Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Orion |
Right ascension | 05h 24m 28.61672s [1] |
Declination | –02° 23′ 49.7311″ [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 color index | –0.90 [2] |
B−V color index | −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. 1,000
ly (approx. 300 pc) |
Orbit [6] | |
Primary | Aa |
Companion | Ab |
Period (P) | 7.989255±0.000005 days |
Eccentricity (e) | 0.011±0.0002 |
Inclination (i) | 85° |
Semi-amplitude (K1) (primary) | 145.5±0.03 km/s |
Semi-amplitude (K2) (secondary) | 150±3 km/s |
Orbit [3] | |
Companion | Ac |
Period (P) | 9.442±0.012 yr |
Semi-major axis (a) | 0.0441±0.0015″ |
Eccentricity (e) | 0.45±0.02 |
Inclination (i) | 102.8±1.8° |
Details | |
η Ori Aa | |
Mass | 11.0±0.5 [6] M☉ |
Radius | 6.3±0.6 [6] R☉ |
Temperature | 26,600 [6] K |
Rotational velocity (v sin i) | 20 [6] km/s |
η Ori Ab | |
Mass | 10.6±0.7 [6] M☉ |
Radius | 5.2±0.4 [6] R☉ |
Temperature | 26,600 [6] K |
Rotational velocity (v sin i) | 130 [6] km/s |
η Ori Ac | |
Mass | 6.78 [7] M☉ |
η Ori B | |
Mass | 8.7 [7] M☉ |
Other designations | |
Database references | |
SIMBAD | data |
Eta Orionis or Algjebbah, Latinized from η 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.
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. [9] The two are estimated to orbit every 1,800 years. [7]
The primary star, Eta Orionis A, is itself a spectroscopic triple star, known from multiple spectral lines with varying radial velocities. [6] 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. [6]
The system lies within the Orion OB1 association, a group of massive stars that includes most of the bright stars of Orion. [10] It is assigned to the oldest and closest part of the association, known as OB1a. [11]
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. [13]
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. [6] 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. [13]