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 925 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 WASP-52b in Pegasus depicted below is one of the latest transiting exoplanets, having being announced only in Nov/2012 and represents the fifty-second discovery by the WASP (Wide Angle Search for Planets) team. WASP-52b is characterized with a mass 0.46 times that of Jupiter while its radius is equivalent to 1.27 Jupiter radii, thus making this exoplanet an inflated hot-Jupiter. WASP-52b requires 108.58 minutes to transit its parent star at a depth of 29.0 mmag or 2.90%. WASP-52b requires 1.7497798 days to its orbit star in a non-eccentric prograde orbit. The parent star, GSC 01161-01407, is a K2V star estimated to have a mass of 0.79 solar masses, a radius equivalent to 0.87 solar radii, a temperature of about 5,000° K and a visual magnitude of 12.0 while lying 457 light-years away. Further details regarding WASP-52 and WASP-52b are available in the paper published by the discovery team led by Guillaume Hebrard et al here.

Note: The C- and K-stars used for the purposes of the differential photometry measurements depicted below were GSC 1161:0574 (mag 10.67) and GSC 1161:0728 (mag 11.00) respectively.