 It has been proposed that this short-term behavior is due to non-radial pulsations, fast rotational modulation, or the presence of a lower-mass companion.Theories that are now discounted include WR 46 being a Super soft X-ray source or a V Sagittae star,

The radial velocity changes of the spectral lines originating most deeply within the stellar wind show clear radial velocity variations with a period of 7.9 hours.However the lines do not change their shape or intensity, which would be expected from a pulsating star Non-radial pulsations have been proposed, with multiple pulsation periods of varying amplitude accounting for the apparently irregular brightness changes.