Quickly localizing the identified white dwarf (WD) binaries is the basic
requirement for the space-based gravitational wave (GW) detection. In fact, the
amplitude of GW signals are modulated by the periodic motion of GW detectors on
the solar orbit. The intensity of the observed signals is enhanced according to
the observation time beyond a year to enhance a high signal to noise ratio
(SNR). As data gap exists, the completeness of the data observed for a long
time depends on filling gaps in the data. Actually, in a year period, the GW
sources have a best observation orbit position of GW detectors, where the
detector response intensity of GW is maximum. Thus, the best positions, where
the direction of GW source is perpendicular to the detection arms, can be
searched for the verified GW sources of the sky map to enhance SNR too. For the
three arms response intensity of the GW signals changing more clearly with the
location of the GW sources relative to the detector, the noises and the
suppression of noise by time delay interferometer are ignored. In the four
chosen sources, the two verification WD binaries: J0806 and V407 Vul are
observed at the best orbit positions by TAIJI for the short time of 2 and 3
days respectively. The intensities of those GWs are above the values of the
TAIJI sensitivity curve, significantly. Compared with a single detector, the
network of two detectors does not significantly improve the accuracy of
location of the verification binaries. The reason of that result is that one GW
source can not be perpendicular to both detectors of TAIJI and LISA. These
results imply that the searching of GW signals and parameter estimation of GW
sources from the experimental data of the space-based mission do not ignore the
orbit positions relevant to GW sources.Comment: 22 pages, 15 figure