The stars in non-evolved detached close binaries with small eccentricities usually rotate synchronously. However, the situation is usually different in the semi-detached systems because the rotational velocity of the gainer may be significantly higher than the synchronous one (Stothers 1973).
The observed values of the rotational velocities of the gainers are available only for eight systems of the ensemble analysed here. They are
summarized in Table 4 along with the references. This table also
contains the ratio of the real equatorial velocity to the synchronous one
/
. The synchronous value
was determined for the
parameters of the system given in Table 1. Only in case of
IZ Per the value of
/
was taken from the solution of the
light curve by
Wolf & West (1993). Since it is not clear how
in
V 448 Cyg listed by Volkova et al. (1993) was obtained this value should be
taken with caution.
Dependence of the degree of asynchronous rotation of the gainer on
for these binaries is plotted in Fig. 20. It can be
immediately seen that systems which periods can be considered constant
(AQ Cas, V 448 Cyg, IZ Per, V 356 Sgr) or where the change is uncertain
(RZ Sct) have gainers rotating significantly faster than the synchronous
value (often more than three times). The exception is u Her. The gainers in
two systems with variable periods, SX Aur and Z Vul, rotate rather close to
the synchronous value. Certainly, the number of the systems is too small to
confirm any clear relation of the rotational velocity of the gainer and
the observed period changes but it is useful to evaluate the role of rotation
of the gainer in the storage of angular momentum of the system (see below).
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Figure 20:
Dependence of the degree of asynchronous rotation of the
gainer on ![]() |
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