The “prototype” Cepheid variable star, going up and down in brightness every 5.366 days in a very predictable way.
This light curve was created using all of the observations made by SPA VSS members during a single year.
Since the brightness changes repeat exactly from once cycle to the next, it is possible to combine all observations into a single light curve showing how the brightness changes during each 5.366 day cycle.
For each observation, the phase (i.e. fraction of the 5.366 day cycle completed) of Delta Cephei was calculated. This might seem a daunting task, but you can do this for your own observations via this helpful spreadsheet (which will also plot a light curve for you)
As can be seen from the resulting light curve, the rise to maximum is somewhat steeper than the fade back down to minimum. This is the case for the majority of Cepheids, There are exceptions to this pattern, however – one such exception is the star Zeta Gem (which also on the section’s programme) in which the light curve is more symmetrical.
| Extreme brightness range | 3.4-4.3 |
| More typical range | always the same range |
| Period of variation | 5.366 days |
| Frequency of observation | Worth checking on every clear night |
| Observe using | Naked eye – if you have a reasonably dark observing site. Otherwise use 40mm or 50mm binoculars. |
| Visibility | Can be observed all year round, but is fairly low in the evening sky from March to May |
Delta Cephei, like other Cepheid variables, is a yellow pulsating supergiant star whose outer layers pulsate in a very regular way.
Its brightness variations were first recognised in 1784 by the York-based amateur astronomer John Goodricke. Although it subsequently came to be regarded as the “prototype” Cepheid variable, it wasn’t the first Cepheid variable discovered – the brightness changes of Eta Aquilae had been discovered a few weeks earlier. However, Delta Cephei is better placed for observation from the UK and consequently it was Delta Cephei that was more closely studied.
The accompanying chart shows the location of Delta Cephei.
You can follow the brightness changes of Delta Cephei by comparing it with the lettered comparison stars.
Although Delta Cephei is generally described as being a naked eye variable star, the truth of that description depends on the amount of light pollution affecting your observing site.
If light pollution is a problem, then you may find it easier to observe Delta Cephei using 40mm (e.g 8×40) or 50mm (e.g. 7×50) binoculars.
At maximum, Delta Cephei will be almost as bright as comparison A.
At minimum, Delta Cephei will be slighty fainter than comparison E.
Mu Cephei is also a variable star. It varies in brightness much more slowly (and less predictably), typically varying over a range of about half a magnitude every two years.
Light Curves
I never intended to become a variable star observer. It was only by accident that I started to observe them. Soon, however, I was hooked!
Over the years, the number of variable stars that I followed steadily increased. The vast majority of the observations have been made using binoculars, with 11×80 binoculars taking over from the 10×50’s during 1992-93. I have also made observations with the naked eye but have never made a variable star observation using a telescope (I almost did once. Someone showed me the Perseus double cluster through a telescope and I came close to estimating the brightness of a variable star within it … but I resisted the temptation …).
In 1992, I was invited by John Isles to take over from him as the Variable Star Section Director and held the post for 8 years. Now I’m back again!
The early part of the year was relatively uneventful, with R Scuti emerging from the morning twilight by late January. 
The brightest nova for many years was discovered by the Japanese observer Koichi Itagaki on Aug 14th 2013. At discovery it was approx mag 6.8.
