Abstract
Microquasar binary stellar systems emit electromagnetic radiation and high-energy particles over a broad energy spectrum. However, they are so far away that it is hard to observe their details. A simulation offers the link between relatively scarce observational data and the rich theoretical background. In this work, high-energy particle emission from simulated twin microquasar jets is calculated in a unified manner. From the cascade of emission within an element of jet matter to the dynamic and radiative whole jet model, the series of physical processes involved are integrated together. A programme suite assembled around model data produces synthetic images and spectra directly comparable to potential observations by contemporary arrays. The model is capable of describing a multitude of system geometries, incorporating increasing levels of realism depending on need and available computational resources. As an application, the modelling process is applied to a typical microquasar, which is synthetically observed from different angles using various imaging geometries. Furthermore, the resulting intensities are comparable to the sensitivity of existing detectors. The combined background emission from a potential distribution of microquasars is also modelled.
Highlights
Microquasars (MQ) comprise a binary stellar system where a main sequence star orbits a compact object, either a neutron star or a black hole [1]
Matter from the star accretes onto the collapsed stellar remnant, resulting in the production of twin relativistic jets pointing in opposite directions
Those jets emit over a broad spectrum, from radio to very high-energy (VHE) γ rays and neutrinos [2,3,4,5,6,7,8,9]
Summary
Microquasars (MQ) comprise a binary stellar system where a main sequence star orbits a compact object, either a neutron star or a black hole [1]. Matter from the star accretes onto the collapsed stellar remnant, resulting in the production of twin relativistic jets pointing in opposite directions Those jets emit over a broad spectrum, from radio to very high-energy (VHE) γ rays and neutrinos [2,3,4,5,6,7,8,9]. The solution of the transport equation from one particle distribution to the along a cascade, allows for the expression of the intensity of emitted neutrinos as a function of dynamic and radiative jet parameters at a given point This way, local model parameters at each space-time point in the model jet are directly connected to the final particle emission at the same point. Normalization and equipartition (and the synthetic imaging process) are described in Appendixes A and B respectively
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Free) 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
