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Figure 1:
The final fate of accretion OMgNe white dwarfs as a function of the initial white dwarf mass and the accretion rate onto the white dwarf. (Figure 3 of [187]; used with permission.) |
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Figure 2:
A comparison between the GW amplitude ![]() ![]() ![]() ![]() ![]() |
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Figure 3:
Type I waveform (quadrupole amplitude ![]() |
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Figure 4:
Type II waveform (quadrupole amplitude ![]() |
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Figure 5:
Type III waveform (quadrupole amplitude ![]() |
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Figure 6:
Movie showing the evolution of a secular bar instability, see Ou et al. [191] for details. |
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Figure 7:
Movie showing the evolution of the regular collapse model A3B2G4 of Dimmelmeier et al. [60]. The left frame contains the 2D evolution of the logarithmic density. The upper and lower right frames display the evolutions of the gravitational wave amplitude and the maximum density, respectively. |
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Figure 8:
Movie showing the same as Movie 7, but for rapid collapse model A3B2G5 of Dimmelmeier et al. [60]. |
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Figure 9:
Movie showing the same as Movie 7, but for multiple collapse model A2B4G1 of Dimmelmeier et al. [60]. |
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Figure 10:
Movie showing the same as Movie 7, but for rapid, differentially rotating collapse model A4B5G5 of Dimmelmeier et al. [60]. |
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Figure 11:
The gravitational waveform (including separate matter and neutrino contributions) from the collapse simulations of Burrows and Hayes [41]. The curves plot the gravitational wave amplitude of the source as a function of time. (Figure 3 of [41]; used with permission.) |
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Figure 12:
The gravitational waveform for matter contributions from the asymmetric collapse simulations of Fryer et al. [87]. The curves plot the the gravitational wave amplitude of the source as a function of time. (Figure 3 of [87]; used with permission.) |
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Figure 13:
The gravitational waveform for neutrino contributions from the asymmetric collapse simulations of Fryer et al. [87]. The curves plot the product of the gravitational wave amplitude to the source as a function of time. (Figure 8 of [87]; used with permission.) |
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Figure 14:
Convective instabilities inside the proto-neutron star in the 2D simulation of Müller and Janka [176]. The evolutions of the temperature (left panels) and logarithmic density (right panels) distributions are shown for the radial region ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 15:
Quadrupole amplitudes ![]() |
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Figure 16:
Movie showing the isosurface of material with radial velocities of ![]() |
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Figure 17:
Movie showing the oscillation of the proto-neutron star caused by acoustic instabilities in the convective region above the shock. |
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Figure 18:
A comparison between the GW amplitude ![]() ![]() ![]() |
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Figure 19:
Meridional plane density contours from the SMS collapse simulation of Saijo, Baumgarte, Shapiro, and Shibata [208]. The contour lines denote densities ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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http://www.livingreviews.org/lrr-2003-2 |
© Max Planck Society and the author(s)
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