supernova -nucleosynthesis and -oscillation
TRANSCRIPT
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
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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$13 < 0.1, |Ým13
2| = 2.4x10-3 eV2, %CP = CP violation phase?
ëìr_íÄn`aaîd
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l>.!"#$%&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
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