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
evolvedsubgiant 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]
Name
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]
Observation
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]
^
abcdJohnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99,
Bibcode:
1966CoLPL...4...99J.
^
abKeenan, Philip C.; McNeil, Raymond C. (1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245,
Bibcode:
1989ApJS...71..245K,
doi:
10.1086/191373.
^
abTakeda, Genya; et al. (February 2007), "Structure and Evolution of Nearby Stars with Planets. II. Physical Properties of ~1000 Cool Stars from the SPOCS Catalog", The Astrophysical Journal Supplement Series, 168 (2): 297–318,
arXiv:astro-ph/0607235,
Bibcode:
2007ApJS..168..297T,
doi:
10.1086/509763,
S2CID18775378.
^Takeda, Yoichi; et al. (February 2005), "High-Dispersion Spectra Collection of Nearby F--K Stars at Okayama Astrophysical Observatory: A Basis for Spectroscopic Abundance Standards", Publications of the Astronomical Society of Japan, 57 (1): 13–25,
Bibcode:
2005PASJ...57...13T,
doi:10.1093/pasj/57.1.13.
^Lubin, Dan; Tytler, David; Kirkman, David (March 2012), "Frequency of Maunder Minimum Events in Solar-type Stars Inferred from Activity and Metallicity Observations", The Astrophysical Journal Letters, 747 (2): L32,
Bibcode:
2012ApJ...747L..32L,
doi:10.1088/2041-8205/747/2/L32.
^Kovacs, N.; Foy, R. (August 1978), "A detailed analysis of three stars in the Eggen's Epsilon INDI moving group", Astronomy and Astrophysics, 68 (1–2): 27–31,
Bibcode:
1978A&A....68...27K.