Iota Orionis
 Location of ι Ori (circled) |
|
| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Orion |
| Right ascension | 05h 35m 25.98191s |
| Declination | –05° 54′ 35.6435″ |
| Apparent magnitude (V) | 2.77 |
| Characteristics | |
| Spectral type | O9 III + B0.8 III/IV |
| U−B color index | –1.08 |
| B−V color index | –0.24 |
| Variable type | (B) Orion |
| Astrometry | |
| Radial velocity (Rv) | 21.5 km/s |
| Proper motion (μ) |
RA: +1.42 mas/yr Dec.: –0.46 mas/yr |
| Parallax (π) | 1.40 ± 0.22mas |
| Distance | approx. 2,300 ly (approx. 700 pc) |
| Orbit | |
| Period (P) | 29.1338 days |
| Semi-major axis (a) | 132 R☉ |
| Eccentricity (e) | 0.764 |
| Inclination (i) | ~60° |
| Periastron epoch (T) | 2,450,072.80 HJD |
| Details | |
| ι Ori Aa | |
| Mass | 23.1 M☉ |
| Radius | 8.3 R☉ |
| Luminosity | 68,000 L☉ |
| Surface gravity (log g) | 3.73 cgs |
| Temperature | 32,500 K |
| Metallicity [Fe/H] | +0.10 dex |
| Rotational velocity (v sin i) | 122 km/s |
| Age | 4.0–5.5 Myr |
| ι Ori Ab | |
| Mass | 13.1 M☉ |
| Radius | 5.4 R☉ |
| Luminosity | 8,630 L☉ |
| Surface gravity (log g) | 3.78 cgs |
| Temperature | 27,000 K |
| Age | 9.4 ± 1.5 Myr |
| ι Ori B | |
| Surface gravity (log g) | 4.0 cgs |
| Temperature | 18,000 K |
| Age | ~3 Myr |
| Other designations | |
| A: ι Ori A, 2MASS J05352597-0554357 | |
| B: ι Ori B, V2451 Ori, 2MASS J05352645-0554445 | |
| C: ι Ori C, 2MASS J05352920-0554471 | |
| Database references | |
| SIMBAD | data |
Iota Orionis (ι Ori, ι Orionis) is a star in the equatorial constellation of Orion the hunter. The apparent visual magnitude of Iota Orionis is 2.77, making it the eighth-brightest member of Orion.
Iota Orionis is the brightest star in an asterism known as Orion's sword. It has the traditional names Hatsya or Hatysa and in Arabic, Na’ir al Saif, which means simply "the Bright One of the Sword." From parallax measurements, it is located at a distance of roughly 1,330 light-years (410 parsecs) from Earth.
Iota Orionis is a quadruple system dominated by a massive spectroscopic binary with an eccentric (e=0.764), 29-day orbit. The two components of ι Ori A are a stellar class O9 III star (blue giant) and a class B0.8 III/IV star about 2 magnitudes fainter. 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 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.
ι Ori has a B8 giant companion at 11" (approximately 5,000 AU) which has been shown to be variable, and likely to be a young stellar object. There is also a fainter A0 star at 49" catalogued as ι Ori C.
NGC 1980 is an open cluster containing a few bright stars including ι 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.
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