supernova nucleosynthesis in the depths- first fully self-consistent result -Shinya Wanajo (NAOJ)
H.-T. Janka, B. Müller (MPA), K. Nomoto (IPMU)
Quarks to Universe in Computational Science (QUCS2012)
December 13-16, 2012, Nara Prefectural New Public Hall

origin of elements beyond iron	
understood (big bang, cosmic rays, stellar evolutions, supernovae)	

not understood	

Zn to U; not understood (light trans-iron, noble metal, rare earth)	
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Wanajo	2	1995ApJS...98..617Tknown problems in SN nucleosynthesis	
production factors from all SNe; Timmes+1995 	

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Wanajo	previous SN
nucleosynthesis based onparametrized 1D modelsv successful up to irongroup elements, butv no production of lighttrans-iron nuclei(Zn to Zr; Z=30-40,A = 64-90) and beyondv little production of
64Zn (49% of Zn),
except for hypernova
models (Umeda &Nomoto 2002)
3	

SN nucleosynthesis in the depths	v T > 4 GK:
NSE (nuclear statisticalequilibrium) consisting ofiron group nucleiv T ~ 4-3 GK:
QSE (quasi-NSE; α-richfreezeout) consisting of αand light trans-iron nucleiv T < 3 GK:
r-process (n-rich) orνp-process (p-rich)v appearance of QSE,r-(or νp-)process highly
dependent on S, τ, Ye
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Wanajo	4	innermost ejecta of SNe	Janka+2012	−evolution stages from the onset+ofn stellar
corecollapse→p+eeupernova explosion on a scale of several 1000 kilometers.
+ow the moment of core bounce andshock
formation(top+p→n+eequasi-stationary accretion (middle left), beginning of thek revival”, middle right), and acceleration of the explosion
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cated in the matter
heated by the outgoing shock, but also Wanajo	
ejecta and the essentially spherically symmetric neutrinosting sites for nucleosynthesis.

ννv elements up to iron areformed in the outer layersv light trans-iron elements
likely to be formed in the
innermost layersv nucleosynthesis-relevant
physics (S, τ, Ye) of thedeepest region extremelycomplex due to mult-D
and neutrino eﬀectsv only self-consistent multidimensional simulations
with neutrino transport
can solve this problem
5	2D SN simulations with ν-transport	
8.8 M¤ ECSN	

8.1 M¤ CCSN	

15 M¤ CCSN	

27 M¤ CCSN	QUCS2012	

Wanajo	v a number of selfconsistent SNmodels with νtransport are now
available (at MPA)v very first result ofSN nucleosynthesis
with such modelsv can we confirm
production of lighttrans-iron nuclei(and beyond) ?
6	9 M¤ self-consistently exploding
ECSN simulation in 2D	

simulation by Bernhard Müller

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Wanajo	7	QUCS2012	

Wanajo	8	neutron-richness in the ejecta	
10-1

10-1

8.8 Msun ECSN

10-2
10-4
10-5
10-6
10-7
0.40

0.450.50

0.55

Ye-1-6e-1

15 Msun CCSN

-2

sun

-3

6Mej [Msun]

10-3
6Mej [Msun]

-5

-8

10-2
10-4
10-5
10-6
10-7
10-4

-7-8

10

Ye distribution in the10
innermost ejecta10(~ 0.01 M¤ )1010v lighter SNe have10
more n-rich ejecta
10
0.40
0.45
0.50
0.55
0.60
due to rapidY
10
expansions (less27 M CCSN
10
ν-processed)
1010v more massive SNe
10have more p-rich
10ejecta due to slow
10
10expansions (more0.40
0.45
0.50
0.55
0.60
Yν-processed)-36Mej [Msun]

6Mej [Msun]

10-3

108.1 Msun CCSN

10-2-4-5-6-7-8-8

0.45

0.50

0.55
Ye

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0.60eWanajo	

9	QUCS2012	

Wanajo	10	NSE, QSE, and νp-process	
1032
101 8.8 Msun ECSN
100
10-1
10-2
10-3
10-4
10-5
10-6
10-7
10-8
10-9
10
10-10
10-11
10-12
10-13
-14
10
0.40
0.45

Yn,p,_/Yh (T9 = 3)

np _

0.50

0.55

Ye
NSE	
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QSE	

(n, p, α) per heavy nucleus at
3 GK for 2500 trajectoriesv n/seed << 1no r-process !
v p/seed > 1 for Ye > 0.51
(weak) νp-processv α/seed < 1 for Ye < 0.45NSEv α/seed > 1 for Ye > 0.45
QSE (α-rich freezeout)νp-process	
Wanajo	11	making light trans-iron: I. n-rich QSE	α-bath	v “α-bath” (~ 3.5 GK)
allows for making
Zn, Ge, Sr, Y, Zrv larger α-separationenergy makes
a nucleus more
tightly boundZr	Zr	
Ge	

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Wanajo	12	making light trans-iron: II. n-rich NSE	
α-deﬁcient bath	As	Kr	Ga	 Kr	Rb	 Kr	 Kr		As	 GaRb	As	 Rb		aGAs		Rb	Kr	Kr
As	
As	
Rb	
Kr		 Rb	
Rb	a
GKr	As	a	GGa	
As	a	
GAs	
Kr	 Rb	
Rb	
Kr	Rb	Rb	As	a	
GAs	 Rb		Gaa	G	Rb	a
Kr	G	aAs	 Kr	Kr	 GQUCS2012	

Wanajo	v “α-deficient bath”(~ 5 GK) allows formaking Ga, As, Se,Br, Kr, Rbv larger binding
energy makes
a nucleus more
tightly boundv n-rich NSE+QSE
make almost alltrans-iron nuclei !
13	making light trans-iron: III. νp-process	v νp-process(Fröhlich+2006;Pruet+2006;Wanajo 2006)
allows for makingZn (64Zn; daughterof 64Ge)v p-rich ejecta help
Zn production !

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Wanajo	14	extreme sensitivity to Ye	0Zn

0.40

0.45

mass fraction

1010-1
10-2
10-3
10-4
10-5
10-6
10-7-810

64 66 67 68 70

Ye
NSE	
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QSE	

nucleosynthesis extremely
8.8 Msun ECSN
sensitive to Ye, e.g.,v 64Zn has two origins
QSE (Ye ~ 0.475) andνp-process (Ye > 0.52)v 66Zn has two origins
NSE (Ye ~ 0.44) andQSE (Ye ~ 0.46)v detailed ν-transport
0.50
0.55
mandatory for
SN nucleosynthesis
beyond iron !!
νp-process	
Wanajo	15	310102

CaCr
Ni
Ge
KrZr
Ti
FeZn
Se
Sr
Mo
8.8 Msun ECSN

101100

10-1
10-2K

104

Ca

mass fraction relative to solar

10-3

Sc
20103

VTi

Mn

CrCo

Ga
Br
YCu
As
Rb
Nb
30
40
atomic number

FeNi

Zn

Ge

Se

KrSrZr

Mo

102
101

15 Msun CCSN

01010-1
10-2

10-3

K

Sc
20V

Mn

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CoGa
Br
Y
Cu
As
Rb
Nb
30
40
atomic number

production factors
108.1 M CCSN
(abundance relative1010to solar)
10v lighter SNe have
1010more NSE-likeKVCoGaBrY
10ScMnCuAsRbNb
203040featureatomic number(intermediate lightCaCrNiGeKrZr
10TiFeZn
Se
SrMo
trans-iron more1010produced)
10 27 M CCSN
10v more massive SNe
10have more QSE1010 K Sc V Mn Co Cu Ga As Br Rb Y Nb
like feature (Zn203040atomic numberand Zr moreproduced)

mass fraction relative to solar

104

mass fraction relative to solar

mass fraction relative to solar

abundances for each SN	
104
32Ca

TiCrFeNiZn

GeSe

KrSrZrMosun

10-1-2-34321sun

0-1-2-3

Wanajo	16	104

103102Ca

TiCrFe

NiZn

GeSe

Kr

SrZr

Mo

all SNe

101
100

10-1
10-2

10-3

KSc
20VMn

CoGa
BrYCu
As
RbNb
30
40
atomic number

105
Zr Ru
Ca
Cr Ni
Ge KrSe
Sr Mo
Ti FeZn
104
103
all SNe
210101
100
10-1
10-2
10-3
10-4
YBrGa
Co
V
Rb Nb
As
Mn Cu
Sc-5
1040
50
60
70
80
90
100
mass number

mass fraction relative to solar

mass fraction relative to solar

integrated abundances	

IMF (initial-mass-function) integrated abundances showv almost all light trans-iron elements (Zn to Zr) can be
explained by the innermost SNe ejectav most of light trans-iron isotopes, including 64Zn, can be
explained as wellQUCS2012	

Wanajo	17	summary	

first self-consistent SN nucleosynthesis with neutrino transportv SNe in the depths can produce all light trans-iron elementsv 64Zn also produced (no need of hypernovae for this isotope?)v result highly dependent on Ye; detailed ν-transport mandatoryv no r-process in SNe (later ν-wind not very promissing;
NS mergers more promissing ?)QUCS2012	

Wanajo	18