DOI

https://doi.org/10.48717/a218-vf26

Project

EM132

Title

EM132A

Abstract

LS I +61 303 is a gamma-ray binary composed of a Be star and a compact object orbiting it every 26.5 days. The nature of the compact object remains unknown and it can be either a black hole or a neutron star. Although it is thought that all gamma-ray binaries host a neutron star and the emission (observed from radio to TeV gamma-rays) is produced due to the interaction between the relativistic pulsar wind and the stellar wind, in the case of LS I +61 303 this scenario remains questioned. Several studies consider that a microquasar scenario, with the presence of a black hole with precessing jets, explains better the observed behavior of the source. But the same number of arguments point to the wind collision scenario. Here we propose to conduct two 8-h EVN+KVN observations at K band to resolve the innest part of the radio emitting region, which would allow us to clarify for the first time the origin of such emission and confront the proposed scenarios.