Astrophotography by Anthony Ayiomamitis

Differential Photometry - Cepheus

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 eclipsing binary star NW Cep is a quick eclipsing binary variable star with a period of 2.7530064 days and which involves a delta mag of 0.90 (p) magnitudes during this brief time interval. The variable nature of NW Cep was discovered by Miller and Wachmann in 1973 and which happens to lie in the same field of view as the delta-Scuti variable star GSC 3986:1266. NW Cep is an Algol-type eclipsing system with spherical or slightly ellipsoidal components which are semi-detached and, hence, for its classification, namely "EA/SD". Further details from the International Variable Star Index are available here whereas an AAVSO finder chart is available here.

Note: The minimum observed below represents a primary minimum. No secondary minima are observable for NW Cep and which is possible for Algol-type variables.

Image Details
Light Curve for NW Cep
Imaging Details
Variable Star:
NW Cep

Other Designation:
N/A

RA / Dec:
22h 13m 48s /
+55° 44' 21"


Magnitude:
10.6 - 11.5 (p)

Period:
2.7530064 days

Variability:
EA/SD

Comparison Star:
GSC 3973:0467

Check Star:
GSC 3973:1365


Date:
Sep 03-04, 2012
21:00 - 02:00 UT+3


Location:
Athens, Greece

Equipment:
AP 305/f3.8 Riccardi-Honders
AP 1200GTO GEM
SBIG ST-10XME
SBIG CFW10
SBIG LRGB filters


Integrations:
Lum :  243 x 60 sec
Dark :  010 x 60 sec
Flat :  ~ 24,100 ADU
Binning :  1x1

Temperatures:
Ambient : + 22.0 ° C
CCD Chip : - 10.0 ° C

Software:
CCDSoft V5.00.201
AIP4Win V2.4.0


Processing:
Reduction
Differential Photometry