1. 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.)

2. Asymmetries in CCSNe Tanaka+,’12 Milisavljevic & Fesen, ‘13 3D mapping of optically emitting ejecta (Cas A) From many observations CCSNe are asymmetric explosions!

3. Asymmetries in CCSNe From many numerical simulations suggest Initiation of CCSNe is asymmetric! Takiwaki+, ‘12 Scheidegger+, ‘10 Suwa+, ‘10Marek&Janka, ‘09 All of these simulations are within the innermost region of star (R/R star <10 -3~-5 ) optical observation is impossible

4. Asymmetries in CCSNe Time T < 〜１ sec Milisavljevic & Fesen, ‘13 Spatial Scale T > １ day 〜 1yr R < 〜１ 0 3 km R > 〜１ 0 6-13 km Too wide dynamical range !!! Hammer+,’10 ~10 8 km Gravitational waves Direct observation by R=0km Neutrinos R 〜 20km

5. Kotake,’11, "Gravitational Waves (from detectors to astrophysics)" Diversity of Gravitational Waveforms

6. 2)MHD explosion Explosion 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 necessaryrotation is necessary Obergaulinger+,’06 (2D) Rotation  Explosion Morphology  GWs

7. GW Emissions from Rotating Core How does rapid rotation affects on the observed GW emissions?

8. Type I signal (Dimmelmeier+,’02) GW Emissions from Rotating Core How does rapid rotation affects on the observed GW amplitude? Obergaulinger+,’06

9. GW Emissions from Rotating Core Type I signal appears irrespective of dimensionality of explosion. 3D Dimmelmeier+,’08 Scheidegger+,’10 (3D) Microphysical EOS 2D Microphysical EOS Nu-cooling 3D-MHD

10. GW Emissions from Rotating Core Dimmelmeier+,’08 Type I signal --->Linear correlation between |h| max and T/|W| b (=β b ) In modern stellar evolution, β i <~0.1% (Heger+,’05, Yoon&Langer,’08) β b <~1%

11. GW Emissions from Rotating Core How does rapid rotation affects on 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

12. GW Emissions from Rotating Core How does rapid rotation affects on the observed GW emissions? 3DGR + Γ-law EOS (Ott+,’05) Low-T/W instability

13. GW Emissions from Rotating Core 3DNMHD + Microphysics (Scheidegger+,’10) m=1 m=2

14. GW Emissions from Rotating Core Because the low-T/W instability occurs in the vicinity of PNS, F GW ~kHz h GW ~10 -20~-19 @D=10kpc Ott+,’07Scheidegger+,’10 AdvLIGO

15. GW Emissions from Rotating Core Blondin&Mezzacappa,’07 Fernandez,’10 GW emissions from one-armed spiral wave one-armed spiral wave (R shock >R>R PNS ) Scheidegger+,’10 T pb ~27ms Full spatial domain Without excising inner boundary 0<φ<2π (for m=1 mode) Neutrino cooling (for R shock )

16. GW Emissions from Rotating Core GW emissions from one-armed spiral wave 3DGR + Neutrino radiation (leakage for cooling term) 15M sun with (KT, Takiwaki & Kotake, arXiv:1304.4372) EquatorPolar Consistent with Ott+,’12

17. GW Emissions from Rotating Core Time evolution of “h=A/10kpc” spectrum S/N(=h/N)=1 (for KAGRA) log(h)

18. GW Emissions from Rotating Core Strong emission from one-armed spiral wave Scheidegger+,’10 T pb ~27ms

19. Angular frequency of “Acoustic+Rotational” mode Ω rot Ω rot+ Ω aco X (cm) GW Emissions from Rotating Core  One armed spiral waves produce GW emission at F~F Doppler.  F Doppler (~200Hz) represents “Acoustic+Rotational” frequency. How is this “~200Hz” determined?

20. GW Emissions from Rotating Core Importance of neutrino-cooling

21. GW Emissions from Rotating Core w/o cooling w/ cooling Unstable region (R ns <R<R shock ) becomes more compact due to ν-cooling Non-axisymmetric structure R ns R shock

22. Importance of neutrino-cooling GW Emissions from Rotating Core Unstable region (R ns <R<R shock ) becomes more compact due to ν-cooling Non-axisymmetric structure Scheidegger+,’10 w/o cooling w/ cooling ~10 times stronger GWs Fully general relativistic 3D-Rad-Hydro!!

23. GW Emissions from Rotating Core In addition, if there is strong magnetic field……. Obergaulinger+,’06 R<60km Total w/ B Type I signal (Dimmelmeier+,’02) w/o B Offset

24. GW Emissions from Rotating Core In addition, if there is strong magnetic field……. 2D 3D Takiwaki+,’08(2D) Scheidegger+,’10 (3D) Slowly varying positive offset originated from MHD jet

25. GW Emissions from Rotating Core If the star rotates sufficiently fast (T/W| b > a few % T/W| i > a few ‰)  Strong Type I signal  Low frequency Emission from MHD jet  Low T/W instability (F~kHz, τ decay ~10ms, from PNS)  One armed spiral wave (F~ a few 100Hz, τ decay ~τ explo (?), above PNS)

26. GW Emissions from Non-Rotating Core Neutrino Matter When rotation is negligible, (Neutrino Explosion occurs) GW waveforms are characterized as 1)Early (Linear) SASI motion 2)Hot Bubble Convection & SASI 3)Explosion Phase Z(km) Muller B.+,’13 Frequency (Hz)

27. Neutrino Matter Advective mode Acoustic mode Blondin+, ‘03 GW Emissions from Non-Rotating Core

28. Local contribution to GW emissions Matter acceleration Muller B.+,’13 T pb =22ms Coherent Stripe Pattern (not stochastic convective one) GW Emissions from Non-Rotating Core

29. SASI (L 〜 1,2….) Convection (higher order L) oror Hanke+,’13 Muller B.+,’13 From Brunt-Vaisalla frequency, Muller+,’13 derived following relation GW Emissions from Non-Rotating Core Brunt-Vaisalla frequency gravitational force at NS surface NS surface temperature Compact parameter

30. Uni- (or Bi-) polar explosion positive GW amplitude low frequency (<100Hz) GW Emissions from Non-Rotating Core

31. Murphy+,’09 Information on explosion morphology is imprinted in GW waveforms GW Emissions from Non-Rotating Core

32. Up to now, there is no GW analysis study using successful ν-explosion model in full-3D Iwakami+, ‘08 GW Emissions from Non-Rotating Core Equipartition of energy Hanke+,’13

33. Light-bulb method in 3D Kotake+,’11 GW Emissions from Non-Rotating Core

34. 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) 128 3 cells * 9 Level nested structure (dx min ~450m) Long term simulations (T pb =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

35. S27.0 S15.0

36. ConvectiveInitiation of SASI (?) SASI S11.2 S27.0 S15.0 S40.0

37. Lack of data SASI feature ?

38. GW Emissions from Non-Rotating Core E gw ↑ M progenitor ↑

39. 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”

40. Lack of data

41. Summary We may be able to link future GW observations and core rotational profile. anti-ν e energy & F peak 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