The rotation of the FE XIV solar corona during the recent solar activity minimum

We analyze data observed by the LASCO C1 coronagraph on board the SOHO spac ecraft during the solar minimum activity from April 1996 to March 1997. Usi ng the phase dispersion technique, we investigate the periodicity and recur rence of Fe XIV emission structures with heliospheric latitude and distance above the Sun's surface with high spatial resolution. We find no significa nt deviation from a rigidly rotating Fe XIV corona with latitude or with di stance from the Sun even on these small scales. In agreement with earlier w ork, the coronal rotation period at solar minimum is about 27.5 +/- 1 days.