DO Cassiopeiae / DO Cas
Light curves and phase diagrams of the EB type eclipsing binary DO Cassiopeiae / DO Cas.
A minimum on 10 November 2012 was followed visually from Somerby using 10x50 binoculars and is shown below.
The following light curve and phase diagram were constructed from 36 images taken with the Cluster Camera of the Bradford Robotic Telescope, using their 'green' filter, between 2014 October 12 and 2016 October 1.
Two primary minima of EB type eclipsing binary DO Cas were obtained with the 2" Titan from Somerby Observatory in November 2013, on the 10th and the 12th.
The light curve is below. The gap in the Nov 10 run was due to cloud.
The light curve is below. The gap in the Nov 10 run was due to cloud.
DO Cas observed coming out of primary eclipse on 2019 February 18 with the 2" Titan at Somerby Observatory.
A primary minimum observed from Somerby Observatory with the 2" Titan on 2020 December 20.
The above observations were combined into a single light curve and phase diagram, below, where the BRT data is in black and the Somerby data is in red.
The above phase diagram in monochrome is below;
The following primary minimum was obtained on 2022 January 4 from Somerby Observatory with the 2" Titan.
The following secondary minimum was obtained on 2022 January 5 from Somerby Observatory with the 2" Titan.
The above two minima have been combined to form the following light curve and phase diagram.
2022 September update
A secondary minimum was observed coming out of minimum from Somerby Observatory, using the 2" Titan, on 2022 September 16. It appears in red in the following light curve and phase diagram.
2022 October update
Ingress into a primary minimum observed from Somerby Observatory, using the 2" Titan, on 2022 October 24. Observations were cut short by incoming cloud.
2024 January update
A secondary minimum was observed coming out of minimum from Somerby Observatory, using the 2" Titan, on 2024 January 9. It appears in red in the following light curves and phase diagram.
The catalogue period for this star is 0.6846661d (GCVS, AAVSO VSX, Kreiner) [Accessed 2024 January 13]. There is a sinusoidal variation evident in its o-c curve which has been attributed to a third body in the system (Kyu-Dong Oh, Chun-Hwey Kim, 1997).
[This page updated 2024 January 13]