[4] The variable nature of this star was discovered at the Moscow Observatory by Lidiya Tseraskaya (L. Ceraski) in 1908.

[11] Observation since 1926 showed that this variable undergoes two different types of eruptions: a short maxima lasting around two days that ranged in brightness between 11.6–12.9 magnitude, and a longer maxima extending for 13 days that ranged between 10.4–11.8 magnitude.

[12] Similar dwarf novae of this class have since been discovered, and SU UMa is now the prototype for this sub-category of variable stars.

[6] It consists of a white dwarf star that is acquiring matter from its close companion via an accretion disk.

[15] X-ray emission has been detected in the vicinity of the white dwarf, which drops by a factor of four during outbursts.