Eta Orionis
Template:Location mark Location of η Orionis (circled) | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Orion |
| Right ascension | Template:RA[1] |
| Declination | Template:DEC[1] |
| Apparent magnitude (V) | 3.42[2] (4.50 + 5.90 + 5.65 + 4.95)[3] |
| Characteristics | |
| Spectral type | Aa: B1 V Ab: B3 V Ac: B3 V B: B2 V[3] |
| U−B Template:Engvar | −0.90[2] |
| B−V Template:Engvar | −0.17[2] |
| Variable type | Algol[4] |
| Astrometry | |
| Radial velocity (Rv) | +19.8[5] km/s |
| Proper motion (μ) | RA: −0.71[1] mas/yr Dec.: −3.46[1] mas/yr |
| Parallax (π) | 3.34±1.07 mas[1] |
| Distance | approx. Template:Rnd ly (approx. Template:Rnd pc) |
| Orbit | |
| Primary | Aa |
| Companion | Ab |
| Period (P) | Script error: No such module "val".[6] days |
| Eccentricity (e) | Script error: No such module "val".[6] |
| Inclination (i) | Script error: No such module "val".[6]° |
| Argument of periastron (ω) (primary) | Script error: No such module "val".[6]° |
| Semi-amplitude (K1) (primary) | Script error: No such module "val".[7] km/s |
| Semi-amplitude (K2) (secondary) | Script error: No such module "val".[7] km/s |
| Orbit[3] | |
| Companion | Ac |
| Period (P) | Script error: No such module "val". yr |
| Semi-major axis (a) | Script error: No such module "val".″ |
| Eccentricity (e) | Script error: No such module "val". |
| Inclination (i) | Script error: No such module "val".° |
| Details | |
| η Ori Aa | |
| Mass | Script error: No such module "val".[6] Template:Solar mass |
| Radius | Script error: No such module "val".[6] Template:Solar radius |
| Surface gravity (log g) | Script error: No such module "val".[6] cgs |
| Temperature | 26,600[7] K |
| Rotational velocity (v sin i) | 20[7] km/s |
| η Ori Ab | |
| Mass | Script error: No such module "val".[6] Template:Solar mass |
| Radius | Script error: No such module "val".[6] Template:Solar radius |
| Surface gravity (log g) | Script error: No such module "val".[6] cgs |
| Temperature | 25,950[6] K |
| Metallicity [Fe/H] | {{{metal_fe2}}} dex |
| Rotational velocity (v sin i) | 130[7] km/s |
| η Ori Ac | |
| Mass | 6.78[8] Template:Solar mass |
| η Ori B | |
| Mass | 8.7[8] Template:Solar mass |
| Metallicity [Fe/H] | {{{metal_fe2}}} dex |
| Other designations | |
| Template:Odlist[9] | |
| Database references | |
| SIMBAD | data |
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Eta Orionis is a multiple star in the constellation Orion. It lies a little to the west of Orion's Belt between Delta Orionis and Rigel, being closer to Delta Orionis than to Rigel. It lies at a distance of around 1,000 light-years from Earth and is part of the Orion OB1 association.
Nomenclature
Eta Orionis, Latinized from η Orionis, is the star's Bayer designation. It has the traditional Arabic name Saif al Jabbar, the Sword of the Giant, but this name is now used for another star, Saiph (Kappa Orionis).[10] It has also sometimes been called by the Latin name Ensis,[10] and Algjebbah.[11]
System
Eta Orionis is listed in multiple star catalogues as having two companions: a bright component B less than 2″ away; and a faint component C nearly 2′ away.[12] The two are estimated to orbit every 1,800 years.[8]
The primary star, Eta Orionis A, is itself a spectroscopic triple star, known from multiple spectral lines with varying radial velocities.[7] The most distant component Ac, has been resolved using speckle interferometry, at a separation of about 0.04″. It orbits the other two in 9.4 years.[3] The two closest stars, Aa and Ab, are separated by only about a tenth of an astronomical unit and orbit in just under eight days.[7]
The system lies within the Orion OB1 association, a group of massive stars that includes most of the bright stars of Orion.[13] It is assigned to the oldest and closest part of the association, known as OB1a.[14]
Variability
Eta Orionis drops in brightness every four days from a combined apparent magnitude of 3.31 to about magnitude 3.6. This is due to eclipses between the two closest components, Aa and Ab.[4] The primary and secondary eclipses are very similar, 0.24 and 0.23 magnitudes deep, respectively.[16]
It has also been suggested that component Ab is intrinsically variable with a period of 0.3 days and a very small amplitude. This star has unusual variable spectral lines and lies with the β Cephei variable instability strip.[7] However, it is now thought that the variable component is either B and Ac, possibly due to an unseen companion or rotational modulation. The actual period is 0.432 days and the 0.3-day period was an alias.[16]
See also
References
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