Leptonic secondary emission in a hadronic microquasar model

TL;DR

This paper models the broadband emission of microquasars considering hadronic interactions, secondary leptons, and electromagnetic cascades, predicting phase-dependent variability in the spectrum.

Contribution

It provides a comprehensive hadronic microquasar model including secondary leptonic emission and electromagnetic cascades, which was not fully addressed in previous models.

Findings

Secondary emission can dominate at ~1 MeV.

Electromagnetic cascades significantly distort high-energy spectra.

Spectral variability is modulated by the orbital period.

Abstract

Context: It has been proposed that the origin of the very high-energy photons emitted from high-mass X-ray binaries with jet-like features, so-called microquasars (MQs), is related to hadronic interactions between relativistic protons in the jet and cold protons of the stellar wind. Leptonic secondary emission should be calculated in a complete hadronic model that include the effects of pairs from charged pion decays inside the jets and the emission from pairs generated by gamma-ray absorption in the photosphere of the system. Aims: We aim at predicting the broadband spectrum from a general hadronic microquasar model, taking into account the emission from secondaries created by charged pion decay inside the jet. Methods: The particle energy distribution for secondary leptons injected along the jets is consistently derived taking the energy losses into account. We also compute the spectral energy distribution resulting from these leptons is calculated after assuming different values of the magnetic field inside the jets. The spectrum of the gamma-rays produced by neutral pion-decay and processed by electromagnetic cascades under the stellar photon field. Results: We show that the secondary emission can dominate the spectral energy distribution at low energies (~1 MeV). At high energies, the production spectrum can be significantly distorted by the effect of electromagnetic cascades. These effects are phase-dependent, and some variability modulated by the orbital period is predicted.