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Massive hot stars produce dense ultraviolet (UV) photon fields in theirsurroundings. If a very high-energy (VHE) gamma-ray emitter is located close tothe star, then gamma-rays are absorbed in the stellar photon field, creatingsecondary (electron-positron) pairs. We study the broadband emission of thesesecondary pairs in the stellar photon and magnetic fields. Under certainassumptions on the stellar wind and the magnetic field in the surroundings of amassive hot star, we calculate the steady state energy distribution ofsecondary pairs created in the system and its radiation from radio togamma-rays. Under the ambient magnetic field, possibly high enough to suppresselectromagnetic (EM) cascading, the energy of secondary pairs is radiated viasynchrotron and single IC scattering producing radio-to-gamma-ray radiation.The synchrotron spectral energy distribution (SED) is hard, peaks around X-rayenergies, and becomes softer. The IC SED is hard as well and peaks around 10GeV, becoming also softer at higher energies due to synchrotron loss dominance.The radio emission from secondary pairs is moderate and detectable as apoint-like and/or extended source. In X-rays, the secondary pair synchrotroncomponent may be dominant. At energies <10 GeV, the secondary pair IC radiationmay be the dominant primary gamma-ray emission and possibly detectable by thenext generation of instruments.

Non-thermal emission from secondary pairs in close TeV binary systems