GRB conference @ YITP Kyoto
13. Nov. 2013

Nucleosynthetic signatures in magneto-rotational
driven core-collapse supernovae

Nobuya Nishimuracontents• introduction• origin of heavy elements• energetic supernovae, GRBs, and nucleosynthesis• magneto-rotational driven supernovae• MHD-SN explosion models• r-process• explosive nucleosynthesis and observation• conclusion

based onN. Nishimura, T. Takiwaki, and F.-K. Thieleman(2013 in prep.)r-process: “cosmic alchemy”- origin of heavy elements (with s-process)- e.g., gold, actinide- nuclear physics- rapid-neutron captures (related to unstable isotopes)- Astronomical sites (?)- non-standard Supernova (SN)- neutron star mergers
Solar system abundanceAnders & Grevesse (1989)r-process: physics & astronomical sites- high neutron density- neutron rich matter from NS?
- explosive events(<< 1 min, neutron’s half life)- separated from the s-process- Astronomical sites- core-collapse supernova (formation of NS)- merger of NS-NS / BH-NS binary→ short GRB? (talk by Wanajo)- “collapsar” jet or disk→ long GRB? (talk by Surman)

Core-Collapse Supernovae: > 10 Msun
the end of
the evolution

the corecollapses

a proto-neutron staris formed

p + e- → n + νeelectron-capture
neutronization•photo-disintegration•electron capture

shock
protoneutron starn + νe → p + e-

neutrino (νe)-burst
figure: wikipedia

core-collapse supernovae-supernova ejecta → iron group elements including 56Ni
neutrino-driven proto-neutron star wind
Wanajo 2013

- difficult to have suitablecondition for the r-process- not very neutron-rich ( > 0.4 )- not high entropy (< 200)by several studies- supportedFischer et al. 2010,Hüdepohl et al. 2010 etc.

→ alternative energetic supernova scenario?

Magnetohydrodynamic (MHD) SNe and magnetars
r-process studies•2D MHD-SNe!
•Nishimura et al. 2006
•Fujimoto, Nishimura,and Hashimoto 2008
(central Black-Hole and disk)•3D MHD-SNe with neutrino!
Winteler et al.et al. 2012
•Winteler2tating core collapses with strong magnetic fields could
be the hypernova/jet-likesolution (Cameron 2003; Nishimura
SN et al. 2006;
Fujimoto et al. 2008).
The present paper has the aim to explore the resultsfrom our 3D magnetohydrodynamic (MHD) calculations,which lead to bipolar jet ejection. The following section 2will discuss the initial models and the explosion dynamics, section 315
will present nucleosynthesis results. Section
4 is devoted to a discussion of uncertainties and an outlook on future investigations.

•Magnetar•strong magnetic field〜10G(〜1 %2.of3D all
neutronMHD-CCSN
MODELstars)•Magneto-driven Supernovae?
•GRB central engine•Hypernovae

The calculation presented here was performed with thecomputational setup similar to our previous investigations (Liebendörfer et al. 2005; Scheidegger et al. 2010).
The initially innermost (600 km)3 of the massive star
are covered by a 3D Cartesian domain uniformly discretized by 6003 cells, resulting in a 1 km resolution,that is embedded in a spherically symmetric domain encompassing the iron core and parts of the silicon shell.
The magnetic fluid is evolved with the ideal MHD code
FISH (Käppeli et al. 2011) and the spherically symmet-Fig. 1.— 3D entropy contours spanning the coordinates planes
with magnetic field lines of the MHD-CCSN simulation ∼ 31 ms
after bounce. The 3D domain size 700 × 700 × 1400 km.

3D MHD simulation
Winteler et al. (2012)

et al. (2005). Although the model provides profiles forrotation and magnetic fields, we use an analytic prescription for their distributions and we will comment on0.02

Ejected Mass [10−5 M⊙ ]

0.03

0.04

0.05

n of Ye from a single tracer in green (red)neutrino absorption estimate). The blue
evolved by the network. Vertical dottedto the time when ν̄e (νe ) neutrinospherevertical line when T = 10 GK.

und estimatesthese numbers
red:andneutrino
absorption
the end of (green:
the simulation.
We deno neutrino)
nbound if its total specific energy
120
gnetic+potential)is positive and if
pointing100outward.
80

UCLEOSYNTHESIS
60

calculations
are performed with a40
n network (Winteler 2011) which
20d (numericallyand physically) up0
etwork (seeet al.0.35
0.10 e.g.
0.15 Thielemann
0.20
0.25
0.30
eaction rates of RauscherYe& Thiele-40

MHD 20code :FISH( Käppeli et al. 2011 )
00.10
0.30
0.35
0.40
progenitor:0.15 0.20 0.25
Ye15Msun (Heger&Woosely 2002)
Fig. 3.— Ejecta masses vs. Ye for the original simulation witho
magnetic
fieldsand: including a simplified prescripti
neutrino
captures (green)
for neutrino heating (red). The12width of a Ye bin is chosen topoloidal 5×10 [G] ( initial )∆Ye = 0.01.

time [s]Ejected Mass [10−5 M⊙ ]100

Winteler, Käppeli, Perego, Arcones,Vasset, Nishimura,
80
Liebendörfer, Thielemann Basel60 collaboration) 2012, ApJL

10−23

Ejected Mass [M⊙ ]0.01

T9 = 10

R = RνeR = Rν¯e

3D-MHD model with leakage scheme
120

10−310−4
10−510−610−760

0.40

M ej = 0.672 10-2 Msun

80

100

120

140160180

Mass Number

200220240

r-process in MHD-SNe: “prompt” vs “delayed”•more long-term simulation model•robustness of resulting r-process•dependency on the explosion mechanism•axisymmetric•special relativistic MHD•leakage scheme forneutrino cooling•25Msun WR star

Takiwaki et al. 2009
prompt(Heger & Woosley)time duration of explosion delayeddelayedpromptAmplification of magnetic fields via field wrapping
differential rotation

magnetic field line

top view
magnetic field lines

side view

Takiwaki 2009Ejected matter: ejection motion and Yepath of ejected tracer particles (post-process)delayedPrompt

0.5

0.5

0.4

0.4

0.3

0.3

Ye

Ye

Ye evolution for different ejecta

0.2
0.1

Z: proton number
pHe
n0 1

2-0.1

45

00.1

ignored νe-capture

0-0.2

0.2

after the bounce (s)-0.1

Mo(42)
Nb(41)
Zr (40)Y (39)
Sr (38)Rb(37)Tc (43)Ru(44) PPCd(48) P
Ag(47)
Pd(46) P
Rh(45)

Sn(50) P
In (49)6 7 8

9Xe(54) P
I (53)Te (52) P
Sb(51)

Ba(56) P
Cs(55)

Ce(58) P
La (57)

Sm(62) P
Pm(61)
Nd(60)
Pr (59)Dy(66) P
Tb (65)Gd(64) P
Eu(63)Er (68) P
Ho(67)

Yb(70) P
Tm(69)

Hf (72) P
Lu (71)Os(76) P
Re(75)
W (74) PP
Ta (73)

Pt (78) P
Ir (77)Hg(80) P
Au(79)

Pb(82)Tl (81)At (85)
Po(84)Bi (83)

199200196197198
194195
192193189190191
188
185186187

183184

179180181182
165166167168169170171172173174175176177178

163164155156157158159160161162
154
153
149150151152
147148134135136137138139140141142143144145146
127128129130131132133

PP

P

Xe(54) P
I (53)Te (52) P
Sb(51)

P

119120121122123124125126
113114115116117118
112
107108109110111

P P
P

P

103104105106
97 98 99 100101102

P

87 88 89 90 91 92 93 94 95 96

P

85 86
83 84

P

Kr (36)
Br (35)Se(34)As (33)Ge(32)
Ga(31)Zn (30)Cu(29)

PP

71 7273 74 75 76 77 78 79 80 81 82

65 66 67 68 69 70
63 64

10 11 12

N: neutron numberpHenB
Be
Li

0 12Mo(42)Nb(41)
Zr (40)Y (39)
Sr (38)Rb(37)Tc (43)Ru(44) PP

Cd(48) P
Ag(47)
Pd(46) P
Rh(45)

Sn(50) P
In (49)456 7 89Ba(56) P
Cs(55)

Ce(58) P
La (57)

Sm(62) P
Pm(61)
Nd(60)
Pr (59)Dy(66) P
Tb (65)Gd(64) P
Eu(63)Er (68) P
Ho(67)

Yb(70) P
Tm(69)

Hf (72) P
Lu (71)Os(76) P
Re(75)
W (74) PP
Ta (73)

Pt (78) P
Ir (77)Hg(80) P
Au(79)

Pb(82)Tl (81)At (85)
Po(84)Bi (83)Fm(100)Es (99)Cf (98)
Bk (97)Cm(96)
Am(95)Pu(94)
Np(93)U (92)
Pa(91)Th (90)Ac (89)Ra(88)Fr (87)
Rn(86)

183184165166167168169170171172173174175176177178

163164155156157158159160161162
154
153
149150151152
147148134135136137138139140141142143144145146
127128129130131132133

PP

P

P

119120121122123124125126
113114115116117118
112
107108109110111

P PP

103104105106
97 98 99 100101102

P87 88 89 90 91 92 93 94 95 96

P85 86
83 84

PPP

71 72

73 74 75 76 77 78 79 80 81 82

65 66 67 68 69 70
63 64

mass fraction (log10)

10 11 120-5199200196197198
194195
192193189190191
188
185186187

179180181182

PPP

Ni (28)55 56 57 58 59 60 61 62
Co(27)Fe (26)53 54
Mn(25)Cr (24)51 52
V (23)Ti (22)49 50
Sc (21)
47 48
Ca(20)
43 44 45 46
K (19)
39 40 41 42
Ar (18)Cl (17)35 36 37 38
S (16)33 34
P (15)31 32
Si (14)
Al (13)29 30
Mg(12)
25 26 27 28
Na(11)
24
Ne(10)
21 22 23F
18 19 20O
15 16 17
NC
13 14

30.1

r-process flow

Fm(100)Es (99)Cf (98)
Bk (97)Cm(96)
Am(95)Pu(94)
Np(93)U (92)
Pa(91)Th (90)Ac (89)Ra(88)Fr (87)
Rn(86)

PP

0after the bounce (s)r-process flow

Ni (28)55 56 57 58 59 60 61 62
Co(27)Fe (26)53 54
Mn(25)Cr (24)51 52
V (23)Ti (22)49 50
Sc (21)
47 48
Ca(20)
43 44 45 46
K (19)
39 40 41 42
Ar (18)Cl (17)35 36 37 38
S (16)33 34
P (15)31 32
Si (14)
Al (13)29 30
Mg(12)
25 26 27 28
Na(11)
24Ne(10)21 22 23F
18 19 20O
15 16 17
NC
13 14

30.1

ignored νe-capture

0-0.2

Kr (36)
Br (35)Se(34)As (33)Ge(32)
Ga(31)Zn (30)Cu(29)

B
Be
Li

0.2

-10

0.2

r-process in MHD-SNe: “prompt” vs “delayed”
successful r-process (prompt)!
r-process is suppressed up to second peak (delayed)2

prompt (B11TW1.00)
prompt (B12TW1.00)
delayed (B11TW0.25)

delayed2nd peak

1abundance, YA

3rd peak0prompt
actinide-1-260

80

100

120

140160mass number, A180200220240r-process result (2/3): “weak” r-elements“weak” r-process pattern (HD122563; Honda 2006)

nucleosynthesis result: key amounts
B11TW0.25 B11TW1.00 B12TW0.25 B12TW1.00 B12TW4.00

delayed prompt prompt prompt prompt

type
ejected mass

(10-2 Msun)
r-proc. mass

(10-3 Msun)

56Ni(10-2 Msun)

1.27

6.88

3.42

9.48

9.38

0.963

1.54

1.15

2.05

2.67

1.07*-0.63*1.19*

1.21** minimum values (component in the first shock wave)• significant amount of r-process matter comparedwith normal supernova (10-5 Msun from PNS wind)• low event rate ( 〜 0.1 - 1 % of all supernova)
have impact on chemical evolution/obervation

optical observation:

Nomoto et al. 2006

smaller amount of 56Ni
faint SN ?

56Ni

our results

56Ni with magnetar formation

Maeda et al. 2007

SN2005bf (type Ib with double peak)
56Ni 〜 0.02 - 0.06 M
sunstrong magnetic field 〜1015 G-XRF060218 (SN2006aj)
Mazzali et al. 2006, Maeda et al. 2007

magnetarSummary•MHD-SNe are still possible candidate for r-process•prompt-magnetic-jets : “main” r-process•delayed-magnetic-jets : ”weak” r-process?
•Large amount of r-process elements (〜10-3 Msun)•MHD-SNe are faint ? and have relation to peculiar SN/XRF.
remaining problem•Long-term simulations•dependence of initial rotations and magnetic ﬁelds•MHD-SN always produce “solar” r-process pattern?
•uncertainties of micro physics (neutrino, ...)
•cases of large oﬀ-axisymmetry•physics of MHD ampliﬁcation process (MRI, reconection ..)・・・