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Class. Quantum Grav. 26 (2009) 204015

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trophysical Journal, 851:62 (12pp), 2017 December 10Class. Quantum Grav. 26 (2009) 204015

h+D equator
hh×+DD equatorpole
h×D pole00
MURPHY, OTT, & BURROWS

h+D (cm)

his point, it is useful to define for future reference theensionless characteristic
GW strain (Flanagan & Hughes
1008), in terms of theGW spectral energy density,0!
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Figure 3. Left: GW signal (rescaled by distancD equator
rotating coreh×collapse,bounce and postbounce nonaxisy
h×D pole[61,62].
Shownaretheh+ (top) and h× (bottom) po−300
010 in 203040 plane
5060
70
8090
the equatorial(red lines)
and alongthe polar at - t bounce (ms)linearly polarized
during the axisymmetric collapse and b
elliptically polarized only tens of milliseconds after bou
panel of figure 4 in [5]. Right: time–frequency (TF) aFigure 3. Left: GW signal (rescaled by distan
the GWs emitted by model s20A2B4. The TF analysis
rotating core collapse, bounce and postbounce nonaxis
window that was shifted over the data in steps of 0.2 ms.
[61, 62]. Shown are the h (top) and h× (bottom) po
the energetic late postbounce+ emission leave
clear and clin the equatorial plane (red lines) and along the polar
linearly polarized during the axisymmetric collapse andelliptically polarized only tens of milliseconds after bopanel of figure 4 in [5]. Right: time–frequency (TF)
the GWs
emittedby models20A2B4.
The TF analysit
that even extremely
rapidly
rotating
cores
stay axisymmetricwindow that was shifted over the data in steps of 0.2 ms
the GW emission
to linearlate
polarization(emission
onlyonc
the energetic
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leaveclearinand−200

h× D (cm)or signals with relatively stable frequencies and amplitudes,0ier transforms and their energy spectra are adequate fre−100
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The20STFT
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01030 of40  results of [64], a core collapsing with a precollapse period P0 ∼t-t(ms)" ∞emits a peak GW amplitude of |hmax | ∼ 1 × 10−21 (|hmax |S̃(f, τ ) =A(t) H (t − τ ) e−2πif t dt,(18)2 −8××bounce

in GWsof theDorder
10 cm)
M⊙emitted
c with bymost of th
Figure 3.
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nonaxisymmetricdynamics
inmodels20A2B4
of
500–800
Hz, extending
to lowerfrequencies
withincreasing
that
evenpolarizations
extremely
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cores staysituatedaxisymmetric[61,62].
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is Shibagaki
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Class. Quantum Grav. 26 (2009) 204015

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0−100Figure 3. Left: GW signal (rescaled by distancD equator
rotating coreh×collapse,bounce and postbounce nonaxisy
h×D pole[61,62].
Shownaretheh+ (top) and h× (bottom) po−300
010 in 203040 plane
5060708090the equatorial(red lines)
and alongthe polar at - t bounce (ms)linearly polarized
during the axisymmetric collapse and belliptically polarized only tens of milliseconds after bou
panel of figure 4 in [5]. Right: time–frequency (TF) aFigure 3. Left: GW signal (rescaled by distan
the GWs emitted by model s20A2B4. The TF analysis
rotating core collapse, bounce and postbounce nonaxis
window that was shifted over the data in steps of 0.2 ms.
[61, 62]. Shown are the h (top) and h× (bottom) po
the energetic late postbounce+ emission leave
clear and clin the equatorial plane (red lines) and along the polar
linearly polarized during the axisymmetric collapse andelliptically polarized only tens of milliseconds after bopanel of figure 4 in [5]. Right: time–frequency (TF)
the GWs
emittedby models20A2B4.
The TF analysit
that even extremely
rapidly
rotating
cores
stay axisymmetricwindow that was shifted over the data in steps of 0.2 ms
the GW emission
to linearlate
polarization(emission
onlyonc
the energetic
postbounce emission
leaveclearinand−200

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results of [64], a core collapsing with a precollapse period P0 ∼emits a peak GW amplitude of |hmax | ∼ 1 × 10−21 (|hmax |""  in GWsof theDorder
10−8cm)M""c2 withmost of th
Figure 3.
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rotating core collapse, bounce and postbounce
nonaxisymmetricdynamics
inmodels20A2B4
of
500–800
Hz, extending
to lowerfrequencies
increasing
thateven extremely
rapidly
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axisymmetrict - t bounce (ms)S. Shibagaki[61, 62]. Shown are the h+ (top)and h×Symposium(bottom) polarizations as seen by observers situated 3
32th Rironkon

and rapidly rotating (bottom) models, respectively.
and rapidly(bottom) models,models, respectively.
Inrotating
the non-rotatings11.2-R0.0-3D (top left) shows typiIn thecal
non-rotating
models,s11.2-R0.0-3D(top inleft)
typi- regions.
featuresof neutrino-driven convection
theshows
postshock(Ottploy thefirst-moment-of-momentum-divergence(FMD) formalism
cal features
neutrino-driven
convectionin thepostshockregions.
ture
proposed
byFinn& Evans(1990)(see also andMurphy
etal.in2009;
The ofrisingplumesgrow
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Müller
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and stronger
Takiwaki &and
Kotake2011inforangularjustification.)
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largersize
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initial small mushroom-like Rayleigh–Taylor fingers.
In models with rapid rotation, a clear oblate explosion is obtainedent,
In modelswith rapidrotation, a clear oblate explosion is obtained
3forRES U LT s27.0-R2.0-3DS
model(bottom right), in which the revived shockfor model s27.0-R2.0-3D (bottom right), in which the revived shock
nals
Fig.
1 showsmore
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for our rapidly
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strongly
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the equatorialplane.
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at isweakly
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respectively.
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mod-due to thebilearlyrevival
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an observer
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oblate explosion
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ake

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obtained in previous 3D mobut with more approximate
The bottom panel of Fig.
(h c ) relative to the sensitivity
for a source at 10 kpc. Seen
pole (green line), the peak
the pink vertical band). Noteof the modulation frequency
is simply because a deformin the frequency of f emits
Hyper-Kamiokande can be superior because it is essentially backfrequency of 2f. Our results
2.0ground free (see Scholberg 2012 for detail).
induced by the low-T/|W| ingulation between the time mod
1 Our 3Dcore
1 Ourrotating
models with
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thehigh-resolution
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andal., in preparation).
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the maximum h c at the peak
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the polar observer than thatPNS
thatespeciallyinthesimulation
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noted that the peak frequenc
especiallyinthesimulation
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2015).
of advanced LIGO, advance(see section 2.3 in Nakamura et al. 2015).
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32thSymposium

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32th Rironkon Symposium

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