Microquasars
(MQ) comprise a binary stellar system where a main sequence star orbits a
compact object, either a neutron star or a black hole. 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 a 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. Synthetic pictures and spectra are produced using
a program suite built on model data, which are directly similar to possible
observations by modern arrays. Depending on the requirements and available
processing power, the model can incorporate progressively higher levels of
realism to describe a wide range of system geometries. The modeling procedure
is used on a typical microquasar, which is artificially observed using a
variety of imaging geometries and at different angles. 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. The emission model, which in our case was NEMISS, should be
altered in order to include the new emission physics. Synthetic imaging code RLOS2
is ready to use with any emission and absorption input, and only minor changes
are required.
Author(s) Details
Theodoros Smponias
Directorate
of Secondary Education of the Dodekanese, Zephyros, 85100 Rhodes, Greece.
Please see
the link:- https://doi.org/10.9734/bpi/strufp/v7/448
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