SLIDE 1 The modeling of the Vela pulsar pulses -
- from op5cal to hard gamma-rays
Bronek Rudak
in collabora5on with J. Dyks Nicolaus Copernicus Astronomical Center (CAMK) Poland
ICRC 2017, Busan, Korea
SLIDE 2
In the talk
1) 3D Outer-Gap model of Very-High-Energy emission expected from Vela-like pulsars: − the origin of the VHE component, − its temporal (pulses) and spectral proper5es. 2) A case for coexistence of the outer gap and an inner gap in the magnetosphere of the Vela pulsar: − the forma5on of core-like pulses in op5cal, UV and in hard X-rays, aligned in phase with the core-like radio pulse (as observed)
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CTA ?
The many faces of the Vela pulsar
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Picture from Benoit CeruW
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Outer gap: primary pairs with ϒ > 107, curvature photons in gamma
Not to scale drawing
Secondary pairs layer: ϒ ~ 100 – 1000, synchrotron photons in op5cal-IR
Hot surface, TBB = 106 K
μB
Inner-Gap pairs, ϒ ~ 100 - 1000 Core emission in coherent radio
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- 1. Primary OG pairs + op5cal-IR photons
(synchrotron photons)
- 2. Inner Gap pairs + op5cal-IR photons
(synchrotron photons)
- 3. Inner Gap pairs + thermal X-ray photons
Processes Results
pulsed VHE component pulsed core op5cal comp. pulsed core hard X-rays comp.
SLIDE 7
The first step: determine α − inclina5on angle (between Ω and μ ) and ζ − viewing angle (between Ω and kobserver ) by reconstruc5ng simultaneously the shapes and phases of the observed main peaks in op5cal and gamma using the „geometrical” version of the OG model. The next step: use α and ζ in the physical OG model.
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Gouiffes 1998 Abdo+ 2010
Two main pulses from Vela in op5cal and gamma rays and their reconstruc5on in a uniform-emissivity version of the OG model,
inclina5on angle α = 70o, viewing angle ζ = 79o
P1 P2 P1 P2 P3
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The OG model - ICS component in VHE α = 70o
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CTA South 50h
Phase-averaged gamma-ray SED in OG model of Vela
Curvature radia5on component ICS component: con5nuous – sok photon field
dashed – sok photon field
α = 70o, ζ = 79o
SLIDE 11
α = 70o The ICS core component in op5cal-UV
P3
SLIDE 12
The ICS core component in hard X-rays α = 70o
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Summary
1) The VHE domain
− Forma5on of pulsed VHE-spectral component is possible in the Vela pulsar in the case of high inclina5on angle, − its lightcurve consists of two pulses at phases ~0.2 and ~0.6, − its expected phase-averaged flux may be of interest to CTA South (for > 50h).
2) The opFcal-UV and the hard X-rays domains
If an inner gap with e--e+ pairs coexists with outer gaps, then
− core-like pulses can form in op5cal, UV and hard X-rays, − they are in phase with the core-like radio pulse (as observed in Vela).
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Back-up slides
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The OG model - Curvature Radia5on component at HE α = 70o
