This archive is a catalogue of the energy radiated by gravitational
waves of 26 supernova core collapse models as described in detail
in these two papers:

1. Dimmelmeier, H., Font, J.A., and M\"uller, E.,
   "Relativistic simulations of rotational core collapse.
    I. Methods, initial models, and code tests",
   Astron. Astrophys., 388, 917-935 (2002);
   astro-ph/0204288.

2. Dimmelmeier, H., Font, J.A., and M\"uller, E.,
   "Relativistic simulations of rotational core collapse.
    II. Collapse dynamics and gravitational radiation",
   Astron. Astrophys., 393, 523-542 (2002);
   astro-ph/0204289.



It contains the following files:

energy_A1B1G1_N.dat      energy_A1B1G1_R.dat
energy_A1B2G1_N.dat      energy_A1B2G1_R.dat
energy_A1B3G1_N.dat      energy_A1B3G1_R.dat
energy_A1B3G2_N.dat      energy_A1B3G2_R.dat
energy_A1B3G3_N.dat      energy_A1B3G3_R.dat
energy_A1B3G5_N.dat      energy_A1B3G5_R.dat
energy_A2B4G1_N.dat      energy_A2B4G1_R.dat
energy_A3B1G1_N.dat      energy_A3B1G1_R.dat
energy_A3B2G1_N.dat      energy_A3B2G1_R.dat
energy_A3B2G2_N.dat      energy_A3B2G2_R.dat
energy_A3B2G4_N.dat      energy_A3B2G4_R.dat
energy_A3B2G4_soft_N.dat energy_A3B2G4_soft_R.dat
energy_A3B3G1_N.dat      energy_A3B3G1_R.dat
energy_A3B3G2_N.dat      energy_A3B3G2_R.dat
energy_A3B3G3_N.dat      energy_A3B3G3_R.dat
energy_A3B3G5_N.dat      energy_A3B3G5_R.dat
energy_A3B4G2_N.dat      energy_A3B4G2_R.dat
energy_A3B5G4_N.dat      energy_A3B5G4_R.dat
energy_A4B1G1_N.dat      energy_A4B1G1_R.dat
energy_A4B1G2_N.dat      energy_A4B1G2_R.dat
energy_A4B2G2_N.dat      energy_A4B2G2_R.dat
energy_A4B2G3_N.dat      energy_A4B2G3_R.dat
energy_A4B4G4_N.dat      energy_A4B4G4_R.dat
energy_A4B4G5_N.dat      energy_A4B4G5_R.dat
energy_A4B5G4_N.dat      energy_A4B5G4_R.dat
energy_A4B5G5_N.dat      energy_A4B5G5_R.dat



The initial models are rotating gamma = 4/3 polytropes in equlibrium
with a central density rho_c_ini = 1.0 * 10^10 g/cm^3.

Each collapse model is specified by three parameters, A, B, and G:

A1: A = 5.0 * 10^9 cm
A2: A = 1.0 * 10^8 cm
A3: A = 5.0 * 10^7 cm
A4: A = 1.0 * 10^7 cm

B1: beta_rot_ini = 0.25%
B2: beta_rot_ini = 0.5%
B3: beta_rot_ini = 0.9%
B4: beta_rot_ini = 1.8%
B5: beta_rot_ini = 4.0%

G1: gamma_1 = 1.325
G2: gamma_1 = 1.32
G3: gamma_1 = 1.31
G4: gamma_1 = 1.30
G5: gamma_1 = 1.28



The parameter _R/_N in the energy name stands for a simulation in
relativistic/Newtonian gravity, respectively. Thus, for example 
'energy_A2B4G1_R.dat' is the gravitational wave energy radiated by model
A2B4G1 in relativistic gravity. One model, A3B2G4_soft, has been
simulated with a soft equation of state. For details we refer to
paper 1 as listed above.



All energies have been obtained by the following formula, Eq. (3)
in the above listed paper 2, where 'A^E2_20' was calculated using
the quadrupole 'stress formula', Eq. (A.5) in the same paper:

E_rad_tot = 1/(32 pi) \int |dA^E2_20/dt|^2 dt

Column 1 is the coordinate time 't' in units of milliseconds.
Column 2 is the energy amplitude 'E_rad_tot' in units of solar masses.



This gravitational wave energy catalogue can be obtained freely
from this URL:
http://www.mpa-garching.mpg.de/rel_hydro/

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23 June 2004, Harald Dimmelmeier (harrydee@mpa-garching.mpg.de).