LONG PERIOD ECLIPSING BINARIES

STAR SYSTEM PERIOD

epsilon Aurigae - 9885 days

KQ Puppis - 9572 days

VV Cephei - 7430.5 days

31 Cygni - 3784 days

EE Cephei -2049.53 days

32 Cygni - 1147.6 days

zeta Aurigae - 972.2 days

V777 Sagittarii - 936.07 days

22 Vulpeculae - 249.1 days

SUGGESTED LONG PERIOD
ECLIPSING BINARY STARS

Following is a list of some long-period eclipsing binary stars that are in need of observations. Some of these star systems make up a class known as the zeta Aurigae class of eclipsing binaries. These are all fairly bright and easy. They can be rather exciting when the star system goes into eclipse. They can all be seen easily from the northern hemisphere except V777 Sagittarii which is at -26 degrees declination.

Note:KQ Puppis is a binary system, but no eclipse has been seen. The period is estimated from spectroscopic measurements and the variability is an intrinsic variability.
The links are brief write-ups on each of these star systems. A summary of data follows these descriptions. These data summaries are the results of observations at the Hopkins Phoenix Observatory, research of papers, star atlases, and various star catalogues. Several years of effort went into compiling these summaries. If information is found to be incorrect or if data that are indicated as unknown become known, please contact the author and this information be be included in future editions.

SUMMARY OF LONG PERIOD ECLIPSING BINARY SYSTEMS

SYSTEM
EPOCH (JD)
PERIOD
NEXT ECLIPSE
TOTALITY
2,435,624 9,885 d (27.1 yr)
2009
670 days
?
 9572 d (26.21 yr)
?
?
2,435,931.4 7,430.5 d (20.34 yr)
2017
490 days
2,437,685.65 3,784 d (10.4 yr)
2014
61.2 days
2,433,225.1 1,147.6 d (3.15 yr)
May 2006
11 days
2,438,386.525 972.164 d (2.7 yr)
July 2006
37 days
2,429,411.7 936.07 d (2.6 yr)
Jan 2006
52 days
2,445,942.
249.1 d (.68 yr)
Oct 2005
10 days
2,434,346.0 2,049.53 d (5.6 yr)
Jan 2009
?
Page Created 6 October 1996
Modified 19 July 2006

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Jeff Hopkins (phxjeff@hposoft.com)

www.hposoft.com