The nova was reported by Taichi Kato of Kyoto University in the International Astronomical Union circular 7552, issued on December 30, 2000.

[6] Examination of the optical spectrum of this nova showed absorption lines of calcium (Ca I), sodium (Na I) and singly ionized iron (Fe II).

[6][7] The infrared spectrum measured on January 31 showed a featureless continuum that decreased with increasing wavelength.

This is theorized to occur when a white dwarf star predominantly accretes helium (rather than hydrogen) from an orbiting companion.

When sufficient helium has accumulated along a shell on the surface of the white dwarf, a run-away thermonuclear explosion results in a nova outburst.