2009ApJ...702.1179M

LS I +61°303 is a γ-ray binary with periodic radio outbursts coincident with the orbital period of P = 26.5 days. The origin of the radio emission is unclear, it could be due either to a jet, as in microquasars, or to the shock boundary between the Be star and a possible pulsar wind. We here analyze the radio spectral index over 6.7 years from Green Bank Interferometer data at 2.2 GHz and 8.3 GHz. We find two new characteristics in the radio emission. The first characteristic is that the periodic outbursts indeed consist of two consecutive outbursts; the first outburst is optically thick, whereas the second outburst is optically thin. The spectrum of LS I +61°303 is well reproduced by the shock-in-jet model commonly used in the context of microquasars and active galactic nuclei: the optically thin spectrum is due to shocks caused by relativistic plasma ("transient jet") traveling through a preexisting much slower steady flow ("steady jet"). This steady flow is responsible for the preceding optically thick spectrum. The second characteristic we find is that the observed spectral evolution, from optically thick to optically thin emission, occurs twice during the orbital period. We observed this occurrence at the orbital phase of the main 26.5 d outburst and also at an earlier phase, shifted by ΔΦ∼ 0.3 (i.e., almost 8 d before). We show that this result qualitatively and quantitatively agrees with the two-peak accretion/ejection model proposed in the past for LS I +61°303. We conclude that the radio emission in LS I +61°303 originates from a jet and suggest that the variable TeV emission comes from the usual Compton losses expected as an important by-product in the shock-in-jet theory.