Lambda Aurigae, Latinized from λ Aurigae, is the Bayer designation for a solar analog[9] star in the northern constellation of Auriga.[13] It is visible to the naked eye with an apparent visual magnitude of 4.71.[2] Based upon parallax measurements, it is approximately 40.7 light-years (12.5 parsecs) distant from the Earth.[14] The star is drifting further away with a high radial velocity of +66.5 km/s,[1] having come to within 24.4 ly (7.5 pc) some 117,300 years ago.[15] It has a high proper motion, traversing the celestial sphere at the rate of 0.844″ per year.[16]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Auriga |
Right ascension | 05h 19m 08.47546s[1] |
Declination | +40° 05′ 56.5896″[1] |
Apparent magnitude (V) | 4.71[2] |
Characteristics | |
Spectral type | G1 V[3] or G1.5 IV-V Fe-1[4] |
U−B color index | +0.13[2] |
B−V color index | +0.62[2] |
R−I color index | 0.32 |
Astrometry | |
Radial velocity (Rv) | +66.53±0.14[1] km/s |
Proper motion (μ) | RA: +520.581[1] mas/yr Dec.: −664.826[1] mas/yr |
Parallax (π) | 80.1054 ± 0.2158 mas[1] |
Distance | 40.7 ± 0.1 ly (12.48 ± 0.03 pc) |
Absolute magnitude (MV) | 4.20[5] |
Details | |
Mass | 1.081+0.054 −0.029[6] M☉ |
Radius | 1.331±0.021[3] R☉ |
Luminosity | 1.732±0.022[3] L☉ |
Surface gravity (log g) | 4.02[7] cgs |
Temperature | 5,890±4.3[8] K |
Metallicity [Fe/H] | +0.12[9] dex |
Rotational velocity (v sin i) | 2[10] km/s |
Age | 4,[9] 5.0–7.9[11] Gyr |
Other designations | |
Database references | |
SIMBAD | data |
ARICNS | data |
This is a G-type main sequence star with a stellar classification of G1 V.[3] It is sometimes listed with a class of G1.5 IV-V Fe-1,[4] which indicates the spectrum is showing some features of a more evolved subgiant star along with a noticeable underabundance of iron. In terms of composition it is similar to the Sun, while the mass and radius are slightly larger.[6] It is 73% more luminous than the Sun[3] and radiates this energy from its outer atmosphere at an effective temperature of 5890 K.[8] At this heat, the star glows with the yellow hue of a G-type star.[17] It has a low level of surface activity and is a candidate Maunder minimum analog.[18]
Lambda Aurigae has been examined for the presence of excess infrared emission that may indicate the presence of a circumstellar disk of dust, but no significant surplus has been observed.[9] It is a possible member of the Epsilon Indi Moving Group of stars that share a common motion through space. The space velocity components of this star are [U, V, W] = [+76, –39, –6] km/s.[19]
This star may have been called by the name Al Hurr, meaning the fawn in Arabic.[20] Lambda Aurigae, along with μ Aur and σ Aur, were Kazwini's Al Ḣibāʽ (ألحباع), the Tent.[20] According to the catalogue of stars in the Technical Memorandum 33-507 - A Reduced Star Catalog Containing 537 Named Stars, Al Ḣibāʽ were the title for three stars : λ Aur as Al Ḣibāʽ I, μ Aur as Al Ḣibāʽ II and σ Aur as Al Ḣibāʽ III.[21]
In Chinese, 咸池 (Xián Chí), meaning Pool of Harmony, refers to an asterism consisting of λ Aurigae, ρ Aurigae and HD 36041.[22] Consequently, the Chinese name for λ Aurigae itself is 咸池三 (Xián Chí sān, English: the Third Star of Pool of Harmony.)[23]
From Earth, Lambda Aurigae has an apparent magnitude of 4.71. The closest large neighboring star to Lambda Aurigae is Capella, located 4.5 light-years (1.4 parsecs) away.[24] Hypothetically viewed from Lambda Aurigae, Capella's quadruple star system would have an apparent magnitude of approximately -5.48,[25] about 40 times brighter than Sirius can be seen at maximum brightness from Earth.[26]
{{cite web}}
: CS1 maint: postscript (link)