|Article in PDF||
vol. 6, N 25 (2006)
Received: 22.10.2006; accepted: 27.10.2006
(E-mail for contact: email@example.com)
|This variable star was discovered by Barsukova (2004) in the vicinity of the hard
source and microquasar candidate 1RXS J190333.1+104355 (Paredes et al., 2003). The
source is associated with an NVSS radio source. Our variable star is located outside
the error circles of these sources but very close to the western border of the ROSAT
error circle. It has a faint companion in 2" to the south-west, with the R_c magnitude
of 16.5. The
companion's contribution was removed from the combined light. The period determination
is based on
52 CCD R_c
observations taken with the 1-m telescope of the Special Astrophysical Observatory
(Russian Academy of Sciences) between JD 2452787
and 2454023. The light curve shape is typical of Mira Ceti type stars.
The V-R_c color near the light maxima is 3.0 mag. No evidence for a physical association
between this star and the X-ray and radio sources was found. |
|Barsukova, E.A., 2004, IBVS 5510
Paredes, J.M., Ribo, M., Marti, J., 2003, New Views of Microquasars. Ed. Ph. Durouchoux & J. Rodriguez, Centre for Space Physics, Kolkata, India, p.371
The light curve folded with the period of 308 days.
A colour CCD image reconstructed from the BVR frames taken on 2005 August 7. The error circles of the 1RXS X-ray source and NVSS radio source are shown. "c" is the comparison star, its BVR_cI_c magnitudes are respectively 18.01, 15.69, 14.08, 12.95.