Profile of and Variability in Double-Peaked Balmer Emission Lines in 3C
  445
  We extract the multiple-epoch Balmer-line profiles of the heavily obscured
quasar 3C 445 from the spectral curves in the literature, and analyze the
emission-line profiles of the H$\alpha$ and H$\beta$ lines and the profile
variability in the H$\alpha$ line in the large time interval of more than three
decades. The profile comparison between the H$\alpha$ and H$\beta$ lines shows
that both Balmer lines share the profile with the same form, while the blue
system 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 disappeared
completely and then did not appear again, however the other two components did
not exhibit significant variation in the velocity or the amplitude. These
findings suggest that the blue system of 3C 445, as with SDSS
J153636.22+044127.0 and its analogs, is probable the result of the shock-heated
outflowing gases. The observation angle of almost edge-on which the previous
studies suggested can easily produce the high-speed and high-temperature shock
in the collision between the massive outflow and the inner surface of the dusty
torus.
