Here is some brief information about my current variable star programme, which was set up during 2008 July.
The programme includes stars drawn from the AAVSO and BAA VSS programmes. As a general rule I use AAVSO charts for telescopic objects owing to the fact that reverse chart formats are available which are more suitable for users of SCT telescopes. For binocular objects I have continued to use mainly BAA VSS charts.
The current programme includes some of the brighter and regularly 'performing' cataclysmic variables (CVs) on the AAVSO list as well as some less frequently outbursting objects on the BAA VSS's Recurrent Objects list. This list was set up by Gary Poyner to monitor less frequently outbursting objects. I also observe large numbers of long-period or 'Mira' variables and semi-regular variables on the BAA binocular programme. I currently log about 1500 observations per year. This total would be significantly greater if I didn't have to commute on a weekly basis.
Cataclysmic variables are eruptive stars and to a large extent consist of close binary systems involving a compact object such as a white dwarf and a main sequence star (see picture on the left (courtesy STAR Conference). The main sequence component acts as a donor star transferring matter to the white dwarf companion. In many cases, this results in the formation of an accretion disk around the white dwarf which for various reasons can undergo a sudden upsurge of brightness as the star goes into outburst. CVs are far from being a homogeneous bunch of objects however; my programme includes short amplitude periodically outbursting dwarf novae such as SS Cyg, U Gem and Z Cam along with 'classical novae' such as GK Per and HR Del where only one dramatic outburst has been recorded. Also included in my programme are a few examples of 'magnetic' CVs such as the polars / intermediate polars AM Her and DQ Her. Here a bright accretion disk does not normally form but instead matter spirals onto the white dwarf by flowing along the magnetic field lines.
There has definitely been an increasing focus on CVs over the past 20 years ago since I was last active as a variable star observer. This is at least partly due to the interest shown by professional researchers such as Dr Boris Gaensicke in the UK and Dr Paula Szkody in the US was has led to highly successful pro-am initiatives.
In addition to CVs, my programme also contains a significant number of LPVs or Miras named after the 'prototype' star Mira (o Cet). Although these stars are approximately periodic, they often display interesting deviations from 'normal' behaviour such as maxima and minima of varying depth, long term period change and 'halts' or slowdowns on the ascending or descending branches of the light curve. Furthermore many of these stars can be bright at maximum, leading to satuation of CCD images. They are therefore eminently suitable for visual observation. I subscribe entirely to the Mike Simonsen's view that a 'mixed diet' involving pulsating red giant stars such as LPVs and semi-regulars combined with CVs is a good way to organize an observing programme. 
The picture on the right below dipicts Mira (courtesy Nasa)
I also observe a number of the rare class of objects known as the R Coronae Borealis stars, named after the prototype R CrB which is currently (2009 Summer) undergoing one of its most prolonged minimum states since systematic observations began. These objects are usually at maximum brightness but show unpredictable fades caused it is thought by the accumulation of carbon particles along the line of site.
In the future it would be interesting to add eclipsing binaries and smaller amplitude variables to the above list, but this depends largely on building up photographic facilities for image analysis.
Details of all stars on my programme can be found here (pdf file)