WX Eri / V1241 Tau: an eclipsing semi-detached binary system
Observed: 15 Oct, 29, 30 Nov, 13, 16 Dec 2007, 1, 23 Jan 2008
25 Jan 2008
Light curves of this eclipsing, semi-detached binary system
with a period of 0.8d are presented and are modeled with BinaryMaker3. No evidence
for a pulsating star in this system is found.
V1241 Tau (WX Eri in the previous edition of the GCVS) is
a binary system with an orbital period of 19.6h. One of the star
was suspected to be pulsating (a delta Scuti type star).
The observations were carried out with a 203mm SC telescope, a Clear
filter and a SBIG ST7E camera (KAF401E CCD).
1569 usable images were obtained, each with an exposure duration of 30s.
For the photometry, the comparison star is GSC4709-01022 with an assumed
unfiltered magnitude of 10.2. The check star is GSC4709-01298 with a measured
average magnitude of 11.500, an average 1-sigma statistical uncertainty
of 0.006mag and a standard deviation of 0.014mag.
An example of a light curve:
Red: V1241 Tau, Blue: the check star shifted by -0.8mag. The error bars
are +/- the 1-sigma statistical uncertainties.
According to the GCVS, the ephemeris t(E) = T0+P0*E for the primary eclipse is:
T0 = 2,427,531.687 HJD (4 Apr 1934)
P0= 0.823,270,38 d
But when I fold my observation with this ephemeris,
the primary eclipse is 23.8mn late. A new ephemeris is then:
T0 = 2,454,434.533 HJD (29 Nov 2007)
(or P0=0.823,270,88 d for the 32,678 cycles between the T0 of the GCVS
and my observations. Note that Srivastava & Kandpal (1986) reported
This gives the phase plot:
The phase coverage of my observing sessions:
Modeling with BinaryMaker3
I model my phase plot with the
I use the parameters of the binary system from Arentoft et al (2004).
All my parameters are HERE.
The results are:
The binary system at orbital phase 0.25. The red ellipses are the orbits,
the inclination being 86°.
Red crosses: the observations, Blue dots: the model.
V1241 Tau is suspected to hold a pulsating star. But the BinaryMaker3
model fits fairly well my observations, with no significant need for more
variability. The residuals between the observations and the BinaryMaker3
model are of 0.015mag on average, with a standard deviation of 0.019mag.
This confirms the non-detections of a pulsating component of Arentoft
et al (2004) (down to 8millimag) and of Pigulski & Michalska (2007).
Arentoft T., Lampens P., van Cauteren P., Duerbeck H.W., Garcia-Melendo
E., Sterken C. (2004) A&A 418 249.
Pigulski A., Michalska G. (2007) arXiv:astro-ph/0703614.
Srivastava J.B., Kandpal C.D. (1986) Ap & Sp Sc 121 301.
Telescope and camera configuration.
Computer and software configuration.
Modeling with BinaryMaker3.