English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

Recently, microquasar jets have aroused the interest of many researchersfocusing on the astrophysical plasma outflows and various jet ejections. Inthis work, we concentrate on the investigation of electromagnetic radiation andparticle emissions from the jets of stellar black hole binary systemscharacterized by the hadronic content in their jets. Such emissions arereliably described within the context of the relativisticmagneto-hydrodynamics. Our model calculations are based on the Fermiacceleration mechanism through which the primary particles (mainly protons) ofthe jet are accelerated. As a result, a small portion of thermal protons of thejet acquire relativistic energies, through shock-waves generated into the jetplasma. From the inelastic collisions of fast (non-thermal) protons with thethermal (cold) ones, secondary charged and neutral particles (pions, kaons,muons, $\eta$-particles, etc.) are created as well as electromagnetic radiationfrom the radio wavelength band, to X-rays and even to very high energygamma-rays. One of our main goals is, through the appropriate solution of thetransport equation and taking into account the various mechanisms that causeenergy losses to the particles, to study the secondary particle concentrationswithin hadronic astrophysical jets. After testing our method on the GalacticMQs SS 433 and Cyg X-1, as a concrete extragalactic binary system, we examinethe LMC X-1 located in the Large Magellanic Cloud, a satellite galaxy of ourMilky Way Galaxy. It is worth mentioning that, for the companion O star (andits extended nebula structure) of the LMC X-1 system, new observations usingspectroscopic data from VLT/UVES have been published few years ago.

Relativistic Magnetized Astrophysical Plasma Outflows in Black-Hole Microquasars