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Pulsar Wind Nebulae at High Energies

Pulsar Wind Nebulae at High Energies. Stephen C.-Y. Ng HKU. Outline. What are pulsar wind nebulae? Physical properties and evolution Why study PWNe ? Common TeV sources, particle accelerators Multiwavelength observations of PWNe Broadband SED Surprise from Fermi : Crab flaring.

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Pulsar Wind Nebulae at High Energies

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  1. Pulsar Wind Nebulae at High Energies Stephen C.-Y. Ng HKU

  2. Outline • What are pulsar wind nebulae? • Physical properties and evolution • Why study PWNe? • Common TeV sources, particle accelerators • Multiwavelength observations of PWNe • Broadband SED • Surprise from Fermi: Crab flaring Stephen Ng

  3. Pulsar Winds • Where doespulsar rotational energy go? • Ė >1035erg/s • < 10% in radiation (mostly -rays) • > 90% in pulsar winds Credit: D. Page Stephen Ng

  4. Pulsar Wind Stephen Ng Credit: CXC/D.Berry

  5. Termination Shock Free -streaming pulsar wind Shocked pulsar wind • Pulsar wind nebulae: broadband synchrotron bubbles(see reviews by Gaensler & Slane 2006; Cheng 2009) Ejecta/ISM c c/3 Termination shock Credit: P. Slane Gaensler & Slane (2006) Stephen Ng

  6. Pulsar Wind Nebula Stephen Ng

  7. Broadband Emission NASA/CXC/ESA/2MASS/NRAO Stephen Ng

  8. Crab Nebula Fermi LAT Synchrotron IC Stephen Ng Abdo et al. (2010)

  9. Why study PWNe? • Relativistic shock physics • Cosmic ray acceleration • Important TeV sources Sironi& Spitkovsky (2011) Stephen Ng

  10. Why study PWNe? • Relativistic shock physics • Cosmic ray acceleration • Important TeV sources e+ excess: dark matter decay? Or pulsars/PWNe? Stephen Ng Aguilar et al. (2013)

  11. Why study PWNe • Relativistic shock physics • Cosmic ray acceleration • Important TeV sources 35 TeVPWNe: largest group,~1/4 identified TeV sources Stephen Ng

  12. PWN Evolution van derSwaluw et al. (2003) Stephen Ng

  13. Free Expansion van derSwaluw et al. (2003) Stephen Ng

  14. Axisymmetric Structure Lyubarsky (2002) CXC/D.Berry Stephen Ng

  15. Torus+Jet Crab Kes 75 Vela Weisskopf+00; Hester+02 Gotthelf+00; Ng+ 08 G54.1+0.3 3C 58 Pavlov+01; Helfand+01 Lu+02; Temim+10 Slane+02; 04

  16. Torus Modelling Crab Vela B1706-44 J2221+6114 J1930+1852 / G54.1+0.3 J2021+3651 B0540-69 J0205+6449 / 3C58 J1833+1034 / G21.5-0.9 B1800-21 J1124-5916 / G292.0+1.8 J0537-6910 / N157B Stephen Ng Ng & Romani (2004; 2008)

  17. HESS TeV Hand of God: MSH 15–52/ PSR B1509–58 Chandra Aharonian et al. (2005) Stephen Ng NASA/CXC/SAO/Slane et al.

  18. Hand of God: MSH 15–52/ PSR B1509–58 Radio Chandra Stephen Ng NASA/CXC/SAO/Slane et al. Ng et al. (2013,in prep.)

  19. Free Expansion van derSwaluw et al. (2003) Stephen Ng

  20. Reverse-Shock Interaction van derSwaluw et al. (2003) Stephen Ng

  21. Vela X Fermi Mattana et al. (2011) TeV X-rays Aharonian et al. (2006) Abdo et al. (2010) NASA/SAO/CXC Stephen Ng NASA/PSU/Pavlov

  22. G327.1–1.1 preliminary Radio Radio + X-ray Ng et al. (2013, in prep.) TeV No Fermi Detection Aceroet al. (2012) Temim et al. (2009) Stephen Ng

  23. Bow Shock van derSwaluw et al. (2003) Stephen Ng

  24. Bow Shocks • Supersonic motion in the ISM  bow shocks ISM ram pressure Pulsar wind pressure CXC/Weiss Stephen Ng

  25. The Frying Pan • G315.9–0.0 / PSR J1437–5959 • ~ 2000 km/s • Longest pulsar tail > 20pc Stephen Ng Ng et al. (2012 )

  26. PSR J1509–5850 / G319.9–0.7 X-ray + Radio Radio Ng et al. (2010) Kargaltsevet al. (2008); Ng et al. (2010) Stephen Ng

  27. Multiwavelength Studies Crab PWN Synchrotron IC Abdo et al. (2010) Stephen Ng

  28. Multiwavelength Studies MSH 15‒52 / PSR B1509‒58 Stephen Ng Abdo et al. (2010)

  29. 1D Modelling Gelfand et al. (2009) Stephen Ng

  30. Time Variability Stephen Ng

  31. Crab Nebula:A Standard Candle? Stephen Ng Wilson-Hodge et al. (2011)

  32. Time Variability Stephen Ng NASA/ASU/Hester

  33. CrabPWN Stephen Ng NASA/ASU/Hester

  34. VelaJet Stephen Ng NASA/CXC/PSU/Pavlov et al.

  35. Vela Jet Durant et al. (2013) Stephen Ng

  36. PSR J18460258 / Kes 75 2000 2006 2009 Stephen Ng Ng et al. (2008); Livingstone, Ng et al. (2011)

  37. Crab -ray Flares Stephen Ng

  38. Crab Flares Stephen Ng Striani et al. (2013)

  39. 2013 Mar Flare Striani et al. (2013); Tavani et al. (2013) Stephen Ng

  40. Flare Spectrum Striani et al. (2013) Stephen Ng

  41. Flare Spectrum Stephen Ng Weisskopfet al. (2013)

  42. Summary • What are pulsar wind nebulae? • Physical properties and evolution • Why study PWNe? • Common TeV sources, particle accelerators • Multiwavelength observations of PWNe • Broadband SED • Surprise from Fermi: Crab flaring Stephen Ng

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