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§

..
(Laboratori Nazionali del Gran Sasso, Italy)

. & ..
( )


§ ( WMAP , arXiv:astro-ph/0603449v2): = 1 c . mh2 = 0.1277 + 0.0080 - 0.0079 ( h = 0.732, m = 0.24) bh2 = 0.02229 ‘ 0.00073 h = 0.732 + 0.031 - 0.032 ns = 0.958 ‘ 0.016 = 0.089 ‘ 0.030 8 = 0.761 + 0.049 - 0.048 r0.002 < 0.65 (95% CL) . , , - . - . w p/ = -0.967 + 0.073 - 0.072 (WMAP+SNLS) = 0.716 ‘ 0.055 (WMAP+HST)


§ § WIMPs - - § § - "" "" § § : , "", , - . (DAMA .). LHC . - . ( ) - .



§ -

M

min

= 105 - 108M



(Aloisio, Blasi & Olinto, 2002)


§ (r) = ((r) - )/ пп (3) P (k ): k k = (2 )3P (k )D (k - k ) Transfer function T (k ): Peq(k ) = Pp(k )T 2(k ) 1 (R ) = 2
2 2 0

k 2 dk P (k )W (k , R)

Peq(k ) k n, eq(M ) M -(n+3)/6 n = -3 - 6 - ns = 1 eq(M ) 2 § 10-4 k ln keq fs()
3/2

ln eq (M ) ln M

k kh0

(ns -1)/2

- : H MPl3V 3/2/V § Running-spectral index dns/dk = 0 § (, 1992) (, , , 1997)


§ M M M M
mi n mi n mi n mi n



10-12M (10-7 - 10-6)M 10-4M (10-5 - 10-4)M



(Zybin, Vysotsky, Gurevich, (Schwarz, Hofmann, Stocker, (Loeb, Zaldarriaga, (Bertschinger,

1999) 2001) 2005) 2006)

1 H (t) r el 1 1 dEk 40 del = = d d n0( ) rel Ek dt 2Ek m d td = 3 § 10
-5

( p)
fL -3/4

2

m 100

-1/2

~ M 1 ~ M 1

-2

g 10
1/8



m T d = 150 100

1/4

g 10




MD =

(x,t) t

=

D(t) a2 (t)

x (x, t)

4 (td)3 (td) 10-13M D 3 (free streaming)
t

x=q+ , M
mi n td

v (t) dt/a(t)
-3/2

= M F S = 10

-8

m 100 GeV

-15/8

~ M 1 TeV

g 10

-15/16

M




§ ,

3 60 0.024 N = 62 § 106, m = 1.2 § 10-10M, z = 350 26 (Diemand, Moore & Stadel, 2005)


§
10 10 dn(M) / dlog M [(h-1Mpc)-3] 10 10 10 10 10 10 10
16 15

14

13

12

M-1

11

10

9

8

10

-6

10

-5

10

-4

10 10 10 -1 M [h Msolar]

-3

-2

-1

10

0

10

1

(Diemand, Moore & Stadel, 2005)


§ : int(r) = c, c 0, r R
- c

r < Rc ; , Rc < r < R ; r > R,
10
10

(1)

1.8 (, , 1988)

-profile, c=1.6 10
9

M = 5.1 10 Msolar -profile, c=1.6 M = 1.1 10-6 Msolar M = 1.3 10
-6

-6

Msolar

(r) / crit.(z=0)

10

8

10

7

r200

10

6

10
5

r

200

Rc/R 0.01 (Moore et al., 2005)

10

-3

10 r [pc]

-2


§

Ncl = 4 r2dr2nt(r)m i
0



-2

annv

dNcl = ncl(l, M , R)d3ldM dR ( ) annv Icl = 4
0 rmax ( )

d sin
0

2 r dr r2

2

Mmax

Rmax

dM

dR ncl(l( , r), M , R)N
Rmin

cl

Mmin

Ihom annv = 2
0 rmax ( )

d sin
0

2 (l( , r)) dr DM 2 m

§ Icl + Ihom int п 1 + S (x c , ) Ihom DM ~ : S 5, H 0.3 -3, int 10-20 -3, ~ п - 0.001 = 102


P S dM = (Press, Shechter, 1974)
Small-scale DM clumps in the Galactic halo

2

1/2

2 c deq -c dM exp 2 2 M D(t)eq dM 2D(t)2eq

DM halo
Sun SMBH

Milky Way


E |E | GM 2/2R T -1 = E /|E | , e-J ,
tf

J

Mh

t T

t1

dth 1 - f 1 t2 2 T (, h) t1

- e dM d = dM d M 2
- 2 /2 t0

2F (M , t1) -J dt1 e M t1

(t,t1 )

t( eq )

d e- 2

2

/2

f1( )

d log eq(M ) dM , dM

2[(1/3) - (1/3, )] , f1( ) 0.2 - 0.3 14 < < 40 1/3 3 2 f1( ) = dM dM 0.02(n + 3) , int M M DM(r) ncl(M , R)d ln M d ln R = (M , )d ln M d M (, , , 2003, 2006)


10 10 dn(M) / dlog M [(h-1Mpc)-3] 10 10 10 10 10 10 10

16

15

14

13

12

M-1

11

10

9

8

10

-6

10

-5

10

-4

10 10 10 -1 M [h Msolar]

-3

-2

-1

10

0

10

1

(Diemand, Moore & Stadel, 2005)


Stellar components of the Milky Way

DM halo
Halo stars
Central bulge

Galactic disk


§ " " (Ostriker, Spitzer, Chevalier, 1972):
2 4gm(z )2m E = A(a) 2 v z ,c : (Gnedin, Ostriker 1997, 1999), (Gnedin, Hernquist, Ostriker, 1999), (Gnedin, Lee, Ostriker, 1999), (Gnedin, 2003) A(a) - (Weinberg, 1994), (Gnedin, Ostriker 1999) a = d, A(a) = 1 a 1 A(a) 1 a 1 A(a) = (1 + a2)-3/2 (Gnedin, Ostriker 1999) : 0

(r) = 4
U (r)

dE

2[E - U (r)]f (E ) s(r) =
Md 2 2 r0

: gm(r) = 2 Gs(r),

e-r

/r0


§ 1 E = 2 d r (r)(vz - vz ) , E = ~
3 2

2 lvrel dl E (l) n,
l

t-1

= l

2 vrel n

E (l > l) + |E |

: 1 4 2 dp P (x, ) = (x) sin ~
0

sin

1

d cos
0 (x)

d [ - (x)]1/2F ()e-

E /|E |


1

0.8

1 0.75

halo
0.6

0.5

disk Pr
100

Pr

0.25

total
0.4

0 80 60

104 103
40 20

r, kpc
0.2

102

cl, Gev cm3
100

5

10

15

20

25

30

35

r, kpc

(, , , 2006) : M = 10-6M = 2. : cl -3.


§
5

np 1.1
4

log

3

np 1.0

2

1

20

40

60

80

100

r, kpc


§ (),
3.5

np 1.1
3

2.5

log

2

1.5

np 1.0

1

0.5

0 0 25 50 75 100 125 150 175

, degrees

= 1.8, M

mi n

= 2 § 10-8M, np = 1.0 np = 1.1


§
2 2 ~ E = 2gm(z )2/(vz ,c), v
1 0.95 0.9

z ,c

= J sin /(mrc), E /|E | = C / sin2
7 6

5

plane of disk

vertical plane

P r,

0.85
4

0.8 0.75

I

3

2

halo

0.7
1

0.65 0 20 40 60 80

, degree

25

50

75

100

125

150

175

, degree

(, , , 2007) : P (r, ), , - r . r = 3, 8.5 20 ( ). 0.04, 0.4 0.9. : .


§ () j

(E )j |E |

. = ? Rc/R 1.8 Ѕ 10-5 (Gurevich, Zybin, 1995) Rc/R 0.01 (Diemand, Moore, Stadel, 2005) 3- r int(r) = п 3 R
0 - r

,

N

4 r2dr2nt(r) i
0

. : (r) = 2 M M
5/2 R


-

- (r) fcl() d,
1/2 d

M = -4

r2 (r) dr.

0 2 d

d

-0.13Qd exp -1.58S 1 T M M

2 gm 4 , Sd = Gi п , Qd = 2 2 vz ,cGi п 3 x m ax

d

2 ~ Tt||

M M

x min

d

d dx dx


.

Gm2 4 Qs = , Ss = Gi п 2 l4 2 vrel пi 3 1 M dM dt 2T 1 2 G
xmax

2 s

2 l dl
0 R xmin

s

t

- (s) - y /s
3

ds n(s)v

rel 2

M M

s

: m = 0.4M, r = 8.5 , h = 1.4 Ѕ 10-5 M/ nh,(r) = (h/m)(r/r)
3

(Bell et. al, 2007)
6

nb,(r) = (b/m) exp -(r/rb)1. b = 8M/3, rb = 1 (Launhardt, Zylka, Mezger, 2002)


: M (t) R(t), (t) M (t) п dM = dt dM dt +
d

-2

dM dt

s

t0 - tG < t < t0 A(a) = 0: І І3 dІ =- - , dt ts td : : : І(t) M (t)/Mi = (1 + t/td) І(t) = exp(-t/ts) 2td І (t0) = (2td + ts) exp(2t0/ts) - ts
2

І M (t)/M

i

-1/2


§

1 0.75 0.5

1 0.75 0.5

Pr
0.25 1 0 0.8 0.6 2 3 4
0.8 3 4 1 0 0.25

Pr



r, kpc
0.4 1



0.6 2

r, kpc
0.4 1

( -) r xc = 0.1 () xc = 0.05 ().


50
250

40 30
ann

Icl IH

IH

200 150 100 50 0

I

20 10 0 0 25 50 75 100 125 150 175

0

25

50

, degree

75 100 , degree

125

150

175

: . . : (Icl - IH)/IH.


§
1014

dlog M , Mpc

3

1012

3 kpc

1010

dn M

8.5 kpc
108 10 8 10 6 10 4

MM

3 8.5 . .


EGRET - Energetic Gamma Ray Experiment Telescope (30 MeV - 30 GeV)

onboard satellite COMPTON-GRO (Gamma Ray Observatory) SUSY interpretation of EGRET excess of diffuse -rays

(neutralino annihilation in the Galactic halo)
E * flux [GeV cm s sr ]
-1

Dark Matter Pion decay Inverse Compton Bremsstrahlung
-4

EGRET background signal mWIMP=50-70 GeV

-2

-1

1991 - 2000

10

2

-5

10

10

-1

1

10

10

2

E [GeV] de Boer, Sander, Zhukov, Gladyshev & Kazakov astro-ph/0508617, hep-ph/0511154