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Hypernovae and Gamma-ray Bursts

Hypernovae and Gamma-ray Bursts. K. Nomoto (U. Tokyo). SN 1998bw. Hypernova Candidates E kinetic > (5-10) × 10 51 ergs. GRB 980425. Spectra of Supernovae & Hypernovae. Ic : no H, no strong He, no strong Si. SiII. Ia. O. Ca. He. Ib. Hypernovae ： broad features

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Hypernovae and Gamma-ray Bursts

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  1. Hypernovae and Gamma-ray Bursts K. Nomoto (U. Tokyo)

  2. SN 1998bw Hypernova CandidatesEkinetic > (5-10)×1051ergs GRB 980425

  3. Spectra of Supernovae & Hypernovae Ic: no H, no strong He, no strong Si SiII Ia O Ca He Ib Hypernovae： broad features blended lines 　　“Large mass at high velocities” Ic 94I 97ef Hyper-novae 98bw

  4. CO Star Models for SNeIc H-rich He ５６Fe C+O 56Co MC+O Si 56Ni Fe Collapse • ~ [dyn• diffusion]1/2 ~• 1/2  Mej R V R c Parameters [Mej, E, M(56Ni)] Light Curve Spectra E  Mej  ½Mej¾E -¼ ５６Ni E  Mej3

  5. Spectral Fitting: SN1997ef Iwamoto et al. 2000 Too Narrow Features Normal SN (E51=1) Small Mej Hypernova (E51=20) Large Mej at High Vel. Broad Features

  6. Light curves of Hypernovae & SNeIc log L (erg/s) Radioactive Decay 56Ni 56Co 56Fe 43 98bw&CO138 42 97ef&CO100 41 94I &CO21 0 50 100 t (days)

  7. Bolometric Light Curves SN 2003dh Mej=8M E=3.8×1052ergs M(56Ni)=0.35M SN 1998bw COMDH SN 2002ap SN 1997ef Mazzali et al (2003)

  8. Type II-P SN 1997D Very narrow lines. V < 1000 km s-1. EK=1-4×1050ergs. V~1000km s-1 2002gd, 1999br Faint M(56Ni)~2×10-3M (Turatto, Mazzali, Young, Nomoto 2002)

  9. Turatto, Mazzali, Young, Nomoto, Iwamoto et al. (1998) SNⅡ 1997D:Faint SN m－M=30.64 (NGC1536) 1987A LBOL 1997D Mms~20M M(56Ni) 0.07M 0.002M 1987A 1997D Mms~ 25－30MR ≤ 300R E~4×1050erg narrow lines

  10. Supernovae/Hypernovae Nomoto et al. (2003) EK Failed SN? 13M~15M

  11. M(56Ni)/M Nomoto et al. (2003) [/Fe]≫0

  12. SNe in Binary Systems Single M1~M2 ”Conservative” M1»M2 ”Non-Conservative” 2 1 2 1 Spiral-in RSG Rapid Rotator SNII Wolf Rayet (WN, WC) He, C+O Star SNIb/c ? SNIb/c Hypernovae?

  13. McWilliam, Ryan, Spite, Co Cr trend [Fe/H] [Fe/H] Mn Zn

  14. Hypernova Nucleosynthesis (1) M(Complete Si-burning) (Zn, Co)/Fe (Mn, Cr)/Fe Fe/(O, Si) (2) More ‐rich entropy Zn/Fe 64Ge Ti/Fe (3) More O burns (Si, S, Ca)/O Low energy High energy

  15. Jet-Induced Explosion Rotating Black Hole + Accretion Disk K. Maeda, 2003

  16. Collimated jets (Z) + Bow shock (All direction) M Lateral expansion Radial Velocity/c Hydrodynamics R/1010cm

  17. Jet-induced Explosion Maeda & Nomoto (2003), astro-ph/0304172 E51=10, MBH(final)=6M, M(56Ni)=0.1M, MCO=14M 0.04 0.04 0.7 s 1 Outflow Inflow (Fallback) 0 0 0 1.5 s R/1010cm

  18. [OI] 6300A 56Fe 16O Interpretation as an Aspherical explosion FeII] 5200A Observation Spherical 15 deg Aspherical Maeda et al. 2002

  19. Element Distribution Bipolar Explosion Model Zn Zn Zn Zn Mn

  20. Spherical 40M, E51=1 Jet 40M, E51=10 [Cr/Fe] [Mn/Fe] Jet 25M, E51=7 Spherical 25M, E51=1 [Co/Fe] [Zn/Fe]

  21. UN2003 Co Cr 15M, E51=1 25M, E51=30 (Hypernova) Mn Zn

  22. Origin of Hypernovae and Gamma-Ray Bursts Hypernovae • High Energy: E>1052erg • Massive: Mms>20-25M, typically 30-40M Black Hole forming Supernovae • Aspherical (Jet-induced) Explosions • Spectra, Light curves, Polarization Rotating Black Hole + Accretion Disk • Type Ic SNe: C+O stars Mergers in Binaries First Stars ? • Hypernova Nucleosynthesis Abundance Patterns of Extremely Metal-Poor Stars

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