VY Cet: a contact binary in a ternary system [Observed: 26 Dec 2006, 3 Nov 2007, 30 Jan 2009, 31 Oct 2014]
Time series of this contact binary in a ternary system are presented.
3 ToMs are measured along with the B-V and V-Rc colors.
V1412 Aql: a simulation []
A Monte Carlo simulation which may be useful to search for eclipses
is proposed.
VZ Lib: a contact binary in a ternary system [Observed: 2007-2009, 14 sessions]
Time series of this eclipsing contact binary are reported and
times of minima (ToM) of the eclipses are measured. This system has a
third component. From the O-C analysis of the observed ToM and of those in
the literature, the orbital parameters of the third body can be
derived: the orbital period is 34.8 yr and the inclination is 11.5 °.
UX Mon: time keeping and modelling of a binary [Observed: 13 Dec 2007, 11-16, 18 Feb, 8, 13, 14 March, 1, 4, 25, 29]
Time series of this eclipsing binary system with extra variability
are presented. The O-C analysis suggests the presence of a third star.
The observations are modelled with BinaryMaker3 and parameters of the
system are derived.
WX Eri / V1241 Tau: an eclipsing semi-detached binary system [Observed: 15 Oct, 29, 30 Nov, 13, 16 Dec 2007, 1, 23 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.
ASAS1826+12: the eclipsing Cepheid [Observed: 7, 12, 13, 14, 15, 17, 19 July, 5, 18 Aug, 5, 6, 12, 15, 19,]
Multicolor photometric measurements of this Cepheid in an eclipsing
binary system (the only known one in our galaxy) are presented.
KZ Hya: a pulsating binary (improved) [Observed: 9 Feb, 11, 14 March, 19 Apr 2007]
This pulsating star is in a binary system with an 8-yr orbital
period. The times of maximum are compared with an improved ephemeris and
the parameters of the binary are derived.
KZ Hya: a pulsating binary [Observed: 23, 24 Dec 2005, 25 Jan, 13 Mar, 7 Apr 2006]
Time-series of this pulsating SXPHE star in a binary system are
presented and compared with other observations.
KZ Hya time keeping [Observations: 25, 27 April, 18, 19 May 2004]
Three pulses are observed for this SX Phe pulsating star. They
are 29 mn late from the 29 yr old GCVS ephemeris.