Evidence of H
periodicities in LS I+61°303
R.K. Zamanov1,
J. Martí2,
J.M. Paredes3,
J. Fabregat4,
M. Ribó3,
and
A.E. Tarasov5
1
National Astronomical Observatory Rozhen,
P.O.Box 136, BG--4700 Smoljan, Bulgaria
2
Departamento de Física, Escuela Politécnica Superior,
Universidad de Jaén,
C/ Virgen de la Cabeza, 2, E--23071 Jaén, Spain
3
Departament d'Astronomia i Meteorologia,
Universitat de Barcelona, Av. Diagonal 647, E--08028 Barcelona, Spain
4
Departamento de Astronomía,
Universidad de Valencia, E--46100 Burjassot, Valencia, Spain
5
Crimean Astrophysical Observatory,
334413 Nauchny, Crimea, Ukraine
We present the results of analyzing
H spectra of the radio
emitting X-ray binary LS I+61°303. For the first time, the same
26.5 d radio period is clearly detected in the
H
emission line.
Moreover, the equivalent width and the peak separation of the
H
emission line seem also to vary over a time scale of 1600 days. This
points towards the  4 yr modulation,
detected in the radio outburst amplitude, being probably a result of
variations in the mass loss rate of the Be star and/or density
variability in the circumstellar disk. In addition, the dependence of
the peak separation from the equivalent width informs us that the
LS I+61°303 circumstellar disk is among the densest of
Be-stars.
1999, A&A, 351, 543
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