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Updated on December 10, 2022


* Profile

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 outburst.

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.

* Returns and Appearances

!Discovered *Appeared -Not observed #Appeared before discovery +Not observed before discovery .Returns in the future
2034 Jan. 10
* 101P
2020 Jan. 12
* 101P
2005 Dec. 25
* 101P/1991 L1
1992 Jan. 25
! 101P/1977 Q1
1978 Feb. 14


The perihelion dates in the past appearances are printed on Catalog of Cometary Orbits 1996.
Information on the discovery and historical highlights are available at General Comet Info (Gary W. Kronk).
The past and future orbital elements calculated by Kazuo Kinoshita (http://www9.ocn.ne.jp/~comet/pcmtn/0101p.htm).


Copyright(C) Seiichi Yoshida (comet@aerith.net). All rights reserved.