GW Orionis is a T Tauri type pre-main sequence hierarchical triple star system.

GW Orionis first came to the attention of astronomers when it was published, as MHA 265–2, in a list of stars whose spectra have bright H and K lines of calcium.

Radial velocities of the primary star were measured from 45 high-resolution spectra and were used to determine the orbital elements.

A trend in the radial velocity residuals indicated either an additional stellar companion with an orbital period of years or a global asymmetric gravitational instability in a circumstellar disc.

[5] Observations of the disk made with the Atacama Large Millimeter Array identified three separate dust rings located at ~46, 188, and 338 astronomical units from the center of the system.