1. Relativistic reconnection Yuri Lyubarsky Ben-Gurion University, Israel

3. current sheet

4.  B j l

6. shock jj   no dissipation: l

7. shock jj   negligible dissipation partial dissipation total dissipation l

8. Total dissipation of alternating fields at the shock if In pulsars Total dissipation in a freely expanding flow at Termination shocks in PWNe at Bow shocks in binary pulsars at Dissipation at shocks in AGNs: Levinson & van Putten 1997 in GRBs: Fan, Wei & Zhang 2004

9. Particle acceleration: talks by Drake and Hoshino

10. resistivity inflow outflow Reconnection at

11. jet with tangled magnetic fields (Heinz & Begelman 2000) current sheet in the pulsar wind

12. Petschek reconnection

13. slow shock

14. Time dependent reconnection: Tolstykh, Semenov & Heyn, poster 48

15. Relativistic Petschek reconnection in case

18. energy balance pressure balance B0B0 B z,out v in  out 

19. reconnection force-free MHD turbulence cascadedissipation Thompson & Blaes 1998; Troischt & Thompson 2004; Cho 2005; Luo & Melrose 2006

20. 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?