Volume 515, June 2010
|Number of page(s)||6|
|Published online||11 June 2010|
Feasibility study of Lense-Thirring precession in LS I +61°303
Max Planck Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany e-mail: [mmassi;lzimmerm]@mpifr-bonn.mpg.de
Accepted: 18 March 2010
Context. Very recent analysis of the radio spectral index and high energy observations have shown that the two-peak accretion/ejection microquasar model applies for LS I +61°303.
Aims. The fast variations of the position angle observed with MERLIN and confirmed by consecutive VLBA images must therefore be explained in the context of the microquasar scenario.
Methods. We calculate what could be the precessional period for the accretion disk in LS I +61°303 under tidal forces of the Be star (Ptidal-forces) or under the effect of frame dragging produced by the rotation of the compact object (PLense-Thirring).
Results. Ptidal-forces is more than one year. PLense-Thirring depends on the truncated radius of the accretion disk, Rtr. We determined Rtr = 300 rg for observed QPO at 2 Hz. This value is much above the few rg, where the Bardeen-Petterson effect should align the midplane of the disk. For this truncated radius of the accretion disk PLense-Thirring for a slow rotator results in a few days.
Conclusions. Lense-Thirring precession induced by a slowly rotating compact object could be compatible with the daily variations of the ejecta angle observed in LS I +61°303.
Key words: black hole physics / radio continuum: stars / pulsars: general / X-rays: binaries / X-rays: indiviual (LS I +61°303)
© ESO, 2010
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