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Pulsar Emission at 10 – 100 GeV

Pulsar Emission at 10 – 100 GeV. Alice K. Harding (NASA Goddard). Spectral cutoffs TeV component from ICS predicted by outer gap models Millisecond pulsars. Measuring spectral cutoffs. Polar cap r = 2R Outer gap r/r LC = 0.6 r/r LC = 0.7

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Pulsar Emission at 10 – 100 GeV

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  1. Pulsar Emission at 10 – 100 GeV Alice K. Harding(NASA Goddard) • Spectral cutoffs • TeV component from ICS predicted by outer gap models • Millisecond pulsars

  2. Measuring spectral cutoffs Polar cap r = 2R Outer gap r/rLC = 0.6 r/rLC = 0.7 r/rLC = 0.8

  3. TeV inverse compton scattering Konopelko et al. 2005

  4. Millisecond pulsars Pulsed emission from a few millisecond pulsars may be detectable above 50 GeV (and more above 10 GeV) for favorable viewing angle (small angle to magnetic axis) Emission above 10 GeV from millisecond pulsars must come polar cap accelerator

  5. Summary • 100 GeV threshold • Constrain or rule out some outer gap models • Measure or constrain ICS TeV component (but need sensitivity) • 50 GeV threshold • Measure high-energy cutoffs in some pulsars (e.g. 1951+32) • Detect few most energetic millisecond pulsars (e.g. 1957+21, 1821-24) at favorable viewing angles • 10 GeV threshold • Detect a range of millisecond pulsars, even at unfavorable viewing angles • Measure HE cutoffs in all EGRET and many GLAST pulsars

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