Pulsar Wind Nebulae at High Energies Stephen C

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 Te. V sources, particle accelerators �Multiwavelength observations of PWNe �Broadband SED �Surprise from Fermi: Crab flaring FAN 4, Jul 9 2013 Stephen Ng

Pulsar Winds �Where does pulsar rotational energy go? � � � Ė >1035 erg/s < 10% in radiation (mostly -rays) > 90% in pulsar winds FAN 4, Jul 9 2013 Stephen Ng Credit: D. Page

Pulsar Wind FAN 4, Jul 9 2013 Stephen Ng Credit: CXC/D. Berry

Termination Shock Free -streaming pulsar wind c Shocked pulsar wind Termination shock Ejecta/ISM c/3 Credit: P. Slane �Pulsar wind nebulae: broadband synchrotron bubbles (see reviews by Gaensler & Slane 2006; Cheng 2009) FAN 4, Jul 9 2013 Stephen Ng Gaensler & Slane (2006)

Pulsar Wind Nebula FAN 4, Jul 9 2013 Stephen Ng

Broadband Emission NASA/CXC/ESA/2 MASS/NRAO FAN 4, Jul 9 2013 Stephen Ng

Crab Nebula Fermi LAT Synchrotron IC FAN 4, Jul 9 2013 Stephen Ng Abdo et al. (2010)

Why study PWNe? �Relativistic shock physics �Cosmic ray acceleration �Important Te. V sources FAN 4, Jul 9 2013 Stephen Ng Sironi & Spitkovsky (2011)

Why study PWNe? �Relativistic shock physics �Cosmic ray acceleration �Important Te. V sources FAN 4, Jul 9 2013 e+ excess: dark matter decay? Or pulsars/PWNe? Stephen Ng Aguilar et al. (2013)

Why study PWNe �Relativistic shock physics �Cosmic ray acceleration �Important Te. V sources FAN 4, Jul 9 2013 35 Te. V PWNe: largest group, ~1/4 identified Te. V sources Stephen Ng

PWN Evolution van der Swaluw et al. (2003) FAN 4, Jul 9 2013 Stephen Ng

Free Expansion van der Swaluw et al. (2003) FAN 4, Jul 9 2013 Stephen Ng

Axisymmetric Structure Lyubarsky (2002) FAN 4, Jul 9 2013 Stephen Ng CXC/D. Berry

Torus+Jet Crab Weisskopf+00; Hester+02 G 54. 1+0. 3 Lu+02; Temim+10 Vela Kes 75 Pavlov+01; Helfand+01 Gotthelf+00; Ng+ 08 3 C 58 Slane+02; 04

Torus Modelling Crab Vela B 1706 -44 J 2221+6114 J 1930+1852 / G 54. 1+0. 3 J 2021+3651 B 0540 -69 J 0205+6449 / 3 C 58 J 1833+1034 / G 21. 5 -0. 9 J 0537 -6910 / N 157 B FAN 4, Jul 9 2013 B 1800 -21 J 1124 -5916 / G 292. 0+1. 8 Stephen Ng Ng & Romani (2004; 2008)

Hand of God: MSH 15– 52 / PSR B 1509– 58 HESS Te. V Chandra NASA/CXC/SAO/Slane et al. FAN 4, Jul 9 2013 Stephen Ng Aharonian et al. (2005)

Hand of God: MSH 15– 52 / PSR B 1509– 58 Radio Chandra NASA/CXC/SAO/Slane et al. FAN 4, Jul 9 2013 Stephen Ng Ng et al. (2013, in prep. )

Free Expansion van der Swaluw et al. (2003) FAN 4, Jul 9 2013 Stephen Ng

Reverse-Shock Interaction van der Swaluw et al. (2003) FAN 4, Jul 9 2013 Stephen Ng

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

ry pre Radio Ng et al. (2013, in prep. ) G 327. 1– 1. 1 l na i m i Radio + X-ray n o i t c. Te. V F o N D i m r e Temim et al. (2009) FAN 4, Jul 9 2013 Stephen Ng Acero et al. (2012) e t e

Bow Shock van der Swaluw et al. (2003) FAN 4, Jul 9 2013 Stephen Ng

Bow Shocks �Supersonic motion in the ISM bow shocks ISM ram pressure Pulsar wind pressure CXC/Weiss FAN 4, Jul 9 2013 Stephen Ng

The Frying Pan �G 315. 9– 0. 0 / PSR J 1437– 5959 �~ 2000 km/s �Longest pulsar tail > 20 pc FAN 4, Jul 9 2013 Stephen Ng Ng et al. (2012 )

PSR J 1509– 5850 / G 319. 9– 0. 7 X-ray + Radio Ng et al. (2010) Radio Kargaltsev et al. (2008); Ng et al. (2010) FAN 4, Jul 9 2013 Stephen Ng

Multiwavelength Studies Crab PWN Synchrotron IC Abdo et al. (2010) FAN 4, Jul 9 2013 Stephen Ng

Multiwavelength Studies MSH 15‒ 52 / PSR B 1509‒ 58 FAN 4, Jul 9 2013 Stephen Ng Abdo et al. (2010)

1 D Modelling FAN 4, Jul 9 2013 Stephen Ng Gelfand et al. (2009)

Time Variability FAN 4, Jul 9 2013 Stephen Ng

Crab Nebula: A Standard Candle? Cospar 7/16/2012 Stephen Ng Wilson-Hodge et al. (2011)

Time Variability FAN 4, Jul 9 2013 Stephen Ng NASA/ASU/Hester

Crab PWN FAN 4, Jul 9 2013 Stephen Ng NASA/ASU/Hester

Vela Jet FAN 4, Jul 9 2013 Stephen Ng NASA/CXC/PSU/Pavlov et al.

Vela Jet FAN 4, Jul 9 2013 Stephen Ng Durant et al. (2013)

PSR J 1846 0258 / Kes 75 2000 FAN 4, Jul 9 2013 2006 2009 Stephen Ng Ng et al. (2008); Livingstone, Ng et al. (2011)

Crab -ray Flares FAN 4, Jul 9 2013 Stephen Ng

Crab Flares FAN 4, Jul 9 2013 Stephen Ng Striani et al. (2013)

2013 Mar Flare Striani et al. (2013); Tavani et al. (2013) FAN 4, Jul 9 2013 Stephen Ng

Flare Spectrum FAN 4, Jul 9 2013 Stephen Ng Striani et al. (2013)

Flare Spectrum FAN 4, Jul 9 2013 Stephen Ng Weisskopf et al. (2013)

Summary �What are pulsar wind nebulae? �Physical properties and evolution �Why study PWNe? �Common Te. V sources, particle accelerators �Multiwavelength observations of PWNe �Broadband SED �Surprise from Fermi: Crab flaring FAN 4, Jul 9 2013 Stephen Ng