Neutrino emission from magnetized micro-quasar jets

TL;DR

This paper models neutrino emission from hadronic micro-quasar jets using relativistic hydrodynamics and semi-analytical methods, focusing on the SS-433 system, and introduces a power-law proton distribution for more realistic simulations.

Contribution

It develops a new simulation approach with a power-law proton distribution in relativistic jets, improving the modeling of neutrino emission in microquasar systems.

Findings

Neutrino energy spectrum can be extracted from the model jet.

The power-law proton distribution influences jet-wind interactions.

The method enables future dynamical simulations of microquasar jets.

Abstract

The hadronic jets in a micro-quasar stellar system are modelled with the relativistic hydrocode PLUTO. We focus on neutrino emission from such jets produced by fast proton (non-thermal) collisions on thermal ones within the hadronic jet. We adopt a semi-analytical approximation for the description of the secondary particles produced from p-p collisions and develop appropriate algorithms using the aforementioned injected protons as input. As a concrete example we consider the SS-433 X-ray binary system for which several observations have been performed the last decades. In contrast to the pre-set distribution of the fast protons along the jet employed in our previous works, in the present paper we simulated it by using a power-law fast proton distribution along the PLUTO hydro-code. This distribution gradually sweeps aside the surrounding winds, during the jet advance through the computational grid. As a first step, in the present work the neutrino energy spectrum is extracted from the model jet, facilitating a range of potential dynamical simulations in currently interesting microquasar jet systems.