frontiers of gw predictions from ccsn model
DESCRIPTION
Frontiers of GW predictions from CCSN Model. Takami Kuroda (Basel Univ.) Kei Kotake(Fukuoka Univ.), Tomoya Takiwaki(NAOJ ), Ko Nakamura ( Waseda Univ.), Kazuhiro Hayama(Osaka -city Univ.) . Asymmetries in CCSNe. From many observations CCSNe are asymmetric explosions!. - PowerPoint PPT PresentationTRANSCRIPT
Frontiers of GW predictions from CCSN Model
• Takami Kuroda (Basel Univ.)Kei Kotake(Fukuoka Univ.), Tomoya Takiwaki(NAOJ),
Ko Nakamura (Waseda Univ.), Kazuhiro Hayama(Osaka-city Univ.)
Asymmetries in CCSNe
Tanaka+,’12 Milisavljevic & Fesen, ‘13
3D mapping of optically emitting ejecta (Cas A)
From many observationsCCSNe are asymmetric explosions!
Asymmetries in CCSNe
From many numerical simulations suggestInitiation of CCSNe is asymmetric!
Takiwaki+, ‘12 Scheidegger+, ‘10
Suwa+, ‘10 Marek&Janka, ‘09
All of thesesimulations are within the innermostregion of star(R/Rstar<10-3~-5)
optical observationis impossible
Asymmetries in CCSNe
TimeT < 〜1 sec
Milisavljevic & Fesen, ‘13
Spatial Scale
T > 1 day 〜 1yr
R < 〜103km
R > 〜1 06-13km
Too wide dynamical range !!!
Hammer+,’10
~108km
Gravitational wavesDirect observation by
R=0kmNeutrinosR 〜
20km
Kotake,’11, "Gravitational Waves (from detectors to astrophysics)"
Diversity of Gravitational Waveforms
2)MHD explosionExplosion Mechanisms
1)ν-driven explosion
“Round” explosion “Oriented” explosion
Buras+,’06 Takiwaki+,’11
Suwa+,’10 Marek&Janka,’09 Takiwaki+,’08 (2D)
Scheidegger+,’10 (3D)
rotation is not necessary rotation is necessary
Obergaulinger+,’06 (2D)
Rotation Explosion Morphology GWs
GW Emissions from Rotating CoreHow does rapid rotation affectson the observed GW emissions?
Type I signal (Dimmelmeier+,’02)
GW Emissions from Rotating CoreHow does rapid rotation affects
on the observed GW amplitude?
Obergaulinger+,’06
GW Emissions from Rotating CoreType I signal appears irrespective
of dimensionality of explosion.
3DDimmelmeier+,’08
Scheidegger+,’10 (3D)
Microphysical EOS2D
Microphysical EOSNu-cooling3D-MHD
GW Emissions from Rotating Core
Dimmelmeier+,’08
Type I signal --->Linear correlation between |h|max and T/|W|b(=βb)
In modern stellar evolution,βi<~0.1% (Heger+,’05, Yoon&Langer,’08) βb<~1%
GW Emissions from Rotating CoreHow does rapid rotation affectson the observed GW emissions?
① Dynamical instability (|T/W|>0.27) …… Rampp + ’98 ② Secular instability (|T/W|>0.13) …… Chandrasekhar ’70 ③ Low |T/W| instability (|T/W|>0.01) …… Watts +’05
Rotational instabilities
GW Emissions from Rotating CoreHow does rapid rotation affectson the observed GW emissions?
3DGR + Γ-law EOS (Ott+,’05)
Low-T/Winstability
GW Emissions from Rotating Core
3DNMHD + Microphysics (Scheidegger+,’10)
m=1
m=2
GW Emissions from Rotating CoreBecause the low-T/W instability
occurs in the vicinity of PNS,• FGW~kHz• hGW~10-20~-19 @D=10kpc
Ott+,’07 Scheidegger+,’10
AdvLIGO
GW Emissions from Rotating Core
Blondin&Mezzacappa,’07 Fernandez,’10
GW emissions from one-armed spiral wave
one-armed spiral wave (Rshock>R>RPNS)
Scheidegger+,’10
Tpb~27ms
•Full spatial domain• Without excising inner boundary• 0<φ<2π (for m=1 mode)
•Neutrino cooling (for Rshock)
GW Emissions from Rotating Core
GW emissions from one-armed spiral wave3DGR + Neutrino radiation (leakage for cooling term)
15Msun with (KT, Takiwaki & Kotake, arXiv:1304.4372)
EquatorPolar
Consistent with Ott+,’12
GW Emissions from Rotating Core
Time evolution of “h=A/10kpc” spectrum
S/N(=h/N)=1 (for KAGRA)
log(
h)
GW Emissions from Rotating Core
€
ψ ij ≡ddt
Strong emission fromone-armed spiral wave
Scheidegger+,’10
Tpb~27ms
€
ψ ≡ (2ψ xy )2 +(ψ xx −ψ yy )2
Angular frequency of “Acoustic+Rotational” mode
Ωrot
Ωrot+Ωaco
X (cm)
GW Emissions from Rotating Core
One armed spiral waves produce GW emission at F~FDoppler.FDoppler(~200Hz) represents “Acoustic+Rotational” frequency.
How is this “~200Hz” determined?
GW Emissions from Rotating CoreImportance of neutrino-cooling
Importance of neutrino-cooling
GW Emissions from Rotating Core
w/o coolingw/ cooling
Unstable region (Rns<R<Rshock) becomes more compact
due to ν-cooling
Non-axisymmetricstructure
Rns
Rshock
Importance of neutrino-cooling
GW Emissions from Rotating Core
Unstable region (Rns<R<Rshock) becomes more compact
due to ν-cooling
Non-axisymmetricstructure
Scheidegger+,’10
w/o cooling
w/ cooling
~10 timesstronger GWs
Fully general relativistic 3D-Rad-Hydro!!
GW Emissions from Rotating CoreIn addition, if there is strong magnetic field…….
Obergaulinger+,’06
R<60km
Total
w/ B
Type I signal (Dimmelmeier+,’02)
w/o B
Offset
GW Emissions from Rotating CoreIn addition, if there is strong magnetic field…….
2D 3D
Takiwaki+,’08(2D) Scheidegger+,’10 (3D)
Slowly varying positive offsetoriginated from MHD jet
GW Emissions from Rotating Core
If the star rotates sufficiently fast (T/W|b > a few % T/W|i > a few ‰)
Strong Type I signalLow frequency Emission from MHD jet
Low T/W instability (F~kHz, τdecay~10ms, from PNS)One armed spiral wave (F~ a few 100Hz, τdecay~τexplo (?) , above PNS)
GW Emissions from Non-Rotating Core
Neutrino
Matter
When rotation is negligible,(Neutrino Explosion occurs)GW waveforms are characterized as
1) Early (Linear) SASI motion2) Hot Bubble Convection & SASI3) Explosion Phase
Z(km
)
Muller B.+,’13
Freq
uenc
y (H
z)
Neutrino
Matter
Advective mode
Acoustic mode
Blondin+, ‘03
GW Emissions from Non-Rotating Core
Local contributionto GW emissions Matter acceleration
Muller B.+,’13
Tpb=22ms
Coherent Stripe Pattern(not stochastic convective one)
GW Emissions from Non-Rotating Core
SASI (L 〜 1,2….) Convection (higher order L)
or
Hanke+,’13
Muller B.+,’13
From Brunt-Vaisalla frequency,Muller+,’13 derived following relation
GW Emissions from Non-Rotating Core
Brunt-Vaisallafrequency
gravitationalforce at NS surfaceNS surface
temperatureCompact parameter
Uni- (or Bi-) polar explosion• positive GW amplitude• low frequency (<100Hz)
GW Emissions from Non-Rotating Core
Murphy+,’09
Information on explosion morphology is imprinted in GW waveforms
GW Emissions from Non-Rotating Core
Up to now, there is no GW analysis studyusing successful ν-explosion model in full-3D
Iwakami+, ‘08
GW Emissions from Non-Rotating Core
Equipartition of energy
Hanke+,’13
Light-bulb method in 3D
Kotake+,’11
GW Emissions from Non-Rotating Core
3DGR + ν-Radiation (Gray M1+Leakage for cooling)Progenitor: 11.2, 15.0, 27.0 & 40.0 Msun (WW95) ~0.3, 1.05, 1.85 & 2.10 Xi(1.5Msun)1283cells * 9 Level nested structure (dxmin~450m)Long term simulations (Tpb=200-250ms)
GW emissions and mass dependence
KT, Takiwaki & Kotake, in preparation
We can investigate• Progenitor dependence• SASI evolution without excising inner boundary• Correlation between GW & Lnu
S27.0
S15.0
Convective Initiation of SASI (?)
SASI SASI
S11.2
S27.0
S15.0
S40.0
Lack of data
SASI feature ?
GW Emissions from Non-Rotating Core
Egw ↑Mprogenitor ↑
How about observations?
Equatorial
Polar
S11.2
S40.0
S15.0_Rot
Hayama+
S15.0_Rot_Ext
•Source is located at optimal direction•SNR is only for “KAGRA”
Lack of data
€
Lν e
€
Lν e
€
Lν e
€
Lν e
Summary
•We may be able to link future GW observations and core rotational profile.•anti-νe energy & Fpeak evolution will tell us, e.g., M/R.•Confirmed SASI (27&40Msun) in 3DGR for the first time•Their GW frequency appears ~100Hz•They can be detected up to ~20kpc•There is oscillation in anti-e neutrino luminosity