1/23

Natsuko Izutani
Univ. of Tokyo2/23

Nucleosynthesis of CC SNe,and compare the SN yields with the observations.

Try to understandGalactic Chemical Enrichment,Stellars and SNe,Or the environment in which they are.

3/23

1. Origin of Co and Zn - do we need HNe ?
(Izutani & Umeda 2010, ApJL)

2. Massive Star ccSN contribution to ChemicalEnrichment (Izutani, Kobayashi, et al. in prep.)
3. SN yields with Neutrino Processes(Kobayashi, Izutani, Amanda, Yoshida, Yong, Umeda, 2011, ApJL)→near future! My work in this group(Izutani, Umeda, Yoshida, Kikuchi, Suzuki, Sumiyoshi…)
complete SN yields (for database:talk of Ishizuka-san) with neutrino processes

4. If I have time…Weak r-Process Star
(Izutani, Umeda, & Tominaga 2009, ApJ)

4/23

H, He→→

Ye~0.5
Progenitor(the last moment of stellar evolution)
Si
Ni56
logXO
C

Ni56 Si
1D hydrodynamics
andPost-process
nucleosynthesis
CrZn(shock wave)

OC

Mn

Mr(Msun)Mr(Msun)5/23

mixing-fallback model (RT, 2D-effect)
O
Ni56
C

can produce [Zn/Fe] >~0with reasonable M(Ni56)
Can produce high [C,O/Fe]

ZnMin

MoutfEjection

6/23

1. Origin of Co and Zn - do we need HNe ?
(Izutani & Umeda 2010, ApJL)

2. Massive Star ccSN contribution to ChemicalEnrichment (Izutani, CK, et al. in prep.)
3. SN yields with Neutrino Processes(Kobayashi, Izutani et al. 2011, ApJL)

4. If I have time…Weak r-Process Star
(Izutani, Umeda, & Tominaga 2009, ApJ)

7/23

Origin of Zn and Co:
Whether it’s HNe or hot-bubble ?

HNHNSN

SNI show HNe are required to produce
Zn and Co !
(Umeda & Nomoto ‘05)

HNe are required toproduce
Zn and Co in EMP stars.

EMP (Cayrel set)

(Frohlich+06)(Heger & Woosley ’10)
Underproduce
Of Zn & Co

SN yields(Thielemann+96)
Proton-rich hot-bubbles
Improve Zn BUT NOT Co !

8/23

What is Hot-bubble ? :Multi-dimensional phenomenon
Of the innermost region of SNe.
Include it
by changing Ye and entropy
In the wider range
Mimicking the 2D-simulation.
(Pruet+’06)

Add the hot-bubble matterto the SN outer yields,
And calculate the total yields.

9/23

BUT

[Co/Fe]EMP(cayrel)

SNe withn-rich matter
Orp-rich matter
Cannot produce
Co !!

SN
Without hot-bubble matter[Zn/Fe](Izutani & Umeda ’10, ApJL)

10/23

HNe are the main origin of Zn and Co.

11/23

1. Origin of Co and Zn - do we need HNe ?
(Izutani & Umeda 2010, ApJL)

2. Massive Star ccSN contribution to Chemical
Enrichment (Izutani, CK, et al. in prep.)
3. SN yields with Neutrino Processes(Kobayashi, Izutani et al. 2011, ApJL)

4. If I have time…Weak r-Process Star
(Izutani, Umeda, & Tominaga 2009, ApJ)

16/23

1. Origin of Co and Zn - do we need HNe ?
(Izutani & Umeda 2010, ApJL)

2. Massive Star ccSN contribution to Chemical
Enrichment (Izutani, CK, et al. in prep.)
3. SN yields with Neutrino Processes(Kobayashi, Izutani et al. 2011, ApJL)

4. If I have time…Weak r-Process Star
(Izutani, Umeda, & Tominaga 2009, ApJ)

17/23

neutrino reaction in SNe

Figure from Yoshida-san’s slides
Reaction rate
TargetReferencen, p:Horowitz, C.J. (’02)
He4, C12 : Yoshida, T.+(’08)
Ni56 (neutral): Suzuki, T.+(’09)
The others from C13 to Kr80: Hoffman & Woosley (’92)

18/23Eν 1
1 1t − r /cφνi (t) =exp(−)Θ(t − r /c)
26 4 πr 3.15Tνi τντν♦neutrino flux

νi : νeµτ ,νeµτ
total neutrino energy : Eν, neutrino irradiation time：τν=3s(Eν= 0, 3e53, 9e53 ergs)♦neutrino energy spectra
Fermi distribution ην = µν / kTν = 0(kTνe ,kTν e ,kTνµτ ) = (4,4,6)(MeV)

19/2325Msun, z= 0 , E = 1e51 ergs

Eν=9e53 ergs

Eν=3e53 ergs

Eν=0 ergs

20/2325Msun, z= 0.02 , E = 1e51 ergs

Eν=9e53 ergs

Eν=3e53 ergs

Eν=0 ergs

21/23

Neutrino reaction to Ne20

Maybe neutrino reaction to Ar40

The models
With•50Msun, E51=1,40,z=0•25Msun, E51=1,10,z=0•15Msun, E51=1,z=0•50Msun, E51=1,40,z=0.004•25Msun, E51=1,10,z=0.004•15Msun, E51=1,z=0.004
Ti44 + p → V45(Sc45) Neutrino reaction to Fe52
•50Msun, E51=1,40,z=0.02•25Msun, E51=1,10,z=0.02•15Msun, E51=1,z=0.02

Include only 15,25,40Msun, z=0, 0.02, E51=1

22/23

Fields stars
Model for globular cluster(Enu=3E53ergs)
Globular clusters
SN+HN+Ia+AGB
SNII+HN+Ia(Kobayashi, Izutani et al. 2011, ApJL)

23/23

Neutrino processes improve
Sc, Mn, K,V, and especially F !