On the Range of Supernova Explosion Energies. K. Nomoto (IPMU / U. Tokyo)

Transcription

1 On the Range of Supernova Explosion Energies K. Nomoto (IPMU / U. Tokyo)

2 AD 1572 Korean & Chinese Record Guest Star as bright as Venus (Sonjo Sujong Sillok: Korea)

3 AD 1572 Tycho Brahe s Supernova Stella Nova (Tycho Brahe 1573) Astronomie Populaire by Camille Flammarion (Paris, 1884)

4 AD 1609 Galileo Galilei's Telescope National Maritime Museum, Greenwich, London Istituto e Museo di Storia della Scienza, Florence

5 Remnant of Tycho s Supernova GreenYellow Blue X-ray (Hot gas with millions of degree) Red Infrared (Circumstellar/ Synthesized dust) (Image: MPIA) White Optical (Foreground/ background stars)

6 Observations of SN Echo (Oort, Zwicky,,,, Rest et al., Krause et al.)

7 Modern Powerful Telescopes Subaru Telescope (8.2m) Very Large Telescope (8.2m) Keck Telescope (10m)

8 Supernova Spectra Fe H Type II Pseudo-continuum + P-Cygni profile C a C a Fe Fe S Si He Si Type Ia O Type Ib Fe N a Si Type Ic O λ v (E/M ej ) 1/2

9 Spectra (Krause, Tanaka, Goto, Usuda, Hattori, Birkmann, Nomoto 08) Bright SN Ia Normal SN Ia Faint SN Ia

10 High Velocity Ca Feature Origin of high velocity Ca? -- Circumstellar interaction? (Gerardy+, Mazzali+) -- Asphericity? ( Echo) 10

11 Echo Tycho s SN:3D structure Tanaka et al. 06, ApJ, 645, 470 high vel Ca

12 MPIA, U. Tokyo, Subaru Telescope (2008)

13 Light Echo Cas A SN=Type IIb SN 1993J (Type IIb) Krause et al. (2008)

14 SNIa Evolution of Stars SNII/Ib

15 The Final Fates of Single Stars M < 0.08 M Brown Dwarf M He White Dwarf M C+O White Dwarf 8 M -- M up O+Ne+Mg WD M up M ONeMg cc-sn + NS 10 M -- M ns Fe-cc-Supernova + NS M ns M Fe-cc-Supernova + BH M Pair Instability SN M SN + BH 10 5 M < M BH(H)

16 Supernova-GRB SN 1998bw Connection GRB

17 (1) GRB / SN 2003dh Stanek et al (2003) ; Hjorth et al (2003)

18 Spectra of Supernovae & Hypernovae Ic: no H, Ia Ib Ic Hyper -novae SiII O Ca He 94I 97ef 98bw no strong He, no strong Si Hypernovae: broad features blended lines Large mass at high velocities Patat et al. (1999)

19 SN2003dh GRB-SN SN2003lw SN1998bw SN2006aj SN1994I SN1997ef SN2002ap

20 56 Co-decay

21 CO Star Models for SNe Ic H-rich Parameters [M ej, E, M( 56 Ni)] M C+O He C+O Si Fe 56 Co 56 Ni Collapse M ms /M M C+O /M ~ ~ ~ Fe Light Curve τ ~ [τ dyn τ diffusion ] 1/2 R ~ V κ M ej 1/2 R c κ ½ M ej¾ E -¼ E M ej 3 Spectra E M ej 56 Ni

22 Spectral Fitting: SN1997ef Too Narrow Features Iwamoto et al. (2000) E 51 =E/10 51 erg Normal SN (E 51 =1) Small M ej Broad Features Hypernova (E 51 =20) Large M ej at High Vel.

23 Supernova GRB Connection Three GRB-SNe = all Type Ic Hypernovae E > erg (~10 normal SN) Large M ms Black Hole Forming SNe Aspherical GRB SN M CO /M M ms /M E/10 51 erg M( 56 Ni)/M bw dh lw

24 Hypernova in Prague

25 Hypernova in Prague

26 Energy M(main seq) Nomoto et al. 03

27 M( 56 Ni) - M(main seq) 27

28 (3) Faint Supernovae SNe 2008ha, 2005cz, 2008S DSS SN 2008ha in UGC (~20 Mpc) Foley et al. (2009)

29 Faint Supernovae SN 2008ha (I?) 2005cz (Ib) (Kawabata+) 2005E (Ib) (Peretz+) 2008S (IIn) (8-10Ms AGB; Prieto+)

30 SN2008ha:Light Curve dashed: 02cx dotted: 05hg (Ib) solid: 05hk Foley et al. (2009) Valenti et al. (2009)

31 SN 2008ha: Spectra (type I) Valenti et al. (2009)

32 Faint SN 2008ha: Spectra(narrow) SN I 2008ha SN Ia Foley et al. (2009) Filippenko (1997)

33 Fallback Supernovae C + O Injection of energy Propagation of shock Fallback Inner layer does not exceed escape velocity Ejection of the outer layer

34 Fallback Supernova Moriya et al. 09

35 Fallback Supernova - abundance distribution Mixing and Fallback Fallback Moriya et al. 2009

36 Fallback models for SN 2008ha - He star core-collapse model (25 M 7 M ) Moriya et al. - CO star core-collapse model (13 M 2.7 M )

37 SN 2008ha: Synthetic Spectra Sauer et al. 2009

38 Hyper Metal Poor Star Frebel et al. (2005)

39 Faint Supernovae EMP (extremely metal-poor) Stars Fallback: small M(Ni) large [CNO/Fe] CEMP (1) Jet-like Energetic Explosion Zn, Co enhanced (2) Weak Explosion Mixing & Fallback

40 Metal Poor Stars Mega Metal Poor (MMP): [Fe/H] < -6 Hyper Metal Poor (HMP): [Fe/H] < -5 Ultra Metal Poor (UMP): [Fe/H] < -4 Extremely Metal Poor(EMP) : [Fe/H] < -3; CEMP Very Metal Poor (VMP): [Fe/H] < -2 Metal Poor (MP) : [Fe/H] < -1 Solar: [Fe/H] ~ 0 Super Metal Rich(SMR): [Fe/H] > +0.5 [Fe/H]=log(Fe/H)-log(Fe/H) (Beers & Christlieb 2005)

41 Hyper Metal-Poor Stars Frebel, Aoki, et al.

42 M=25M, E= erg (Weak Explosion) [Fe/H]=-5.3 Log X Ni 56 Fe O He C H Ne C -2-3 Ti Mg O -4 M BH ~6M Mr (M ) Fallback Ejecta (little Fe) Mixing Umeda & Nomoto (2003) N

43 HMP stars: 1D Low E models (E 51 < 1) mixing & fallback low [Co/Fe] (Frebel et al. 2004) (Bessel, Christlieb Ti Co :high [Co/Fe] Iwamoto et al. (2004) Limongi & Chieffi (2006) Heger & Woosley (2008)

44 Jet-induced Nucleosynthesis Jet BH/NS Jet BH Special relativistic hydrodynamics (Tominaga et al. ApJL 2007) cf. Collapsar (e.g., MacFadyen et al. 01) Magnetorotational Supernovae (e.g., Moiseenko et al. 06). E dep : Energy deposition rate (Rotation, B etc.) Same mass and explosion energy 40M 1.5x10 52 erg

45 Mixing-fallback vs. Jet SN model High entropy due to the energy concentration. Mixing-fallback model Jet SN model

46 (Frebel et al. 2004) HMP Stars Jet-induced SN models (Christlieb et al. 2002) High E High Co/Fe Fallback Small Fe Dark Hypernova Tominaga et al. 2007

47 GRB at z=0.089 (2) No-SN GRBs Della Valle et al. 06, Gal-Yam et al. 06, Fynbo et al. 06, Gehrels et al. 06 GRB at z=

48 Dark Hypernova non-sn GRB GRB Della Valle et al Fynbo et al Gal-Yam et al M( 56 Ni) < 10-3 Ms

49 First stars --Metal-poor stars -- GRB connection Hypernovae with relativistic jets M ms ~ M sun Larger. E dep Smaller GRBs GRB-HNe No-SN GRBs Metal-Poor stars EMP stars UMP stars HMP stars

50 8 10 M Stars Super AGB Stars (1.07 M < M core < M Ch ) degenerate ONeMg core 8 M < M < M up ONeMg White Dwarfs M up ~ 9 M ( Z ) M up < M < 10 M (M core ~ M Ch ) ONeMg Core Collapse SNe II due to Electron Capture Nomoto 1984

51 Electron Capture in ONeMg Core 24 Mg(e -,ν) 24 Na (e -,ν) 24 Ne ρ> gcm -3 collapse

52 Presupernova Density Structure Nomoto- Umeda et al.-

53 9M Star Neutrino Heating Weak Explosion Steep Density Gradient E exp = erg M ej ~ 0.002M Kitaura, Janka, & Hillebrandt (2006)

54 SN 2008S Botticella et al. 2009

55 Progenitor of SN 2008S No detection in NIR a) GMOS /Gemini b) Bok K Detection in MIR Spitzer/IRAC c) 4.5 micron d) 5.8 micron Dust-enshrouded progenitor Botticella et al Prieto et al. 2008, 09

56 Faint SNe IIn: SN 2008S, NGC300-OT (Della Valle et al. 08; Pastorelle 08; Botticella et al. 09) Progenitor = Super AGB star? (Prieto et al. 08,09 Thompson et al. 08) SN Impostor? (Smith et al. 09 Bond et al. 09 Berger et al. 09) Botticellar et al. 2009

57 SN 2008S Botticella et al. 2009

58 Faint Supernovae SN 2008ha ~ Core collapse - Fallback SN? ~ SNe 2002cx, 2005hk-like? narrow line feature ~ SNe 2005E, 2005cz-like? large [Ca/O] SN 2008S-like? Thermonuclear, Core Collapse, or Impostor? EMP star-connection [Ca/O, O/Fe]?

59 Most Luminous Supernova 2006gy M( 56 Ni)~15M or CSM interaction

60 SN 2006gy SN 2006gy (R) Subaru R band (394day) M( 56 Ni)=20M!? 2 arcsec SN 1998bw M( 56 Ni)=0.4M Mirror image subtracted Also Agnoletto et al. (08) Kawabata, Tanaka, et al. (ApJ 2009)

61 SN2006gy vs PISN PISN

62 Nuclear Instability (O, Si- burning) Ohkubo, Nomoto, et al.

63 M : Nuclear Instability Woosley, Blinnikov, Heger (2007)

64 Final Fates of Massive Stars Rotation Magnetic Field? Hypernova + X-Ray Flash + Neutron Star Hypernova + GRB + Black Hole Supernova + Neutron Star Faint/Dark SN + Black Hole ~ 25 30M M ms

65 Absolute magnitude Luminosity Single star (solar metallicity) IIn Type II-P II-L / IIb IIa? NS-forming 08S 05ap 08es 06jc 08D Cas A? 99as, 07bi Hypernovae Ib/c BH-forming (Faint SNe) IIb, 03bg? IIc, 02ic? M( 56 Ni) AGB Fe core Wolf-Rayet Mass (M )

66 Absolute magnitude Luminosity IIn 08S Single star (low metallicity) Type II-P NS-forming IIn 06gy Pulsational instability BH-forming (Faint SNe) Core Collapse PISN M( 56 Ni) AGB Fe core Mass (M )

67 Diversity & Peculiarities of Supernovae vs. Progenitors, Mechanisms * Ultra-Luminous SNe (IIn, II-L, Ic) * Ultra-Faint SNe (IIn): AGB progenitors? * Ic: GRB-SNe, Hypernovae; aspherical * Ib: Energetic (HN-like); aspherical Dusty LBV, WR connection?