Double periodic variable

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A double periodic variable is a type of binary star. As the name implies, the systems vary in brightness not only due to eclipses of one star by the other, but also on a cycle of roughly 33 times longer than the orbit. The star gaining mass from the other has a thick disk of material surrounding it, and the systems apparently lose mass cyclically into the interstellar medium over time. The cause for the secondary longer variability still is not established.[1] The stars are extremely rare, with less than fifteen candidates known as of July 2014.

List[edit]

The following list contains selected double periodic variables that are of interest to amateur or professional astronomy. Unless otherwise noted, the given magnitudes are in the V-band.

Star
Maximum
magnitude
Minimum
magnitude
Eclipse period
(in days)
Spectral
type
V393 Scorpii 7.39 8.31 7.72 B3III
AU Monocerotis 8.20 9.16 11.11 B5IV+F8-G0II-III

References[edit]

  1. ^ Otero, S. A.; Watson, C.; Wils, P. "Variable Star Type Designations in the VSX". AAVSO Website. American Association of Variable Star Observers. Retrieved 11 May 2014.