1 / 35

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

cecily
Download Presentation

The First Stars and Hypernovae

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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

More Related