Volume 493, Number 3, January III 2009
|Page(s)||829 - 833|
|Published online||04 December 2008|
Studying the properties of the radio emitter in LS 5039
Max Planck Institut für Kernphysik, Saupfercheckweg 1, Heidelberg 69117, Germany e-mail: firstname.lastname@example.org
Accepted: 4 November 2008
Context. LS 5039 is an X-ray binary that presents non-thermal radio emission. The radiation at ~5 GHz is quite steady and optically thin, consisting of a dominant core plus an extended jet-like structure. There is a spectral turnover around 1 GHz, and evidence of variability on timescales of 1 yr at 234 MHz.
Aims. We investigate the radio emitter properties using the available broadband radio data, and assuming two possible scenarios to explain the turnover: free-free absorption in the stellar wind, or synchrotron self-absorption.
Methods. We use the relationships between the turnover frequency, the stellar wind density, the emitter location, size and magnetic field, and the Lorentz factor of the emitting electrons, as well as a reasonable assumption regarding the energy budget, to infer the properties of the low-frequency radio emitter. Also, we put this information in context with the broadband radio data.
Results. The location and size of the low-frequency radio emitter can be restricted to few AU from the primary star, its magnetic field to ~3 10-3–1 G, and the electron Lorentz factors to ~. The observed variability of the extended structures seen with VLBA would point to electron bulk velocities 3 108 cm s-1, whereas much less variable radiation at 5 GHz would indicate velocities for the VLBA core 108 cm s-1. The emission at 234 MHz in the high state would mostly come from a region larger than the dominant broadband radio emitter.
Conclusions. We suggest a scenario in which secondary pairs, created via gamma-ray absorption and moving in the stellar wind, are behind the steady broadband radio core, whereas the resolved jet-like radio emission would come from a collimated, faster, outflow.
Key words: radio continuum: stars / X-rays: binaries / stars: individual: LS 5039 / radiation mechanisms: non-thermal
© ESO, 2009
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