ι Orionis is the system's Bayer designation. The designations of the three constituents as Iota Orionis A, B and C, and those of A's components - Iota Orionis Aa and Ab - derive from the convention used by the Washington Multiplicity Catalog for multiple star systems, and adopted by the International Astronomical Union. The system has the traditional name Nair al Saif, from the Arabic nayyir as-sayf "the Bright One of the Sword", though this is little used. Since Bečvář's 1951 Atlas Coeli, it has borne the proper nameHatysa. Kunitzsch was unable to find an older source for the latter name. In 2016, the IAU organized a Working Group on Star Names to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems. It approved the name Hatysa for the component Iota Orionis Aa on 5 September 2017 and it is now so included in the List of IAU-approved Star Names. Iota Orionis B is a variable star and in 2011 it was given the variable star designation V2451 Orionis.
Distance
Iota Orionis has a parallax of in the Hipparcos new reduction, indicating a distance around. The previous published Hipparcos parallax was, suggesting a closer distance. Gaia Data Release 2 has individual parallaxes for the two fainter components of the Iota Orionis star system of and, indicating distances of and respectively, with margins of error of just a few parsecs. There is little doubt that all three stars are at the same distance. Iota Orionis is generally assumed to be associated with the open cluster NGC 1980, which is at a distance of around. However, they may not lie at exactly the same distance and Iota Orionis may have a complex history involving stellar encounters and runaway stars. NGC 1980 contains few bright stars other than Iota Orionis. Only eighteen other stars are considered members in a survey down to 14th magnitude, most of them around 9th magnitude but including the 5th magnitude stars HR 1886 and 1887.
Properties
Iota Orionis is dominated by Iota Orionis A whose two components are a stellar class O9 III star and a class B0.8 III/IV star about 2 magnitudes fainter. The combined spectral type has long been accepted as O9 III and it was listed as a standard star for that type. The collision of the stellar winds from this pair makes the system a strong X-ray source. Oddly, the two objects of this system appear to have different ages, with the secondary being about double the age of the primary. In combination with the high eccentricity of their 29-day orbit, this suggests that the binary system was created through a capture, rather than by being formed together and undergoing a mass transfer. This capture may have occurred, for example, through an encounter between two binary systems, with one star being donated from each binary and two runaway stars being ejected. The primary component of Iota Orionis A is a class O giant star with a mass of about. It has a surface temperature of and radius of, resulting in a bolometric luminosity of. It is calculated to be around nine million years old. The secondary star of the spectroscopic binary pair is a class B giant or subgiant with a mass of about. It has a temperature of and radius of, resulting in it radiating over 8,000 times as much energy as the sun. Iota Orionis B is a B8 giant at 11" which has been shown to be variable, and likely to be a young stellar object. It is also a helium-weakchemically peculiar star. The fainter Iota Orionis C is an A0 star at 49".
