Abstract
Some short-period, detached binary systems have recently been reported to
experience very rapid orbital decay, much faster than is expected from the
angular-momentum loss caused by gravitational radiation alone. As these systems
contain fully convective stars, magnetic braking is not believed to be
operative, making the large orbital-period derivative puzzling. Here we explore
whether a resonant interaction between the binary and a surrounding
circumbinary (CB) disk could account for the observed orbital decay. Our
calculations indicate that the observed orbital-period derivatives in seven
detached binaries can be produced by the resonant interaction between the
binary and a CB disk if the latter has a mass in the range of $10^-4-10^-2~
M_ødot$, which is of the same order as the inferred disk mass
($\sim2.410^-4~ M_ødot$) in the post-common-envelope binary NN Ser.
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