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We extract the multiple-epoch Balmer-line profiles of the heavily obscuredquasar 3C 445 from the spectral curves in the literature, and analyze theemission-line profiles of the H$\alpha$ and H$\beta$ lines and the profilevariability in the H$\alpha$ line in the large time interval of more than threedecades. The profile comparison between the H$\alpha$ and H$\beta$ lines showsthat both Balmer lines share the profile with the same form, while the bluesystem of the H$\beta$ line is seriously weaker than that of the H$\alpha$line. Moreover, the blue system of the H$\alpha$ line suddenly disappearedcompletely and then did not appear again, however the other two components didnot exhibit significant variation in the velocity or the amplitude. Thesefindings suggest that the blue system of 3C 445, as with SDSSJ153636.22+044127.0 and its analogs, is probable the result of the shock-heatedoutflowing gases. The observation angle of almost edge-on which the previousstudies suggested can easily produce the high-speed and high-temperature shockin the collision between the massive outflow and the inner surface of the dustytorus.

Profile of and Variability in Double-Peaked Balmer Emission Lines in 3C 445