AGB超新星爆発における元素合成
和南城，野本（IPMU）
H. -Th. Janka, F. S. Kitaura, B. Müller (MPA)
arXiv:0810.3999

supernovae from 8-10M~ stars
AGB SN from of an ONeMg core (up to ~30% of all SNe)
Nomoto 1984, 1987; Miyaji & Nomoto 1987

Â progenitor of Crab SN?
Nomoto et al. 1982; Davidson et al 1982

Î carbon-rich?? >9.5M~??
MacAlpine & Satterfield 2008

Â low-luminosity SNe?
SN1997D, Chugai & Utrobin 2000
SN2003gd, Hendry et al. 2005

Î < 17M~ for all SNeIIP??
Smartt et al. 2008

Î new SNe class ofSN2008S-like transientswith AGB progenitors??
Prieto et al. 2008; Thompson et al. 2008

Crab Nebula, hubblesite.org

origin of r-process nuclei?
Honda et al. 2004 (Ishimaru, Wanajo, Aoki, & Ryan 2004)
François et al. 2007

8-10 M~

20-25 M~no starÍ Ïdispersion

Â chemical evolution studies favor
the low-mass end (8-10M~ stars)
Ishimaru & Wanajo 1999; Ishimaru et al. 2004

Â r-process models related to
8-10M~ stars
Wanajo et al. 2003; Ning et al. 2007
but Janka et al. 2008; Hoffman et al. 2008

>30 M~

self-consistent explosion of a 9M~ star!
weak explosion by neutrino heating
Kitaura, Janka, & Hillebrandt 2006Îthe only case (1D)with accurate ν transportÎEexp =1°1050 erg
Mej=0.014M~
s=10-30 k/mu
Ye=0.46-0.53
Nucleosynthesisin the SN withno parametersÎ most reliable SN yields
to date!?

initial compositions (Ye)ÂYe, min = 0.464

nucleosynthesis
Â Fe (as 56Ni) production
at Ye ≥ 0.49
(0.002-0.004M~)
Â 64Zn and light p-nuclei(e.g., 92Mo) at Ye = 0.46-0.49
Hoffman et al. 1996; Wanajo 2006

Â marginal νp-process
at Ye > 0.50
Flohrich et al. 2006;
Pruet et al. 2006
Wanajo 2006

Â no r-process (up to 90Zr)
at least tpb < 1s with 1D
Hoffman et al. 2008

overproduction factors
Â strong overproduction of 90Zr at Ye ~ 0.47

mass-averaged yields
Â strong overproduction of 90Zr, high Ni/Fe (~ 10 solar)
Â little production of 56Ni (=0.002-0.004M~ in mass fraction)

Ye,min=0.464

contribution to the Galaxy
X ( 90 Zr) / X ( 16 O)f== 0.029
9016
1 − f M ( Zr) / M ( O)otherf : fraction of ONeMg SNe relative to all SNeII/Ibc
M ( 16 O)other = 1.5M : average ejecta mass of 16 O
per event from SNe (> 10M )Â f = 0.028
Â 81% of solar 90Zr is from s-processÂ no more than 1% of all core-collapse supernovae....
in agreement with Hoffman et al. 2008

initial compositions (Ye)ÂYe, min = 0.475

mass-averaged yields
Â only 2% increase of Ye,min cures the overproduction of 90Zr !!
Â robust production of 64Zn and p-nuclei 74Se, 78Kr, 84Sr, 92Mo

Ye,min=0.475

contribution to the GalaxyX ( 64 Zn) / X ( 16 O)
f== 0.3964
16
1 − f M ( Zn) / M ( O)otherf : fraction of ONeMg SNe relative to all SNeII/Ibc
M ( 16 O)other = 1.5M : average ejecta mass of 16 O
per event from SNe (> 10M )Â f = 0.28
Â origin solar 64Zn (dominant isotope) is uncertain
Â up to ~ 30% of all core-collapse supernovae !!!
(consistent with 8-10M~)

2D effect ? (preliminary)

8.8 M~(Kitaura et al. 2006)

8.8 M~(Muller & Janka in prep.)conclusions
Â up to ~30% (~8-10M~) of all core-collapse supernovaepossible origin of 64Zn and p-nuclei 74Se, 78Kr, 84Sr, 92Mo
Â little 56Ni production (=0.002-0.004M~ in mass fraction)
consistent with the Crab SN (with high Ni/Fe ~10 solar),
low-luminosity SNeIIP (SN1997D, SN2003gd, ....),
new class of luminous transients (SN2008S, ....)
Â carbon-rich gas of Crab, AGB progenitor of SN2008S
mass range ~9.5-10 M~ (~7-8% of all SNe)