It was discovered at 15 mag on January 30, 1952. Then it was observed
for one month until February 25. But it has not been observed since
that.
The brightness in 1952 yields the absolute magnitude of H10 = 12.0
mag.
It must have been observable at 14.5-15 mag in good condition before
the perihelion passages in 1958 and 1978, but not been observed. In
2004, it became in good condition after the perihelion passage like at
the discovery, when it must have reached to 14.5 mag. However, it was
not recovered even by automated surveys.
Therefore, the brightness in 1952 must have been due to a temporary
outburst. The usual brightness will be so faint as H10 = 18.0 mag or
fainter.
Kazuo Kinoshita's calculation reveals that it will pass close by
Jupiter in 2009, then the perihelion distance will decrease from 1.9
A.U. down to 1.2 A.U. As a result, it will be observable brighter than
before by 2 mag.
Another new outburst may occur due to coming closer to the sun.
However, the condition in 2011, when it comes closer to the sun for
the first time, will be too bad to observe.
The condition in 2017 is good, so it may be recovered by automated
surveys.
Profile
Appeared
Appeared before discovery
Not observed before discovery
