The puzzling emission of γ-ray binaries
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1 Credit: F. Reddy/NASA/GSFC The puzzling emission of γ-ray binaries Guillaume Dubus with special thanks to Benoît Cerutti & Astrid Lamberts Texas symposium, Dallas, dec Institut de Planétologie et d Astrophysique de Grenoble
2 Binaries > 100 MeV Many types detected in past years by Fermi, AGILE, VERITAS, HESS, MAGIC X-ray binary gamma-ray binary nova colliding wind binary recycled pulsars, black widow see Dubus, 2013, Astron. Astrophys. Rev., 21, 64
3 Binaries > 100 GeV only gamma-ray binaries in very high energy gamma-rays gamma-ray binary
4 Gamma-ray binaries massive non-thermal emission above 1 MeV dominates 5 known systems incl. one with pulsar all rotation-powered?
5 Interacting pulsar wind Termination shock very close to pulsar: down to scale ~10 4 RLC massive star wind shocked stellar wind adapted from Lamberts et al pulsar shocked pulsar wind pulsar wind termination shock 0.1 AU
6 Gamma-ray emission two components : pulsar & pulsar wind nebula (PWN)? Hadasch pulsar-like PWN-like GeV spectra like that of the 100+ Fermi/LAT pulsars TeV (X-ray) emission similar to pulsar wind nebulae
7 Puzzle: pulsar-like component orbital modulation unexpected for pulsar emission within light cylinder Hadasch Abdo pulsar-like PWN-like modulation best understood as inv. Compton on stellar light
8 Puzzle: pulsar-like component orbital modulation unexpected for pulsar emission within light cylinder pulsar-like Hadasch PWN-like origin of pulsar-like component - striped wind (Pétri & GD 2011) - cold wind (à la Khangulyan+ 2012) - thermalized particles at shock (Zabalza+ 2013, GD & Cerutti 2013) - shocked stellar wind (Bednarek 2011) a clue to pulsar emission process?
9 Puzzle: GeV flare of PSR B Fermi/LAT lightcurve (Abdo et al. 2011) orbit close to periastron orbital phasing unexpected for inverse Compton scattering of stellar photons
10 Puzzle: GeV flare of PSR B Fermi/LAT lightcurve (Abdo et al. 2011) max expected here orbit close to periastron orbital phasing unexpected for inverse Compton scattering of stellar photons
11 Puzzle: GeV flare of PSR B Fermi/LAT lightcurve (Abdo et al. 2011) max expected here orbit close to periastron max occurred here orbital phasing unexpected for inverse Compton scattering of stellar photons
12 Puzzle: GeV flare of PSR B Extremely efficient radiation with Lγ ~ spindown power! If inverse Compton, need very high radiation density to allow electrons orbit close to periastron to cool on a scale ~ dorb - Be disc photons? (Khangulyan+ 2012) - SSC on PWN emission? (GD & Cerutti 2013) dorb ~ 4 au
13 Puzzle: GeV flare of PSR B Extremely efficient radiation with Lγ ~ spindown power! If inverse Compton, need very high radiation density to allow electrons orbit close to periastron to cool on a scale ~ dorb - Be disc photons? (Khangulyan+ 2012) - SSC on PWN emission? (GD & Cerutti 2013) dorb ~ 4 au Alternatives to IC - Doppler boosting (GD+ 2010, Kong+ 2012) - conversion to EM wave (Mochol & Kirk 2013) - Crab-like reconnection unrelated to orbit? next periastron : May 2014
14 The puzzling γ-ray binaries Gamma-ray binaries powered by pulsar spindown, energy dissipated in shock with stellar wind new probes of pulsar physics Puzzle: the GeV spectral component Is the similarity with emission from other pulsars telling us something about pulsar physics or... a red herring? Puzzle: the gamma-ray flare of PSR B Is it due to complex inverse Compton geometry (need simulations of interaction region see A. Lamberts, MHD // tomorrow) or is it evidence for alternate emission mechanisms?
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