A variable star, as its name suggests, is a star whose magnitude varies intrinsically, in contrast to eclipsing binaries whose magnitude varies as a result of one star in the binary system eclipsing the other. True variables are one of five types, namely Mira stars, semiregular stars, cepheids, eruptive variables and, finally, cataclysmic variables. Minimum to maximum magnitude can range from days to many months with some variables displaying irregular periods.

A popular method for the study of variable stars, particularly short-term variables, is by the use of the technique known as "differential photometry". Rather than measure the (variable) magnitude of a variable star on an absolute scale, measurements are made over time relative to one or more non-variable star(s) and these differences are then plotted so as to study and illustrate the relative or differential change in magnitude. Due to the very large number of variables stars, the field of differential photometry represents one of the key fields in astronomy whereby the amateur astronomer can make a meaningful and long-lasting contribution to both science and astronomy.

More recently, the search for extrasolar planets (over 750 discovered so far) has identified yet another interesting application for the practice of differential photometry whereby the minute drops in magnitude of a star hosting an exoplanet are studied. Further details for the interested party are available here.

Note: The light curve for exoplanet HAT-P-32b in Andromeda depicted below is one of the latest transiting exoplanets, having being announced in June/2011, and represents the thirty-second discovery by the Hungarian-based HATNet Project team. HAT-P-32b is characterized with a mass 0.816 times that of Jupiter while its radius is equivalent to 1.79 Jupiter radii, thus making this exoplanet one of the most inflated "hot Jupiter" finds to date. HAT-P-32b requires 186.5 minutes to transit its parent star at a depth of 20.3 millimag or 2.03%. It has an eccentric orbit with a period of 2.150008 days with possible tidal effects at play. The parent star, GSC 3281:0800, is a late F- or early G-type dwarf estimated to have a mass of 1.160 solar masses, a radius equivalent to 1.219 solar radii, a temperature of 6,207° K and to lie at a distance of 923 light-years away with a visual magnitude of 11.289.

Further details regarding HAT-P-32 and HAT-P-32b are available in the paper published by the discovery team led by Hartman et al here.

Note: The C- and K-stars used for the purposes of the differential photometry measurements depicted below were GSC 3280:0995 (mag 11.20) and GSC 3281:0221 (mag 11.20) respectively.