It was bright and visible visually at the discovery in 1977. However,
in its next appearance in 1992, it faded by about 3 mag, although the
perihelion distance reduced from 2.56 A.U. down to 2.36 A.U. The
brightness at the discovery seems to be caused by a temporary
The brightness is similar botn in 1992 and 2005. It is faint by CCD
observations. However, a few visual observers reported it much
brighter than CCD observations.
The nucleus was split into two components in 1992 appearance, although
the comet itself became fainter than before. Two components were also
observed in 2005 appearance.
Syuichi Nakano's calculation revealed that the component B in 2005 is
a return of the component B in 1992 (NK 1298B).
The component B in 2005 was as bright as in 1992. Therefore, the two
components will continue returning together also in the future.