shock
j j
32
45
23/2
23/2
v ;
;
;
0
000
0
crl
rl
rl
rl
rl
negligible dissipation
partial dissipation
total dissipation
eBmcr 1
2
0
l
RlBB 0
2
2
5.2
2/1
20
41 ;c
BmceL
mc
leBlR
Total dissipation of alternating fields at the shock if
In pulsars 63 10...10...120 mc
leB
5.2
2/1
0 mceL
lR Total dissipation in a freely expanding flow at
Termination shocks in PWNe at lR
Bow shocks in binary pulsars at lR 310Dissipation at shocks in AGNs: Levinson & van Putten 1997
in GRBs: Fan, Wei & Zhang 2004
;)2/1( cPl
tan v;ln1)0,0( in
tan20 cBB l
x
clc 1.0v )/ln(4in
Time dependent reconnection: Tolstykh, Semenov & Heyn, poster 48
,0
z out
out
BB
1
0 2
2 20 ,in z outB B v
1/out
energy balance
pressure balance
0in, v BB outz
2
40 3 2
2.
sout
routz
h
B
B0
Bz,out
vin
out
2inv
10
, B
B inz
reconnection force-free MHD turbulence
cascade dissipation
Thompson & Blaes 1998; Troischt & Thompson 2004; Cho 2005; Luo & Melrose 2006
Conclusions
1. In freely expanding outflows, r’B/l’ grows with the distance; however total dissipation of alternating field generally
occurs at too large distance 2 .Dissipation at the termination shock is a plausible
mechanism, at least in pulsar winds
3 .Fast reconnection of tangled field is possible if l’<R/At >>1, magnetic energy is generally not transferred
to the plasma. Dissipation via turbulent MHD cascade?