Japanese Young Physicist Summer School

Tokyo, August 19 – 24, 2008

Supernova !-Nucleosynthesis

and !-Oscillation

Taka Kajino

National Astronomical Observatory

Department of Astronomy, University of Tokyo

!"#$%&'()*+

,-.//// /0.// 1./////+++/232456789:

/,-//////;1</ =1<//// ///////////,->.?

///////////////////////////////@A(BCDEFGHIJKG?

//////////////////////////L@'H'MINOPQRFG STUVG>.W? ///

,-.8X#YZ[

L\]^ Wolfgang Pauli _`ab`cdefghijRkl>.m//

,-.8X#YZ[DnoV4DpqrVsGk>.tuD(nvwxy#zf

'{|Azf8}~h��sR4U8Dnfg��(�t'��rVk��>.m

Fred Reines ' Clyde Cowan _`a�bcdrp��

��h�QRk��D!"#$%&8fgh��m

!"#$%& - ��8l>.

- L@8�������

8�:?

��pfg����s8L@h*k�P���8l>.

l>.8��\�

Cabbibo�J��� \�

L@>.////////¡h¢£��>.//////@AhP¤¥�>.

¦§¨©//////////¦ª¨©

////////¦«¨©

0.//////1.//¬!"#$%&

,-.

W >. (­®@Ad

,-.8X#YZ[

!"#$%&@Ae¯�°

±²��8³§\�+

´µ-_¶·d8�V'¸¹$º»¼%½º»8¾¿+

Majorana * Dirac *+

ÀÁ#ÀÂÃ'!"#$%&ÂÃ8ÄEFÅG+

@A_1.Æx$d

¨©

!8@A

ÀÁ#ÀÇ1.È8@A

!"

`ÉbÊ

FË/`É`É +

`É`ÉÊ

/////// // E = mc2

Ì4Dq�sG�l>.8¨Í�¤`É`ÉÊÎGvwxy#8ÏÐ}~85r6V+

/!i + !i / e+ + e- / 2" (#)

!"#$%&'()*+$%('(,-).)/#'01,"'$12)34-+&5+

!"""#$%&'#%(#)*+,#-.$,+

M. Koshiba detected core-collapse neutrinos

from SN1987A using water-Cherenkov lights

in KAMIOKANDE !

JÑÒÓÔÕ'Ö.× S-K

Super-K, SNO, ØÙÚºÛ (�.Ü !)

determined Ým122 and "12 uniquely.

Þ#ß#Øà½Øºá (Äâ !8ãäå¥)

determined Ým232 and "23 uniquely.

#23

Ým

23

2

LMS

12-n23- !"#$%&æ|ßÚç#Y(��èpéC

Ým

12

2

#12

+ Cabbibo Angle

13- æ|ßÚç#Y(êéCsin22$13 < 0.1, |Ým13

2| = 2.4x10-3 eV2, %CP = CP violation phase?

ëìr_íÄn`aaîd

/////¦ï8&#Xxðñò

óôr_íõÄnïÉÉ�d

/////¦b8&#Xxðñò

l>.!"#$%&8-@Normal

L

H

Ne

m!

Normal @Aö÷

Inverted

L

H

Inverted @Aö÷

Ne

3

2

1

2

1

3

!"#$%&@A

1.øù

1.øù

!"#$%&@A

úû_üýþ8ÿd////////üýþ8!"

üýþ!"#$%&L@æ|_MSWd#$'

%lÿh&�séC��'}8()?Wolfenstein (1978), Mikheyev & Smirnov (1986)n*ì�ë+r_,-.d

SN1987A!"#$%&h KAMIOKANDE & IMB D�

/�k00_11.2d!"#$%&83/ Davisr

/�kÄâ_à"#>.2d!"#$%&83/ëìr_íÄd

4é)5/b¨©8!"#$%&_!e !µ !&d(

æ|RsOGp6V76�?Pontecorvo (1957)n8�, �9ì_1962d

æ|8:'e;<p4=KVsGFG? /$13, 'm13, %CP?

JÑÒÓr_íÄ, 1987d

NS He HO/CSi ONi

7Li, 11

B

11B, 15

N, 19

F

138La, 180

Tar-process

Neutrino%lÿ (!-Process)

�>,-.þ*r N! ~ 1058

ÿ÷8�.?'NOPQ: The !-process(e.g., Woosley et al., 1990; WW95; Heger et al. 2005; Yoshida et al. 2004, 2005)

üýþ!"#$%&

! + (Z, A) @A(Z-z, A-a) + az + !’

!e + (Z, A) @A(Z-z+1, A-a) + az + e-

!e + (Z, A) @A(Z-z-1, A-a) + az + e+

Neutral current¬B

Charged current¬B

E!e = 12MeV

E!e = 20MeV

E!µ& = 24MeV

Before

Explosion

M

ass F

racti

on

After

Explosion

(C10 s)

Si O-Ne-Mg O/C He/C He/N H

M

as

s F

rac

tio

n

!-processes

in outer layers?!

!

!

!

SN-Neutrino Oscillation (MSW) Effect on !-Process

Conversion Probability Supernova

Density Profile & Resonance

H-Resonance

138La, 180Ta 15N, 19F 7Li, 11B

Parameters:

25Msolar SN model (Hashimoto & Nomoto 1999)

- sin22$13 = 0.04

- Ým132 = 2.4x10-3 eV2

- L! = 3x1053 erg, &! = 3 sec Fermi-Dirac distr. of !-spectrum,

so that the observed 11B abundance

- E!e=12MeV, E!e=20MeV, E!µ& =24MeV in Supernova Nucleosynthesis is reproduced.

!e

!e!µ !&

!µ !&

!µ !&

!µ !&!e

!e

Adiabatic

Non-Adiabatic

7

Supernova !-Process & Key Reactions

Yoshida, Kajino & Hartman,

Phys. Rev. Lett. 94 (2005), 231101

(!(E): SM cal.

!

! ~15%

~85%

H-Resonance

MSW (matter)

Neutrino Oscillation

Effect

Additional Charged Current Int.

!µ&(!µ&) !e (!e)&

energetic energetic

Center

outside

E!

E!

!e –spectrum

Low-E comp. disappears !

High-E comp. appears !

&µ, && &e

Neutrino Oscillation (MSW Effect) through

propagation

Parameters:

25Msolar progenitor SN model

(Hashimoto & Nomoto 1999)

- sin22$13 = 0.04

- Ým132 = 2.4x10-3 eV2

- L! = 3x1053 erg, &! = 3 sec

- T!e=3.2MeV, T!e=5.0MeV, T!µ& =6.0MeV

7Be, 11C abundance

SN Nucleosynthesis with Neutrino Oscillations

10-9

10-8

10-7

10-6

10-5

2 3 4 5 6M

as

s F

ra

cti

on

Mr / M

11B

11C

O-rich O/C He/C He/N

10-10

10-9

10-8

10-7

10-6

2 3 4 5 6

Ma

ss

F

ra

cti

on

Mr / M

7Be

7Li

O-rich O/C He/C He/N

no mix no mix

mix

no m

ix

mix

mix

Supernova nucleosynthesis (!-process)

16.2 M star supernova model corresponding to SN 1987A

Increase by a factor of 2.5 and 1.4

Increase in the rates of charged-current reactions4He(!e,e

-p)3He and 12C(!e,e-p)11C in the He layer

Normal mass hierarchy, sin22!13 = 0.01

Yoshida, Kajino, Yokomakura, Kimura,Takamura &

Hartmann,

PRL 96 (2006) 09110; ApJ 649 (2006), 349.

10-6 10-4 10-2

NO 13-mixing

L

T!e < T!e < T!µ&, !µ&

3.2MeV 5.0MeV 6.0MeV

= ==

larger effect !

Normal

Mass Hierarchy

L

Ne

m!

H-Resonance

Normal

Inverted

smaller effect !

H-Resonance

Inverted

Ne

m!

7Li/11B

Normal

Mass Hierarchy

Inverted

10-6 10-5 10-4 10-3 10-2 10-1

No Mixing

7Li/11B - Ratio

Long Baseline Exp:

T2K (Kamioka)

T2KK (KOREA)

Double CHOOZ

Daya Bay

Astrophysics:

Mass Hierarchy

Ým132

13-Mixing Angle$13

Yoshida, Kajino, Yokomakura, Kimura,Takamura

& Hartmann, PRL 96 (2006) 09110; ApJ 649 (2006), 349.

11B DEF C 2497 A _��GHId 11B/10B, JKLMþDNBp¿O! Rebull et al. ApJ 507 (1998) 387; Proc. (2000)

7Li DEF C 6708 A (�P�GHI)

7Li & 7Li/6Li,JKLMþDNBp¿O!////Many observations (1982 – present)

7Li/11B-\�iB8åQNB8()

üýþ1987A RS *pþT_üýþRSd JKLMþ8NB

////êBC////////////êBC////////////BC¿O

(1) ÄGHIn��GHIp��üýþ8U]èNB

X V¸Wº/_üýþ��d

Y & Z V¸Wº _AGBþ��d

Y & Z V¸Wº _ýþ��d

(2) ¹¸X#Ú#V¸Wº_Y%ZºØ#¼W$d8[\

How to know SN !µ&-Spectrum ?Grav. Potential

constraint

Woosley & Weaver ApJS 101 (1995), 181.

OVERPRODUCTION

GCE constraints on 11B

from meteoritic 11B/10B Yoshida-Kajino-Hartmann (2005)

Consistent with

Thomas-Janka et al.

2004/_MPA)

Yoshida, T., Kajino, T., and Hartmann, D., PRL 94 (2005), 231101.

Galactic Chemical Evolution of 9Be & 10,11B

Overproduction

OLD stars SUN 16

17

Livermore Model Woosley and Weaver ApJS 101 (1995) 181.

T!µ,& = 8 MeV

T!µ,& = 6 MeV

Yoshida, Kajino & Hartmann,

PRL 94 (2005), 231101.

/ ]11B has two origins:

// Supernova !)process

//Galactic Cosmic Rays

/////// (GCR)

/] 9Be has pure GCR.

/] 11B >> 10B

Constraints on neutrino temperatures

WBP+SFO

SPSDMK+PSDMK2

Yoshida, Kajino, Hartmann,

PRL 94 (2005)

SN contributions in GCE:

WBP+SFO

-2.0

Probing !-4He Cross Section

4He("NT,n)3He(4He,p)6Li

4He("NT,p)3H(4He,n)6Li

New measurement

using inverse-Compton "-rays !

Shima et al.

Phys. Rev. C72 (2005) 044004

+ New Experiment (2008)

4He(!, !’), 4He(!e, e- ), 4He(!e, e

+)

4He("NT, n)3He and 4He("NT, p)3H

No renormali- Good probezation, needed! for !-A!

( ')2 2

IV VV

A

i gV g q p p

m m

A g

!

!

" # + +

"

r r r r r

r r

EM-current = V, Weak-current = V - A

Gamow-Tellar operator =

±! "#J

r ][rr±!"

r

Spin-Dipole operator =

Weak operator in non-relativistic limit

Similarity between Electro-Magnetic & Weak Interactions

We still don’t have the !-beam !

However, we can use Electro-Magnetic PROBE !

4He("NT, n)3He and 4He("NT, p)3H

4He(!, !’), 4He(!e, e- ), 4He(!e, e

+)

Counts

Excitation Energy (MeV)

0 2 4 6 8 10 12 14

Charge Exchange Reactions ///B(GT)

////////////////////////// Y. Fujitar_^Äd58Ni(3He, t)58Cu E = 140 MeV/u

58Ni(p, n)58Cu Ep = 160 MeV

Y. Fujita et al., EPJ A 13 (’02) 411.

H. Fujita et al., PRC 75 (’07)

J. Rapaport et al.

NPA (‘83)

4He (7Li,7Be)

From S. Nakayama group (Tokushima University)

Charge Exchange Spin-Flip & -Nonflip Reactions

Neutrino induced reactions

on 12C and 4He

! New Shell-Model Hamiltonian in p-sd shell:

! SFO = Suzuki, Fujimoto & Otsuka, PR C67, 044302 (2003)

"Enhanced spin-isospin interactions

Proper tensor components

� Improved spin and magnetic properties

Proper shell evolution

Effective Single-Particle Energy

///// for N=8 Nuclei

Effects of Tensor Force on Shell EvolutionOtsuka, Suzuki, Fujimoto, Grawe, Akaishi, PRL 69 (2005)

Exp: LSND

PR C64 (2001)

EXPAllen et al.

(1990)

DAR ! spectra Exclusive 12C @/12N (1+)

]_FO*: gAeff/gA=0.95

/Suzuki, Chiba, Yoshida, Kajino, Otsuka,

//PR C74 (2006)]`BP: Warburton-Brown

]aT: Hayes-Towner, PR C62, 015501 (2000)

p:Cohen-Kurath (8-16)2BME, sd: USD of Wildenthal,

pf: KB3, p-sd and others: Millener-Kurath

]bCSM: Hayes-Navratil-Vary, PRL 91 (2003)

AV8’(2-body) + TM’(99) (3-body)

]cRPA: Kolb-Langanke-Vogel, NP A652, 91 (1999)

Inclusive = Exclusive (1+g.s.) + Excited state!h3"

Exp:

LSNDPR C64

(2001)

2d: gAeff/gA = * 0.75 *0.70

Cf. Gaarde et al.

q= 0.65 (CK)Quenching of spin-dipole strength

2-

!Cross Section Dependence on 7Li/11B-ratio

Previous SM-(!(E) of Haxton

Woosley, Haxton, Hoffmann, Wilson, ApJ. (1990).

Hoffmann & Woosley, ApJ. (1992).

New SM-(!(E) using WBP(4He) &

SFO(12C) interactions

Suzuki, Chiba, Yoshida, Kajino & Otsuka,

Phys. Review C74 (2006), 034307.

Haxton (1990) Suzuki et al. (2006)

Hoffman & Woosley

(1992)

Almost the same result ! ! 7Li/11B-ratio is SM independent !

0.6

!"#$%&e#Ùp��fg��(DEFG*+J-PARK !-Physics p²h?

/////////////// SUMMARY

`iNBè���_based on ,-NBdejGkekV¼º±²

��8lm8n�(nl>.o�p%l8��h4=��L\]n�8qr-hs�tK7km±²��'GU�®èFuvD8!"#$%&nU.'�.?'8NOPQh4=��w'(n��lm'xyL@_ü´µ->.nz8l>.d83h4=��k{pqrD5�m

2i!"#$%&L@æ|#$_MSW#$deüýþ!"#$%&|}DPrV� 7Li, 11B, 138La, 180Ta z8%lÿAp~����h�øpn���w'DnêC8!"#$%&ÂÃ� "13 '@Aö÷Ým13

2 h��péCDE���-e5�m

bi!"#$%&��.?¬Bh��F�L\��DéC��w'(nekV¼º%lÿpou�xyl>.8:�h4=Rno8ñòl>.D5�ü´µ->.8@Ah�®Rn!"#$%& �

�2 (��2) üýþ��¿O8°8§2h¯�sG���-e

5�m