CK Aqr time keeping. Evidence for a ternary [Observed: 2005-20]
Photometric measurements of the contact binary system CK Aqr are
presented. 49 times of minimum were obtained between 2005 and 2020. Along
with already published observations, this allows the derivation of an
improved ephemeris. The resulting O-C diagram shows oscillations which
are interpreted as the light time travel effect due to a third component,
with a period of 8.2 years.
VZ Lib: a contact binary in a ternary system [Observed: 2014 (1 session, 1 ToM), 2016 (1 session, 1 ToM), 2018 (1]
New photometric observations are presented for this contact binary
in a ternary system. A total of 113 times of minimum are analyzed and
are found to be in agreement with the ephemeris of Liao et al (2019).
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.