Документ взят из кэша поисковой машины. Адрес оригинального документа : http://hea.iki.rssi.ru/conf/hea2007/presentations/25.12.2007/01-gnedin.pdf
Дата изменения: Wed Jan 30 21:11:42 2008
Дата индексирования: Tue Oct 2 01:10:15 2012
Кодировка:
Поисковые слова: m 103

: .
.. , . , . , , ~ -G ~ -G. . ( , ) , . . , . . .

: . .., .., . . . . . . . . . . . . . . Neutron Stars: L= B RS sin c

BS = . в pp

B=

eB = . в B ( G me c = ( BS ) KeV

)

B

. . : ( ) . . . -. . : : p B = - b ( ) GHz - , b ( RA = . BS RS M S M

mas ) -

Jy S p

. :

RS M S M D B = M kpc ( p Beq = C ( ) ( + k ) Lsyn ( ) d V ; k = ; = MHz ; e + :

(

)

-

p GHz ):

Jy S p

= GHz

Lsyn Cic Bic = Lic Csyn

+

syn ic

+

;S

-

! . . :
B = . N V µ G V /, .

pos

e

.
: B 7 в 10
-9

(

bh

2

)

12

(Barrow et al. 1997)

Kronberg (1994) + : B < 10- 9 G Cosmological perturbations (Takahashi et al., 2000): B 10 Biermann Mechanism: B 10
- 19 - 19

G at 10kpc co-moving scale.

G (N.Gnedin et al., 2000)
- 14

Rogachevskii et al. (2006): colliding protogalactic clouds B 10 Cosmological MHD simulations (Dolag et al., 2002): B 10

G.

- 2.5 z

µ G.
- 16

Piotrovich et al. (2007): axion magnetic conversion + PVLAS experiment B 10

G

Intergalactic Magnetic Field: Chandrasekhar-Fermi Method.

B=

4 Vturb ; B = 2.64 в 10 3
2 - 29

- 12

fN

e

V , V [ cm s ] , [ radian

]

cr

= 1.125 в 10

H0 3 2 75 g cm ; b h = 0.0224 ± 0.0009 : WMAP 3 year.
- 15

B = 1.375 в 10

f (1+ z

)

32

V ; V =

(

3 2 VFWHM ;

)

B = 1.19 в 10

- 15

(

1+ z

)

32

VFWHM

z 6 , VFWHM 106 , 1,

B 10 - 8 G

Axion Birefringence 1 2 22 = g a B L 8

=

(

g a B ma 48
B > 10
- 12

)

2

L

3

CERN g< 1.4 в 10 a G

-9

(

)

-1

AGN (Equipartition)
R.-Y. Ma, F. Yuan, arXiv:0706.0124. BH = k 2 Lbol c / RH , k 1 Lbo GM = Mc 2 , RH = 2 c
2 a 1+ 1- M

l

BEd

M = 6.2 в 10 M BH
8

1

2

1

2

1 a 1+ 1- M
2

,=

Lbol LEd

.
z Lbol/LE 0. 4 4 0. 5 0 0. 3 1 0. 6 1 0. 9 4 1. 1 1
d

a/M = 0, = 0.057 9. 0x1 0 3 G 1. 5x1 0 4 G 7. 1x1 0 3 G 1. 8x1 0 4 G 3. 5x1 0 4 G 3. 5x1 0 4 G

a/M = 0.95, a/M = 0.998, a/M = 1.0, = 0.19 = 0.32 = 0.42 7. 5 x10 3 G 1 . 2 2x 1 04 G 6. 0 x10 3 G 1. 5 x10 4 G 2. 9 3x10 4 G 2 . 9 3 x1 0 4 G 7. 15x1 0 3 G 1. 16x1 0 4 G 5. 7x10 3 G 1. 43x1 0 4 G 2. 8x10 4 G 2. 8x10 4 G 6. 6 x10 3 G 1. 0 x10 4 G 5. 3 x10 3 G 1. 4 x10 4 G 2. 7 x10 4 G 2. 7 x10 4 G

J0836+0054 5.810 J1030+0524 6.309 J1044-0125 5. 77 8

J1306+0356 6.016 J1411+1217 5.927 J1623+312 6. 24 7

.

to - observation, tS - seed, M

BH

( to )

=M

BH

( tS )

L 1 - to - t S exp ; = , LEdd

Mc 2 = = 0.45 в 109 yrs Salpeter Time (M/ Begelman) LEdd B ( seed ) = BH

(

1 - ( to - t S ) to ) exp 2 M
seed

Two most popular accretion models:

102 M , M

seed

103 M .

.

a = 0:M M

seed

a 10 M , zs = 20 В 30 ; = 0.95 : M M
2

seed

103 M , z s = 20 В 30 ;

(merging), ?!

a = 1.0 : M M

seed

105 M , zs > 20 ;

(seed). SDSS J1044-0125,

zo = 5.778
eed

a = 0.0 : Bs M

eed

= 8.6 в 107 G, zs = 30; Bs

= 4.8 в 107 G, zS = 20; = 1.9 в 107 G, zS = 30;

a = 0.95 : Bs M

eed

= 1.16 в 107 G , zs = 20; Bs

eed

a = 0.998 : Bs M a = 1.0 : Bs M

eed

= 5.0 в 106 G, zs = 30;

eed

= 1.7 в 106 G , z s = 30;

Testing Cosmological Models.
:

p = W , W = - 1 3, W > - 1 zs = 20

a M a M

M seed = 56M (103 M ) a = 0.95 : M Bseed = 8.2 в 107 G (107 G ) M seed = 103 M (105 M ) = 0.998 : Bseed = 5.2 в 107 G (5 в 106 G ) M seed = 1.3 в 104 M ( 105 M ) = 1.0 : Bseed = 4.8 в 108 G (1.7 в 106 G )

a = 0.0 , zs = 10 M
M Bs
seed

= 2 в 104 M (105 M )

eed

= 4.8 в 106 G (1.9 в 106 G )