[2] The distance to this system is approximately 1,150 light years from the Sun, based on parallax measurements.

[9] It was given its variable star designation, CR Boötis, in 1987,[11] in literature up until that time it was called PG 1346+082.

Rapid flickering suggests this is a close binary system undergoing mass transfer, while emission by neutral helium indicates there is a thick accretion disk orbiting a compact object.

The lack of hydrogen in the spectrum demonstrates that the donor star is a helium white dwarf with a lower mass than the primary.

The first is a lower state of quiescence that displays regular superoutbursts similar to ER Ursae Majoris on a roughly 46 day cycle.