æ±äº¬å¤§å­¦å®‡å®™ç·šç ”ç©¶æ‰€ 理論グループ

2 2
G
M
0
0
-5
/ M G
0
5
10 0 0.5
L SUGRA = − 1 2 eR + eg ij ∗ ˜Dµ φ i ˜Dµ φ ∗j − 1 2 eg2 D (a) D
[]
1
/ M G
+ieg ij ∗χ j ¯σ µ ˜Dµ χ i + eɛ µνρσ ψ µ¯σ ν ˜Dρ ψ σ
− 1 4 ef R (ab) F (a)
+ i 2 e [
µν F µν(b) + 1 8 eɛµνρσ f I (ab) F (a)
λ (a) σ µ ˜Dµ λ (a) + λ (a)¯σ µ ˜Dµ λ (a) ]
− 1 2 f (ab) I ˜D
[
µ eλ (a) σ µ λ (b)]
MD5
µν F ρσ
(b)
2011611

2011611

•
•
•
•
•
2011611

2011611

-16
100 GeV10 cm
•
•
•
•
•
2011611

•
•
•
•
•
•
•
•
2011611

WMAP
http://map.gsfc.nasa.gov/
2011611

PLANK 2013?
http://www.rssd.esa.int
2011611

•
•
•
• Extra-Dimension
2011611
http://map.gsfc.nasa.gov

• 20
• (SLAC Spires)
http://www.yukawa.kyoto-u.ac.jp/spires/hep/
find ea Kawasaki, Masahiro or a Ibe, Masahiro
2011611

2011611

• gravitino
Kawasaki, Kohri, Moroi (2005)
2011611

• Q-
Hiramatsu, Kawasaki, Takahashi (2010)
Q
2011611

•
Hiramatsu, MK, Sekiguchi, Yamaguchi, Yokoyama (2010)
differential spectrum !P free (k;12.25t crit ,25t crit )
10 3
10 2
10 1
10 0
0 50 100 150 200
10 -1
10 -2
comoving wavenumber k
2011611
Figure 7: Differential energy spectrum of radiated axions between t 1
= 12.25t cr

4
•
PAMELA
COSMIC RAYS FROM DARK MATTER ANNIHILATION AND ... PHYSICAL REVIEW D 79, 083522 (2009)
In this section, we calculate the abundances of light
elements for several different DM scenarios, taking account
of nonthermal production processes discussed in
the previous section. Then, we compare the theoretical
results with observational constraints to derive the upper
bound on hvi. As we will see below, the constraints on the
cross section depend on the dominant annihilation process;
if DM dominantly annihilates into charged leptons and/or
photons, the photodissociation processes are the most important
effect, while the hadronic effects become more
significant when colored particles are produced by the
annihilation. In the following, we consider several typical
cases.
2011611
A. Charged-leptonic modes
The simplest way of explaining the PAMELA and ATIC
anomalies is to adopt the possibility that DM dominantly

5
•
Shift symmetry
superpotential
Kähler potential
Φ ⇒ Φ + iC
K = c(Φ + Φ ∗ )+(Φ + Φ ∗ ) 2 + |X| 2
MK, Yamaguchi, Yanagida (2000)
W = mXΦ
V/m 2 M
2 G
100
1
chaotic inflation
0
-10
-5
/ M G
0
5
10 0 0.5
/ M G
2011611

•
•
•
•
• (IPMU)
• A5 (A1)
2011611

•
•
•
2011611

• M1
•
• M2
•
• 12
hep-ph, astro-ph
• 1~D3
•
•
2011611

H16 H17 H18 H19 H20 H21 H22
2 2 2 1 2 3 3
0 0 1 1 1 0 1
H16 H17 H18 H19 H20 H21 H22
2 0 1 1 0 2 1
1 0 0 1 2 0 0
KEK 1
1
1
1
2011611