOfrom10kpc) -- signal to noise ratio of the GW signal, assuming a distance of 10kpc and aLIGO sensitivity
T_c_b(MeV) -- central temperature at bounce
Ye_c_b -- central electron fraction at bounce
alpha_c_b -- central lapse at bounce
beta1_IC_b -- ratio of rotational kinetic to gravitational potential energy of the inner core at bounce
fpeak(Hz) -- frequency of the post-bounce GW oscillations
j_IC_b() -- angular momentum of the inner core at bounce
omega_0(rad|s) -- initial (pre-collapse) rotation rate used in Equation 5
omega_max(rad|s) -- maximum rotation rate achieved outside of 5km
rPNSequator_b(km) -- radius of the rho=10^11 g/ccm contour along the equator at bounce
rPNSpole_b(km) -- radius of the rho=10^11 g/ccm contour along the pole at bounce
r_omega_max(km) -- radius where omega_max occurs
rho_c_b(g|ccm) -- central density at bounce (not time averaged)
rhobar_c_postbounce(g|ccm) -- central density time averaged after bounce
s_c_b(kB|baryon) -- central entropy at bounce
t_postbounce_end(s) -- time of the end of the postbounce signal (t=0 is core bounce)
tbounce(s) -- time of core bounce (t=0 is the beginning of the simulation)
https://zenodo.org/record/201145
10.5281/zenodo.201145
oai:zenodo.org:201145
url:https://zenodo.org/communities/nrgw-opendata
info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/4.0/legalcode
gravitational wave
core-collapse supernova
Equation of State Effects on Gravitational Waves from Rotating Core Collapse
info:eu-repo/semantics/other
dataset
oai:zenodo.org:46733
2019-04-10T03:44:00Z
openaire_data
user-nrgw-opendata
Radice, David
Bernuzzi, Sebastiano
Ott, Christian D.
2016-02-29
We distribute complete gravitational-wave signals in the Advanced LIGO band (10 Hz - 8192 Hz) of the inspiral and merger of two neutron stars. These waveforms been constructed by hybridizing numerical-relativity data obtained with the WhiskyTHC code [1] with tidal effective-one-body waveforms [2,3]. More details on the procedure used to generate these waveforms are given in [4].
The waveforms are distributed as HDF5 files containing the amplitude and phase of the -2 spin-weighted spherical harmonics multipoles of the strain:
\(( h_+ - \mathrm{i} h_\times )_{l,m} = \frac{A_{l,m}}{D_{\rm cm}} \exp(-\mathrm{i} \phi_{l,m} )\)
where \(D_{\rm cm}\) is the distance in cm from the source.
The data files include a machine readable "/metadata" group with:
/metadata/EOS: name of the equation of state
/metadata/M_{A|B}: mass in isolation of star A (or B) in grams
/metadata/R_{A|B}: radius of star A (or B) in cm
/metadata/k2T: tidal coupling constant of the binary (see [3])
/metadata/kl_{A|B}: l=2,3,4 dimensionless Love numbers of star A (or B)
We store amplitude and phase for multipoles modes up to l=4 as time series sampled at 16384 Hz.
We make these waveforms freely available in the hope that they will be useful. We kindly ask you to cite [3] and [4] in any publication resulting from the use of these waveforms.
---
[1] http://www.tapir.caltech.edu/~david_e/whiskythc.html
[2] https://eob.ihes.fr/
[3] S. Bernuzzi, A. Nagar, T. Dietrich, T. Damour; Modeling the Dynamics of Tidally Interacting Binary Neutron Stars up to the Merger; Phys.Rev.Lett. 114 (2015) 16, 161103.
[4] D. Radice, S. Bernuzzi, C. D. Ott; The One-Armed Spiral Instability in Neutron Star Mergers and its Detectability in Gravitational Waves; arXiv:1603.05726.
https://zenodo.org/record/46733
10.5281/zenodo.46733
oai:zenodo.org:46733
url:https://zenodo.org/communities/nrgw-opendata
info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/4.0/legalcode
gravitational waves
neutron stars
The One-Armed Spiral Instability in Neutron Star Mergers and its Detectability in Gravitational Waves
info:eu-repo/semantics/other
dataset
oai:zenodo.org:3235675
2019-05-30T19:07:41Z
openaire_data
user-nrgw-opendata
David Radice
Albino Perego
Kenta Hotokezaka
Steven A. Fromm
Sebastiano Bernuzzi
Luke F. Roberts
2019-05-30
We release dynamical ejecta data from binary neutron star merger simulations. The outflows are extracted at a fixed coordinate sphere with radius 300 G/c^2 Msun (= 443 km). Only material unbound according to the geodesic criterion is considered to be part of the dynamical ejecta. See [1] for more details.
Included data:
`Table2.txt`: Table 2 of the paper in machine readable format
`tabulated_nucsyn.h5`: nucleosynthesis yields from pre-computed parametrized trajectories. The first three indices of each dataset are Ye, entropy, and expansion timescale tau. For example `Y_final[iYe, ientr, itau, iiso]` gives the final abundance of isotope `iiso` with `A[iiso]` and `Z[iiso]` for a trajectory with initial Ye = `Ye[iYe]`, initial entropy `s[ientr]`, and expansion timescale `tau[itau]`.
`[model].tar`: ejecta data for individual simulations. The naming convention is the same as in the paper.
For each model we provide:
`outflow.txt`: angle integrated outflow rate and cumulated ejecta mass. Data are given in units with Msun = G = c = 1 (eg, the conversion factor for time to seconds is 4.9258e-6).
`hist_entropy.dat`: histogram of the ejecta as a function of the entropy (in kb)
`hist_vinf.dat`: histogram of the ejecta as a function of the asymptotic velocity (in units of c)
`hist_ye.dat`: histogram of the ejecta as a function of the electron fraction Ye.
`profile.txt`: 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.
`hist_ye_theta.h5`: histograms of the ejecta as a function of the asymptotic velocity and the polar angle.
`hist_ye_entropy_tau.h5`: histograms of the ejecta as a function of Ye, entropy, and expansion timescale tau.
Additionally we distribute:
Initial data generated with LORENE and associated EOS tables.
EOS tables used for the evolution
Parameter file used for each simulation
For the multidimensional histograms the indices are ordered as specified in the file name, ie the file `hist_ye_theta.h5` tabulates the ejecta mass as a function of Ye (first index) and polar angle theta (second index).
[1] 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
https://zenodo.org/record/3235675
10.5281/zenodo.3235675
oai:zenodo.org:3235675
info:eu-repo/grantAgreement/EC/H2020/714626/
doi:10.5281/zenodo.3235674
url:https://zenodo.org/communities/nrgw-opendata
info:eu-repo/semantics/openAccess
http://creativecommons.org/licenses/by/4.0/legalcode
Binary Neutron Star Mergers: Mass Ejection, Electromagnetic Counterparts, and Nucleosynthesis
info:eu-repo/semantics/other
dataset
oai:zenodo.org:61308
2017-09-06T07:08:29Z
openaire_data
user-nrgw-opendata
Harms, Enno
Lukes-Gerakopoulos , Georgios
Bernuzzi, Sebastiano
Nagar, Alessandro
2016-09-01
We release gravitational wave fluxes at null-infinity from a spinning test-body in circular equatorial orbits around a Schwarzschild black hole. Four different prescriptions are used for the dynamics: the Mathisson-Papapetrou formalism under the Tulczyjew (TUL) spin-supplementary-condition (SSC), the Pirani (PIR) SSC and the Ohashi-Kyrian-Semerak (OKS) SSC, and the spinning particle limit of the effective-one-body Hamiltonian (HAM) of [Phys.~Rev.~D.90,~044018(2014)]. For more details see xxxx .
The multipolar fluxes are given for l=2,3 m=1,2,3 at the Boyer-Lindquist radii
r = 4 5 6 7 8 10 12 15 20 30 ,
in cases they were not computed the data contains a "42". Note that the fluxes in these data files are assumed to contain both the +m and -m contributions, since they are identical for equatorial orbits and aligned spins.
Additionally, the data files contain the key numbers describing the circular dynamics (see paper).
Units c=G=1.
https://zenodo.org/record/61308
10.5281/zenodo.61308
oai:zenodo.org:61308
url:https://zenodo.org/communities/nrgw-opendata
info:eu-repo/semantics/openAccess
http://creativecommons.org/publicdomain/zero/1.0/legalcode
gravitational waves
spinning bodies
binary black holes
Teukolsky equation
Spinning test-body orbiting around Schwarzschild black hole: circular dynamics and gravitational-wave fluxes
info:eu-repo/semantics/other
dataset
oai:zenodo.org:57844
2019-04-10T03:45:31Z
openaire_data
user-nrgw-opendata
Bernuzzi, Sebastiano
Radice, David
Ott, Christian D.
Roberts, Luke F.
MÃ¶sta, Philipp
Galeazzi, Filippo
2016-07-12
We release neutron star merger waveforms computed using fully general relativistic simulations of equal and unequal-mass binaries drawn from the galactic population. The simulations employ finite-temperature microphysical equations of state (LS220, DD2, and SFHo) and neutrino cooling. Please, see
http://arxiv.org/abs/1512.06397
for details.
Each tarball refers to a simulation and contains
Curvature multipolar waveform \(\psi^{(4)}_{\ell m}\)
Metric multipolar waveform \(h_{\ell m}\)
Radiated energy and angular momentum
Files:
waveforms/Psi4_l?_m?_r200.txt
Columns: \(t,\ \Re{(\psi^{(4)}_{\ell m})},\ \Im{(\psi^{(4)}_{\ell m})} \)
waveforms/Rh_l?_m?_r200.txt
Columns: \(u/M,\ \Re{(h_{\ell m})}/M,\ \Im{(h_{\ell m})}/M,\ \Re{(\dot{h}_{\ell m})},\ \Im{(\dot{h}_{\ell m}}),\ M\omega_{\ell m},\ A_{\ell m}/M,\ \phi_{\ell m},\ t \)
waveforms/Ej_r200.txt
Columns: \(E_b,\ j,\ E_\text{rad},\ J_\text{rad},\ t \)
where
\(t\) simulation time
\(u\) retarded time
\(M\) binary mass
\(\omega_{\ell m}\) wave frequency
\(A_{\ell m}\) wave amplitude
\(\phi_{\ell m}\) wave phase
\(E_\text{GW}\) radiated energy
\(J_\text{GW}\) radiated angular momentum
\(E_b\) binary energy
\(j\) binary specific angular momentum
Please refer to the paper and references therein for the definition of the different quantities.
Units \(c=G=M_\text{Sun}=1\)
https://zenodo.org/record/57844
10.5281/zenodo.57844
oai:zenodo.org:57844
url:https://zenodo.org/communities/nrgw-opendata
info:eu-repo/semantics/openAccess
http://creativecommons.org/publicdomain/zero/1.0/legalcode
Binary neutron stars
Gravitational waves
Numerical relativity
How loud are neutron star mergers?
info:eu-repo/semantics/other
dataset