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Frontiers of GW predictions from CCSN Model

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!.

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Frontiers of GW predictions from CCSN Model

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  1. Frontiers of GW predictions from CCSN Model • Takami Kuroda (Basel Univ.) • Kei Kotake(Fukuoka Univ.), TomoyaTakiwaki(NAOJ), • Ko Nakamura (Waseda Univ.), Kazuhiro Hayama(Osaka-city Univ.)

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

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

  4. Asymmetries in CCSNe Too wide dynamical range !!! T < 〜１sec T > １day〜1yr Time R< 〜１03km Spatial Scale R> 〜１06-13km ~108km Direct observation by Milisavljevic & Fesen, ‘13 Hammer+,’10 Gravitational waves R=0km Neutrinos R〜20km

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

  6. Explosion Mechanisms 1)ν-driven explosion 2)MHD explosion Takiwaki+,’11 Buras+,’06 Scheidegger+,’10 (3D) Obergaulinger+,’06 (2D) Marek&Janka,’09 Takiwaki+,’08 (2D) Suwa+,’10 “Round” explosion “Oriented” explosion Rotation  Explosion Morphology GWs • rotation is not necessary • rotation is necessary

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

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

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

  10. GW Emissions from Rotating Core 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% Dimmelmeier+,’08

  11. GW Emissions from Rotating Core How does rapid rotation affects on the observed GW emissions? Rotational instabilities ①Dynamical instability (|T/W|>0.27) …… Rampp + ’98 ②Secular instability (|T/W|>0.13) …… Chandrasekhar ’70 ③Low |T/W| instability (|T/W|>0.01) …… Watts +’05

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

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

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

  15. GW Emissions from Rotating Core GW emissions from one-armed spiral wave Scheidegger+,’10 • Full spatial domain • Without excising inner boundary • 0<φ<2π (for m=1 mode) • Neutrino cooling (for Rshock) Blondin&Mezzacappa,’07 Fernandez,’10 Tpb~27ms one-armed spiral wave (Rshock>R>RPNS)

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

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

  18. GW Emissions from Rotating Core Scheidegger+,’10 Tpb~27ms Strong emission from one-armed spiral wave

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

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

  21. GW Emissions from Rotating Core Importance of neutrino-cooling Rshock w/o cooling w/ cooling Rns Unstable region (Rns<R<Rshock) becomes more compact due to ν-cooling Non-axisymmetric structure

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

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

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

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

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

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

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

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

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

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

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

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

  34. GW emissions and mass dependence • 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) KT, Takiwaki & Kotake, in preparation • We can investigate • Progenitor dependence • SASI evolution without excising inner boundary • Correlation between GW & Lnu

  35. S15.0 S27.0

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

  37. Lack of data SASI feature ?

  38. GW Emissions from Non-Rotating Core Egw ↑ Mprogenitor↑

  39. How about observations? Hayama+ • Source is located at optimal direction • SNR is only for “KAGRA” Polar S15.0_Rot_Ext Equatorial S15.0_Rot S40.0 S11.2

  40. Lack of data

  41. Summary • We may be able to link future GW observations and core rotational profile. • anti-νe energy & Fpeakevolution 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

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