Pulsar Wind Nebulae at High Energies
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Pulsar Wind Nebulae at High Energies Stephen C.-Y. Ng HKU
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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. - PowerPoint PPT Presentation
Transcript of Pulsar Wind Nebulae at High Energies
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Pulsar Wind Nebulae at High EnergiesStephen C.-Y. NgHKU
OutlineWhat are pulsar wind nebulae?Physical properties and evolution
Why study PWNe?Common TeV sources, particle accelerators
Multiwavelength observations of PWNeBroadband SEDSurprise from Fermi: Crab flaring
FAN 4, Jul 9 2013Stephen Ng2Pulsar WindsWhere does pulsar rotational energy go? >1035erg/s < 10% in radiation (mostly -rays) > 90% in pulsar winds
FAN 4, Jul 9 2013Stephen Ng
Credit: D. Page
3Pulsar WindFAN 4, Jul 9 2013Stephen NgCredit: CXC/D.Berry
Termination ShockFAN 4, Jul 9 2013Stephen Ng
Terminationshockcc/3Free -streaming pulsar windEjecta/ISMCredit: P. SlaneShocked pulsar windPulsar wind nebulae: broadband synchrotron bubbles(see reviews by Gaensler & Slane 2006; Cheng 2009)Gaensler & Slane (2006)
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Pulsar Wind NebulaStephen Ng
FAN 4, Jul 9 2013
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NASA/CXC/ESA/2MASS/NRAOBroadband EmissionFAN 4, Jul 9 2013Stephen Ng7Stephen NgCrab NebulaFAN 4, Jul 9 2013
Abdo et al. (2010)SynchrotronIC
Fermi LAT8Why study PWNe?Relativistic shock physicsCosmic ray accelerationImportant TeV sources
FAN 4, Jul 9 2013Stephen NgSironi & Spitkovsky (2011)
Why study PWNe?Relativistic shock physicsCosmic ray accelerationImportant TeV sources
FAN 4, Jul 9 2013Stephen Ng
Aguilar et al. (2013)e+ excess: dark matter decay? Or pulsars/PWNe?Why study PWNeRelativistic shock physicsCosmic ray accelerationImportant TeV sources
FAN 4, Jul 9 2013Stephen Ng
35 TeV PWNe: largest group,~1/4 identified TeV sourcesPWN EvolutionFAN 4, Jul 9 2013Stephen Ngvan der Swaluw et al. (2003)
Free Expansion
FAN 4, Jul 9 2013Stephen Ngvan der Swaluw et al. (2003)Axisymmetric StructureFAN 4, Jul 9 2013Stephen Ng
CXC/D.BerryLyubarsky (2002)14Torus+Jet
Kes 75Gotthelf+00; Ng+ 08
Lu+02; Temim+10G54.1+0.3
Slane+02; 043C 58
Weisskopf+00; Hester+02Crab
Pavlov+01; Helfand+01Vela
Torus ModellingCrabVelaB1706-44J2221+6114J1930+1852 / G54.1+0.3B0540-69J0205+6449 / 3C58J0537-6910 / N157BB1800-21J2021+3651J1833+1034 / G21.5-0.9J1124-5916 / G292.0+1.8Stephen NgNg & Romani (2004; 2008)FAN 4, Jul 9 2013
16Viewing geometryHand of God:FAN 4, Jul 9 2013Stephen Ng
Aharonian et al. (2005)HESS TeVMSH 1552 / PSR B150958
NASA/CXC/SAO/Slane et al.Chandra17Hand of God:FAN 4, Jul 9 2013Stephen NgMSH 1552 / PSR B150958
NASA/CXC/SAO/Slane et al.ChandraRadio
Ng et al. (2013,in prep.)18Free Expansion
FAN 4, Jul 9 2013Stephen Ngvan der Swaluw et al. (2003)Reverse-Shock Interaction
FAN 4, Jul 9 2013Stephen Ngvan der Swaluw et al. (2003)NASA/PSU/PavlovVela XStephen Ng
Aharonian et al. (2006)TeV
Abdo et al. (2010)Fermi
Mattana et al. (2011)
NASA/SAO/CXCX-rays
21G327.11.1FAN 4, Jul 9 2013Stephen Ng
Acero et al. (2012)TeV
Temim et al. (2009)Radio + X-ray
Ng et al. (2013, in prep.)Radiopreliminary
No Fermi Detection22Bow Shock
FAN 4, Jul 9 2013Stephen Ngvan der Swaluw et al. (2003)Bow ShocksSupersonic motion in the ISM bow shocksStephen Ng
CXC/Weiss
ISM ram pressurePulsar wind pressureFAN 4, Jul 9 201324
The Frying PanG315.90.0 / PSR J14375959~ 2000 km/sLongest pulsar tail > 20pcFAN 4, Jul 9 2013Stephen NgNg et al. (2012 )
25PSR J15095850 / G319.90.7
Ng et al. (2010)FAN 4, Jul 9 2013Stephen Ng
Kargaltsev et al. (2008); Ng et al. (2010)X-ray + RadioRadio26
Multiwavelength StudiesFAN 4, Jul 9 2013Stephen NgCrab PWN
Abdo et al. (2010)SynchrotronIC
Synchrotron degeneracy
Multiwavelength StudiesFAN 4, Jul 9 2013Stephen NgAbdo et al. (2010)
MSH 1552 / PSR B1509581D ModellingFAN 4, Jul 9 2013Stephen Ng
Gelfand et al. (2009)Time VariabilityFAN 4, Jul 9 2013Stephen NgCrab Nebula: A Standard Candle?Cospar 7/16/2012Stephen NgWilson-Hodge et al. (2011)
Crab calibration source, flux unit31Time VariabilityFAN 4, Jul 9 2013Stephen NgNASA/ASU/Hester
Highly dynamic systems32Crab PWN
FAN 4, Jul 9 2013NASA/ASU/Hester Stephen Ng33Vela JetFAN 4, Jul 9 2013Stephen NgNASA/CXC/PSU/Pavlov et al.
34Vela JetFAN 4, Jul 9 2013Stephen Ng
Durant et al. (2013)
Ng et al. (2008); Livingstone, Ng et al. (2011)PSR J18460258 / Kes 75FAN 4, Jul 9 2013
200020062009Stephen NgCrab -ray FlaresFAN 4, Jul 9 2013Stephen Ng
Crab FlaresFAN 4, Jul 9 2013Stephen NgStriani et al. (2013)
2013 Mar FlareFAN 4, Jul 9 2013Stephen Ng
Striani et al. (2013); Tavani et al. (2013)39Flare Spectrum
FAN 4, Jul 9 2013Stephen NgStriani et al. (2013)Flare SpectrumFAN 4, Jul 9 2013Stephen Ng
Weisskopf et al. (2013)
SummaryWhat are pulsar wind nebulae?Physical properties and evolution
Why study PWNe?Common TeV sources, particle accelerators
Multiwavelength observations of PWNeBroadband SEDSurprise from Fermi: Crab flaring
FAN 4, Jul 9 2013Stephen Ng42
