The influence of model parameters on the prediction of gravitational wave signals from stellar core collapse

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Volume 514 (May 2010)

A&A, 514 (2010) A51

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Table 3:

Summary of GW related quantities^a.
Model	t_f[ms]	$E_{GW} [M_{\odot}c^2]$	Dir.	$\vert A_{+,b,\max}\vert$	$\vert A_{\times,b,\max}\vert$	$\vert A_{+,pb,\max}\vert$	$\vert A_{\times,pb,\max}\vert$	$f_{b} [{\rm Hz}]$	f_TW[Hz]
R0E1CA	130.8	$2.15\times10^{-11}$	I	3	<1	3	<1	-	-
R0E1CA	130.8	$2.15\times10^{-11}$	II	2	<1	5	1	-	-
R0E3CA	103.9	$5.72\times10^{-11}$	I	2	<1	10	<1	-	-
R0E3CA	103.9	$5.72\times10^{-11}$	II	2	<1	8	<1	-	-
R0STCA	70.3	$1.35\times10^{-11}$	I	3	<1	4	<1	-	-
R0STCA	70.3	$1.35\times10^{-11}$	II	1	<1	3	<1	-	-
R1E1CA	112.8	$1.36\times10^{-10}$	I	3	<1	12	6	-	-
R1E1CA	112.8	$1.36\times10^{-10}$	II	3	<1	15	1	-	-
R1E3CA	130.4	$1.43\times10^{-10}$	I	2	<1	10	5	-	-
R1E3CA	130.4	$1.43\times10^{-10}$	II	3	<1	17	<1	-	-
R1E1DB	112.8	$1.24\times10^{-10}$	I	3	<1	12	6	-	-
R1E1DB	112.8	$1.24\times10^{-10}$	II	3	<1	15	2	-	-
R1STCA	45.8	$2.01\times10^{-11}$	I	2	<1	3	1	-	-
R1STCA	45.8	$2.01\times10^{-11}$	II	2	<1	6	<1	-	-
R1E1CA_L	92.9	$1.04\times10^{-10}$	I	3	<1	4	2	-	-
R1E1CA_L	92.9	$1.04\times10^{-10}$	II	2	<1	10	1	-	-
R2E1AC	127.3	$5.52\times10^{-9}$	I	2	2	6	5	-	-
R2E1AC	127.3	$5.52\times10^{-9}$	II	105	<1	1	3	841	-
R2E3AC	106.4	$5.31\times10^{-9}$	I	2	2	4	4	-	-
R2E3AC	106.4	$5.31\times10^{-9}$	II	104	<1	1	<1	803	-
R2STAC	64.0	$7.62\times10^{-9}$	I	3	3	6	6	-	-
R2STAC	64.0	$7.62\times10^{-9}$	II	133	<1	2	1	680	-
R3E1AC	62.5	$5.58\times10^{-8}$	I	2	1	15	16	-	725
R3E1AC	62.5	$5.58\times10^{-8}$	II	393	<1	10	2	880	-
R3E2AC	45.5	$6.53\times10^{-8}$	I	2	1	11	13	-
R3E2AC	45.5	$6.53\times10^{-8}$	II	409	<1	5	3	882	-
R3E3AC	57.5	$6.44\times10^{-8}$	I	2	2	6	9	-
R3E3AC	57.5	$6.44\times10^{-8}$	II	409	<1	6	3	891	-
R3STAC	50.2	$1.05\times10^{-7}$	I	5	4	9	11	-	935
R3STAC	50.2	$1.05\times10^{-7}$	II	526	<1	5	3	854	-
R3E1CA	69.4	$8.05\times10^{-8}$	I	3	3	9	9	-	-
R3E1CA	69.4	$8.05\times10^{-8}$	II	426	<1	5	3	897	-
R3E1DB	62.7	$7.76\times10^{-8}$	I	8	8	13	11	-	-
R3E1DB	62.7	$7.76\times10^{-8}$	II	425	<1	8	3	886	-
R3E1AC_L	196.7	$2.14\times10^{-7}$	I	1	1	136	136	-	909
R3E1AC_L	196.7	$2.14\times10^{-7}$	II	437	<1	70	9	909	-
R4E1AC	98.7	$7.74\times10^{-8}$	I	1	<1	37	37	-	662
R4E1AC	98.7	$7.74\times10^{-8}$	II	512	<1	20	6	385	-
R4STAC	67.2	$1.91\times10^{-7}$	I	2	1	102	109	-	902
R4STAC	67.2	$1.91\times10^{-7}$	II	536	<1	53	3	396	-
R4E1EC	100.8	$7.51\times10^{-8}$	I	1	1	25	20	-	611
R4E1EC	100.8	$7.51\times10^{-8}$	II	492	<1	15	7	866
R4E1FC	80.1	$7.29\times10^{-8}$	I	<1	<1	16	19	-	828
R4E1FC	80.1	$7.29\times10^{-8}$	II	516	<1	9	3	859	-
24E1FC_L	97.6	$3.42\times10^{-7}$	I	2	1	316	298	-	673
24E1FC_L	97.6	$3.42\times10^{-7}$	II	536	<1	157	6	485	-
R4E1CF	19.1	$6.50\times10^{-8}$	I	1	1	4	4	-
R4E1CF	19.1	$6.50\times10^{-8}$	II	518	<1	ring-down	2	370	-
R5E1AC	93.2	$1.20\times10^{-8}$	I	1	1	18	18	-	727
R5E1AC	93.2	$1.20\times10^{-8}$	II	238	<1	10	11	317	-

Notes. ^(a) t_f is the time after core bounce when the simulation was stopped. E_GW is the total energy released in gravitational radiation. We present the maximum amplitudes at different stages of their time-evolution in polar (I) and equatorial (II) direction. The subscripts b and pb stand for bounce and postbounce. f_b denotes the peak frequency of the GW burst at bounce, while f_TW stands for the spectral peak from the narrow band emission caused by a low T/|W| instability. The electronic wave forms of all models are available upon request.

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