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Quickly localizing the identified white dwarf (WD) binaries is the basicrequirement for the space-based gravitational wave (GW) detection. In fact, theamplitude of GW signals are modulated by the periodic motion of GW detectors onthe solar orbit. The intensity of the observed signals is enhanced according tothe 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 longtime depends on filling gaps in the data. Actually, in a year period, the GWsources have a best observation orbit position of GW detectors, where thedetector response intensity of GW is maximum. Thus, the best positions, wherethe direction of GW source is perpendicular to the detection arms, can besearched for the verified GW sources of the sky map to enhance SNR too. For thethree arms response intensity of the GW signals changing more clearly with thelocation of the GW sources relative to the detector, the noises and thesuppression of noise by time delay interferometer are ignored. In the fourchosen sources, the two verification WD binaries: J0806 and V407 Vul areobserved at the best orbit positions by TAIJI for the short time of 2 and 3days respectively. The intensities of those GWs are above the values of theTAIJI sensitivity curve, significantly. Compared with a single detector, thenetwork of two detectors does not significantly improve the accuracy oflocation of the verification binaries. The reason of that result is that one GWsource can not be perpendicular to both detectors of TAIJI and LISA. Theseresults imply that the searching of GW signals and parameter estimation of GWsources from the experimental data of the space-based mission do not ignore theorbit positions relevant to GW sources.

Sky location of Galactic white dwarf binaries in space-based gravitational wave detection