LS I+61 303: microquasar or not microquasar?

TL;DR

This paper investigates whether LS I+61 303 is a microquasar or a different type of binary system, using observational data and 3D simulations to clarify its nature.

Contribution

The study provides new 3D SPH simulation results supporting the microquasar interpretation of LS I+61 303, challenging previous claims of a Be/neutron star binary.

Findings

Simulation results favor an accretion-powered microquasar model.

Supports the microquasar interpretation over the colliding wind binary hypothesis.

Provides insights into the system's high-energy emission variability.

Abstract

LS I +61 303 is a puzzling object detected from radio up to high-energy gamma-rays. Variability has recently been observed in its high-energy emission. The object is a binary system, with a compact object and a Be star as primary. The nature of the secondary and the origin of the gamma-ray emission are not clearly established at present. Recent VLBA radio data have been used to claim that the system is a Be/neutron star colliding wind binary, instead of a microquasar. We review the main views on the nature of LS I +61 303 and present results of 3D SPH simulations that can shed some light on the nature of the system. Our results support an accretion powered source, compatible with a microquasar interpretation.