LS I+61 303: microquasar or not microquasar?

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.

4 figs, 4 pages, contributing paper to the Conference "High Energy Processes in Relativistic Outflows", Dublin, September, 2007

References in corpus (7)

• Gamma-ray binaries: pulsars in disguise ?
• Modeling interaction of relativistic and nonrelativistic winds in binary system PSR 1259-63/SS2883. I.Hydrodynamical limit
• Accretion vs colliding wind models for the gamma-ray binary LS I +61 303: an assessment
• Joint H-alpha and X-Ray Observations of Massive X-Ray Binaries. II. The Be X-ray Binary and Microquasar LS I +61 303
• XMM-Newton observation of a spectral state transition in the peculiar radio/X-ray/gamma-ray source LS I +61 303
• Inverse Compton e-p pair cascade model for the gamma-ray production in massive binary LSI +61^o 303
• High-energy gamma-ray emission from the inner jet of LS I+61 303: the hadronic contribution revisited