The primary belongs to the rare class of subdwarf B stars, being former red giants with their hydrogen envelope completely stripped by a stellar companion.

[9] The binary nature of NY Virginis was first identified in 1998,[1] and the extremely short orbital period of 0.101016 d, together with brightness variability on the timescale of 200 seconds was noticed, resulting in the identification of the primary star as a B-type subdwarf in 2003.

This non-standard system indicates that it is a "normal" luminosity for a hot subdwarf and that the spectrum is dominated by hydrogen rather than helium.

[4] Studies in 2022 have noted that since planetary models generally fail to predict subsequent changes in eclipse timing,[13] and the most recent two-planet model as of 2021 results in orbits that are unstable on an astronomically-short timescale.

The same team also find that it is valid that there are exoplanets in the system creating the eclipe timing variations, and that the moderate eccentricites of the previous model likely caused the orbital instability.