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High-mass microquasars (HMMQs) are systems from which relativistic jets arelaunched. At the scales of several times the binary system size, the jets areexpected to follow a helical path caused by the interaction with a strongstellar wind and orbital motion. Such a trajectory has its influence on thenon-thermal emission of the jets, which also depends strongly on the observingangle due to Doppler boosting effects. We explore how the expected non-thermalemission of HMMQ jets at small scales is affected by the impact of the stellarwind and the orbital motion on the jet propagation. We studied the broadbandnon-thermal emission, from radio to gamma rays, produced in HMMQ jets up to adistance of several orbital separations, taking into account a realistic jettrajectory, different model parameters, and orbital modulation. The jettrajectory is computed by considering momentum transfer with the stellar wind.Electrons are injected at the position where a recollimation shock in the jetsis expected due to the wind impact. Their distribution along the jet path isobtained assuming local acceleration at the recollimation shock, and coolingvia adiabatic, synchrotron, and inverse Compton processes. The synchrotron andinverse Compton emission is calculated taking into account synchrotronself-absorption within the jet, free-free absorption with the stellar wind, andabsorption by stellar photons via pair production. Asymmetric light curves areobtained owing to the helical trajectory of the jets. The presence of helicalshaped jets could be inferred from asymmetries in the light curves, whichbecome noticeable only for large jet Lorentz factors and low magnetic fields.Model parameters could be constrained if accurate phase-resolved light curvesfrom GeV to TeV energies were available.

A model for high-mass microquasar jets under the influence of a strong stellar wind