1. 2007-01-182007- 01-18 The Evolution & Structure of Pulsar Wind Nebulae Gaensler, B. M., & Slane P.O. ARA&A, 2006, 44:17

2. 2 Observational : Gaensler, B. M., & Slane P.O. ARA&A, 2006, 44:17Observational : Gaensler, B. M., & Slane P.O. ARA&A, 2006, 44:17 Theoretical : Reynolds & Chevalier, 1984, ApJ, 278:630Theoretical : Reynolds & Chevalier, 1984, ApJ, 278:630 (RC84) Swaluw, et al., 2004, A&A, 420:937; Chevalier, 2005, ApJ, 619:839 References

3. 3 SNR => pulsar-driven SNR => PWN Prototype: Crab

4. 4 The Prototype—Crab nebula SN 1054 Central star 16m  pulsar P=33 ms Pdot=36 ns/day Edot~5*10^38 erg/s L~3*10^38 erg/s Pulsar-driven wind nebula

5. 5 Theoreticall Theoretically Marvelous testing ground for studying –Relativistic flows and their interactions with surrounding –Shocks –Pulsar itself –Mechanisms of high v birth kicks of pulsars –etc.

6. 6 Theory of pulsar & radiation Spin-down –Edot –n –Age –B Evolution –P(t) –Edot(t) Crab (Pacini & Salvati 1973) (Manchester & Taylor 1973)

7. 7 Goldreich & Julian 1969 Kennel & Coroniti 1984a,b Bogovalov & Khangoulyan 2002 Bogovalov et al. 2005 Pulsar Wind-magnetodynamic

8. 8 Emission & Spectra of nebulae Radio: X-ray: Synchrotron (Ginzburg & Syrovatskii, et al., 1965)

9. 9 Emission & Spectra of nebulae (Ginzburg & Syrovatskii, et al., 1965) ν r expected increase:Δα = 0.5, <typically observed Δαinferred at low ν  high B Steepening of spectrum with time: Relic breaks in the spectrum can be produced by a rapid decline in the pulsar output over time, and these breaks propagate to lower frequencies as the PWN ages (Pacini & Salvati 1973). Steepening of spectrum with radius: … (Kennel & Coroniti 1984) –Mixing of electrons of different ages at each radius?  diffusion?

10. 10 The nature of this spectral steepening is not understood; theory above is based on a simple pow-law assumption. Rapid decline of injection (  inherent spectrum deviate from power-law?), modifications from discrete acceleration sites, all contribute to a complicated integrated spectrum. “As a result, the interpretation of spectral steepening as being due to synchrotron losses can lead to drastically wrong conclusions about PWN properties.” Emission & Spectra of nebulae

11. 11 Observationally Detailed structrues: Crab especially 40-50 PWN Category: –Composite (with a shell-like SNR) –Crab-like –Cometary (pulsar with high v, few) Evolution  Evolution

12. 12 Evolution Phase I: t<τ, expand into homogeneous ejecta –Phase II(if sweep core slow ejecta all up): constant-mass shell Phase III : t>= τ,Edot down Phase IV: reverse shock pass (theoretical, eg., RC84)

13. 13 Evolution Phase I – Expanding into Unshocked Ejecta Phase II – Interact with SNR Reverse Shock Phase III – Inside a Sedov Shock Phase IV – Pulsar in Interstellar Gas

14. 14 Phase I – Expanding into Unshocked Ejecta

15. 15 Phase I

16. 16 Chevalier, 1977 RC84

17. 17

18. 18

19. 19 Wind Termination shock γ>~10^6 Bpwn ~ 300 μG (Crab) Bpwn ~ 80 μG (3C58)

20. 20 Torus, Jet, Wisp & Filament

21. 21 Torus σ P y ~ 0.25 pc (Bogovalov & Khangoulyan 2002, 2005)

22. 22 Theory: Invisible in standard model Observation: visible! kink instabilities in the toroidal field accelerate particles  limit collimation  curved jets a wide variation in fraction of Edot  considerable differences in the additional acceleration efficiency Jet

23. 23 Enhancement on Torus Doppler beaming & relativistic effect Crab: v ~ c/3 (0.2c – 0.6c) φ~ 30 deg.  I near /I far ~ 5 (Pelling, et al., 1987)

24. 24 G54.1+0.3: luminosity, geometry Puzzles (Lu et al., 2002)

25. 25 Crab: –inner ring (uniform) –variable knots (~months) unstable quasi-stationary shocks outside the termination shock at high latitudes (  large σ  small shock radius) (Komissarov & Lyubarsky 2004) Puzzles

26. 26 G320.4-1.2

27. 27 Wisp (Koji Mori, 2002) ACIS-S3 (11/3/2000- 4/6/2001) v ~ 0.5c (Heter et al. 2002)

28. 28 Variation nature: unveiled –Synchrotron instabilities –Cmpression of e/e + pair plasma (~0.15 pc) Radio structures (VLA) similar to optical/X-ray  accelerate in the same region as for the X-ray emitting population (Bietenholz et al. 2004) Wisp

29. 29 Optical: –R-T instabilities as the expanding relativistic bubble sweeps up and accelerates slower moving ejecta (Hester et al. 1996) –simulation  60-75% mass concerntration (eg.,Jun 1998) Filaments

30. 30 Radio: –Expanding PWN encounters filaments, compress & increase n & B  enhance synchrotron emission (Jun 1998, Bucciantini et al. 2004) No X-ray: –High energy electron suffer synchrotron loss Filaments

31. 31 X-ray filaments of 3C58: associated with radio, not with optical different mechanism -magnetic loops torn from the toroial field by kink instabilities Filaments

32. 32 Phase II – Interact with SNR Reverse Shock

33. 33 Phase II Phase III

34. 34 Phase III – Inside a Sedov Shock

35. 35 Phase II Phase III

36. 36 Phase IV – Pulsar in Interstellar Gas

37. 37 Phase III Phase IV

38. 38 V PSR ~ 400-500 km/s, 1000 km/s Bow shock & Cometary PWN

39. 39 Very young pulsar & PWN –Crab, 3C58(1181?), SN1987A, SN1986J Winds from highly magnetized NS TeV Observations of PWN –Crab (Weekes et al. 1989, etc.) Pulsar Winds in Binary Systems –Double pulsar PSR J0737-3039 –PSR B1957+20, PSR B1259-63 Other & Recent results

40. 40

41. 41 Thank you for your attention!