Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Auriga |
Right ascension | 05h 38m 38.08510s [1] |
Declination | +30° 29′ 32.7054″ [1] |
Apparent magnitude (V) | 5.406 [2] (6.29 / 6.21) [3] |
Characteristics | |
Spectral type | G8III + A1IV or B9.5V [4] |
U−B color index | +0.25 [5] |
B−V color index | +0.45 [5] |
Variable type | suspected [6] |
Astrometry | |
Proper motion (μ) |
RA: -21.32
[1]
mas/
yr Dec.: -10.10 [1] mas/ yr |
Distance | 163 [4] pc |
Absolute magnitude (MV) | −0.29 [7] |
Orbit [4] | |
Primary | 26 Aur A |
Companion | 26 Aur B |
Period (P) | 52.735±0.156 yr |
Semi-major axis (a) | 0.154±0.001" (21.1+3.2 −2.4 AU) |
Eccentricity (e) | 0.653±0.002 |
Inclination (i) | 124.22±0.29° |
Longitude of the node (Ω) | 127.08±0.38° |
Periastron epoch (T) | 1974.927±0.026 |
Argument of periastron (ω) (secondary) | 309.07±0.14° |
Details | |
26 Aur A | |
Mass | 2.1 ± 1.0 [4] M☉ |
26 Aur B | |
Mass | 3.0 ± 0.4 [4] M☉ |
Other designations | |
Database references | |
SIMBAD | data |
26 Aurigae is a binary star [3] system in the northern constellation of Auriga. It is visible to the naked eye as a faint star with an apparent visual magnitude of 5.41. [2]
The distance to this system remains poorly constrained. The new
Hipparcos reduction gives a
parallax of 5.76±6.42.
[1] The original Hipparcos parallax was given as 7.29±0.96,
[8] leading to a distance of 137.2+20.8
−16.0
pc being assumed in many texts. A distance of 163 pc has been derived from fitting the spectrum.
[4]
26 Aurigae is a visual binary system, and the two stars orbit each other every 52.735 years with an ellipticity of 0.653 and an angular separation 0.154 ″. [4] The system is made of a magnitude 6.29 [3] G-type red giant, and a hotter magnitude 6.21 [3] star that has been classified as an early B-type main-sequence star to an A-type subgiant star. [4] Component A is the cool giant star, the brighter but less massive of the pair. [9] [4] The hotter star is sometimes listed as the primary on the basis of its stronger showing in the blended spectrum. [10]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Auriga |
Right ascension | 05h 38m 38.08510s [1] |
Declination | +30° 29′ 32.7054″ [1] |
Apparent magnitude (V) | 5.406 [2] (6.29 / 6.21) [3] |
Characteristics | |
Spectral type | G8III + A1IV or B9.5V [4] |
U−B color index | +0.25 [5] |
B−V color index | +0.45 [5] |
Variable type | suspected [6] |
Astrometry | |
Proper motion (μ) |
RA: -21.32
[1]
mas/
yr Dec.: -10.10 [1] mas/ yr |
Distance | 163 [4] pc |
Absolute magnitude (MV) | −0.29 [7] |
Orbit [4] | |
Primary | 26 Aur A |
Companion | 26 Aur B |
Period (P) | 52.735±0.156 yr |
Semi-major axis (a) | 0.154±0.001" (21.1+3.2 −2.4 AU) |
Eccentricity (e) | 0.653±0.002 |
Inclination (i) | 124.22±0.29° |
Longitude of the node (Ω) | 127.08±0.38° |
Periastron epoch (T) | 1974.927±0.026 |
Argument of periastron (ω) (secondary) | 309.07±0.14° |
Details | |
26 Aur A | |
Mass | 2.1 ± 1.0 [4] M☉ |
26 Aur B | |
Mass | 3.0 ± 0.4 [4] M☉ |
Other designations | |
Database references | |
SIMBAD | data |
26 Aurigae is a binary star [3] system in the northern constellation of Auriga. It is visible to the naked eye as a faint star with an apparent visual magnitude of 5.41. [2]
The distance to this system remains poorly constrained. The new
Hipparcos reduction gives a
parallax of 5.76±6.42.
[1] The original Hipparcos parallax was given as 7.29±0.96,
[8] leading to a distance of 137.2+20.8
−16.0
pc being assumed in many texts. A distance of 163 pc has been derived from fitting the spectrum.
[4]
26 Aurigae is a visual binary system, and the two stars orbit each other every 52.735 years with an ellipticity of 0.653 and an angular separation 0.154 ″. [4] The system is made of a magnitude 6.29 [3] G-type red giant, and a hotter magnitude 6.21 [3] star that has been classified as an early B-type main-sequence star to an A-type subgiant star. [4] Component A is the cool giant star, the brighter but less massive of the pair. [9] [4] The hotter star is sometimes listed as the primary on the basis of its stronger showing in the blended spectrum. [10]