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 510 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-18b in Hercules depicted below is one of the
latest transiting exoplanet discoveries, having being announced late July/2010, and represents the eighteenth discovery
by the Hungarian-based HATNet Project team. HAT-P-18b is characterized with a low mass of only 0.197 times that of
Jupiter and in spite of a larger radius (0.995 RJup), thus making this find a low-density Saturn-mass
exoplanet with a negligible core mass. HAT-P-18b requires 163 minutes to transit its parent star at a depth of 18.3
mmag (1.83%).
The parent star, GSC 2594:646, is a K2 dwarf estimated to have a mass of 0.77 solar masses, a radius equivalent to
0.75 solar radii, a temperature of 4,803° K and to lie at a distance of 541 light-years away with a visual magnitude
of 12.759. Further details regarding HAT-P-18 and HAT-P-18b 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 2595:392 (mag 11.7) and GSC 2594:102 (mag 12.5) respectively.
Parent Star: HAT-P-18 GSC/SAO Catalog: GSC 2594:646 Constellation: Hercules RA / Dec: 17h 05m 23s / +33° 00' 47" Magnitude: 12.759 Distance: 541 light-years Exoplanet: HAT-P-18b Period: 5.508023 + 0.000006 d Transit Duration: 163 mins Transit Depth: 18.3 mmag Minimum Mass: 0.197 MJup Radius: 0.995 RJup Pred Transit Details:
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Date: May 13-14, 2011 23:30:00 - 04:14:40 UT+3 Location: Athens, Greece Equipment: AP 305/f3.8 Riccardi-Honders AG AP 1200GTO GEM SBIG ST-10XME SBIG CFW10 SBIG LRGB filters Integrations:
Temperatures:
Software: CCDSoft V5.00.201 AIP4Win V2.2 Processing: Reduction Differential Photometry |