High-energy gamma-ray emission from the inner jet of LS I+61 303: the hadronic contribution revisited

Abstract

LS I+61 303 has been detected by the Cherenkov telescope MAGIC at very high energies, presenting a variable flux along the orbital motion with a maximum clearly separated from the periastron passage. In the light of the new observational constraints, we revisit the discussion of the production of high-energy gamma rays from particle interactions in the inner jet of this system. The hadronic contribution could represent a major fraction of the TeV emission detected from this source. The spectral energy distribution resulting from p-p interactions is recalculated. Opacity effects introduced by the photon fields of the primary star and the stellar decretion disk are shown to be essential in shaping the high-energy gamma-ray light curve at energies close to 200 GeV. We also present results of Monte Carlo simulations of the electromagnetic cascades developed very close to the periastron passage. We conclude that a hadronic microquasar model for the gamma-ray emission in LS I +61 303 can reproduce the main features of its observed high-energy gamma-ray flux.

arXiv comment6 pages. Sligth improvements made. Accepted version by Astrophysics and Space Science

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Cited by in corpus (9)

• Accretion vs colliding wind models for the gamma-ray binary LS I +61 303: an assessment
• A magnetar-like event from LS I +61 303 and its nature as a gamma-ray binary
• A compact pulsar wind nebula model of the gamma-ray loud binary LS I +61 303
• Leptonic secondary emission in a hadronic microquasar model
• Long-term TeV and X-ray Observations of the Gamma-ray Binary HESS J0632+057
• Gamma-gamma absorption in the $\gamma$-ray binary system PSR B1259-63/LS 2883
• Dynamical and radiative simulations of $\gamma$-ray jets in microquasars
• Results from MAGIC's first observation cycle on galactic sources
• LS I+61 303: microquasar or not microquasar?