  We have investigated the report of Tamura and Takeuti that the Halpha line of
the F-type post-AGB star HD56126 is variable on time scales of minutes. To this
end, HD56126 was observed on two occasions with the William Herschel Telescope.
Seventeen, respectively thirty spectra were taken within time span of 1.5 hours
in order to detect any short term variations. We find that the Halpha line
profile changed strongly over the two month interval, but no evidence is found
for short term variability. The variability Tamura and Takeuti claim to find is
probably due to the low signal-to-noise in their spectra.
