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The First Stars and Hypernovae

The First Stars and Hypernovae. K. Nomoto (Univ. of Tokyo). M > 10 5 M  : SMS (Super Massive Stars) GR instability Collapse M ~ 300 － 10 5 M  : VMO (Very Massive Objects) Nuclear Instability Pulsational Mass Loss M ~ 130 － 300M  : Pair Creation Instability

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The First Stars and Hypernovae

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  1. The First Stars and Hypernovae K. Nomoto (Univ. of Tokyo)

  2. M > 105M:SMS (Super Massive Stars) GR instability Collapse M ~ 300－105M: VMO (Very Massive Objects) Nuclear Instability Pulsational Mass Loss M ~ 130－300M: Pair Creation Instability Collapse Nuclear Explosion M ~ 8－130M: Fe core Collapse HypernovaeBH SNe IINS

  3. First Stars (Pop III Stars) • First Supernovae (Type II, Ibc, Hypernovae, Pair) • Early Cosmic Chemical Evolution • AGB Stars • Supernovae (Type Ia) • Abundance Ratios @high z, low Z • EMP (Extremely Metal-Poor) Stars: Halo, dSph • DLA • ICM, … • -elements: [(O, Mg, Si, S, Ar, Ca)/Fe], [Si/O] • Fe-peak elements: [(Ti, Cr, Mn, Co, Ni, Zn)/Fe] • R-process, s-process elements Cosmic Clock

  4. [Cr, Mn, Co/Fe] Inhomogenitiy for [Fe/H]<-2.5 O,Ne,Mg...., Fe Galactic Chemical Evolution [Fe/H]=log(Fe/H）-log(Fe/H) Halo Disk Homogeneous enrichment 2.5

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

  6. C-rich EMP Stars 2 [C/Fe] 1 0 -1 -4 -3 -2 -1 0 [Fe/H] Aoki et al. (2002)

  7. First Generation Stars/SupernovaeandExtremely Metal-Poor Stars • EMPs: [Fe/H] < -2.5 • Trends in [(Zn, Co, Mn, Cr)/Fe] • C, N-rich Stars • Variation in C/Mg, Mg/Si, ．．． • HE0107-5240 (Christlieb et al.) • Low mass star formation @[Fe/H]~ －5.3? • Core-Collapse Supernovae • Black Hole Formation M > 20-25M Variations in Explosion energy Hypernovae Mixing & Fallback Faint SNe Jets, … Rotation? Binary?

  8. 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

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

  10. 56Co decay

  11. 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

  12. Spectral Fitting: SN1997ef Iwamoto et al. 2000 Too Narrow Features Normal SN E51=1 MCO = 6M Hypernova E51=20, MCO = 11M  Broad Features

  13. 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)

  14. SN 2003dh GRB/SN Connection

  15. SN 2003dh : Early spectra Hjorth et al (2003)

  16. GRB 030329/SN 2003dh (36d) Matheson et al. Kawabata et al. (Subaru) IAU Circ. 8133 Similar to SN 1998bw at < ~ 30 days (Stanek et al.; Hjorth et al.) to SN 1997ef at > ~ 30 days (Kawabata et al.)

  17. 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)

  18. 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

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

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

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

  22. 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?

  23. 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

  24. LowEnergyｖｓ High Energy Explosion 28Si 28Si 16O 56Ni 16O 56Ni

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

  26. First Supernovae and EMP stars • EMPs: [Fe/H] < －2.5 • Trends in [(Zn, Co, Mn, Cr)/Fe] • C, N-rich Stars • HE0107-5240 (Christlieb et al.) • Black-Hole Forming Supernovae Variations in Explosion Energy Rotation Mixing & Fallback Binarity Jets, … High Energy, Jets Mixing & Fallback (~25M－130M)

  27. Type Ia/IIn SN2002ic (Kotak et al. 2003)

  28. Discovery of H-lines in SN Ia 2002ic Hamuy et al(2003)

  29. SN2002ic: ~222d(Subaru) ―― SN2002ic ―― SN1997cy(IIn) ―― SN1999E(IIn)

  30. SN2002ic: Bolometric Light Curve

  31. High r T~107K low r T~109K Reemit in Optical X-ray Reverseshock Coolingshell Forwardshock Circumstellar Interaction Model ejecta • CSM r= r0 *(R/R0) –n H line • Ejecta SNIa (W7) • Contact Discontinuity R0=1e+15cm r =r0～1-25e-15g/cm3 CSM (Chevalier & Fransson)

  32. Result(I)-Light Curve • Density r0=2.5e-14g/cm3 • Index n=1.8 (Suzuki et al. 2003)

  33. Origin of H-rich CSM Binary Single AGB Star→SN I1/2

  34. Circumstellar Medium of SN2002ic • Mass ~2-3M • M ~ 10-4M yr-1 • Aspherical • Binary Scenario: Massive Companion → WD wind → SN Ia • Single Star Scenario: AGB Star (Low Metallicity?) → Type I1/2

  35. First Supernovae [Fe/H] : -5 -4 -3 -2.5 Faint SNe Hypernovae Normal SNe Black-Hole Forming Supernovae (20-130M) ⇒ First Black Hole > 2~6M Faint SNe(High and Low energy)⇒C,O-rich ejecta ⇒Efficient Cooling of ISM ⇒ Formation of Low Mass C,O-rich 2nd Generation Stars

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