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40 Aurigae

From Wikipedia, the free encyclopedia
Binary star in the constellation Auriga
40 Aurigae
Observation data
Epoch J2000      Equinox J2000
ConstellationAuriga
Right ascension06h 06m 35.09702s[1]
Declination+38° 28′ 57.5204″[1]
Apparent magnitude (V)5.345[2]
Characteristics
Spectral typeA4m[3]
U−Bcolor index+0.11[4]
B−Vcolor index+0.23[4]
Astrometry
Radial velocity (Rv)16.90 ± 7.4[5] km/s
Proper motion (μ)RA: 9.84[1]mas/yr
Dec.: −52.54[1]mas/yr
Parallax (π)9.57±0.34 mas[1]
Distance340 ± 10 ly
(104 ± 4 pc)
Orbit[3]
Primary40 Aur A
Companion40 Aur B
Period (P)28.28 d
Eccentricity (e)0.56
Periastronepoch (T)JD 2420468.197
Argument of periastron (ω)
(secondary)
178.4°
Semi-amplitude (K1)
(primary)
51.4 km/s
Semi-amplitude (K2)
(secondary)
62.5 km/s
Details[6]
Surface gravity (log g)3.88 ± 0.08 cgs
Temperature7838 ± 52 K
Metallicity [Fe/H]+0.35 ± 0.05 dex
Other designations
HD 41357,GCRV 3828,IRAS 06031+3829,SBC7 265,2MASS J06063509+3828578,AG+38° 663,GSC 02925-00806,PLX 1403,TD1 5967,BD+38° 1377,HIC 28946,PPM Star Catalogue 71223,TYC 2925-806-1,FK5 2465,HIP 28946,ROT 972,UBV 6148,GC 7723,HR 2143,SAO 58749,uvby98 100041357.
Database references
SIMBADdata

40 Aurigae is abinary star in theconstellationAuriga. Itsapparent magnitude is 5.345,[2] meaning it can just barely be seen with the naked eye. Based onparallax estimates made by theHipparcos spacecraft, the system is located some 340light-years (104parsecs) away.[1]

40 Aurigae is aspectroscopic binary, meaning the two stars are too close to be individuallyresolved, but periodicDoppler shifts in theirspectra indicate there must beorbital motion. In this case, light from both stars can be detected and it is a double-lined spectroscopic binary.[3] The two have anorbital period of 28.28 days and a fairly higheccentricity of 0.56.[3] The primary star is anA-type main-sequence star and shows unusual absorption lines in its spectrum, so it is anAm star[3] with aneffective temperature of 7,838K.[6]

References

[edit]
  1. ^abcdefvan Leeuwen, F.; et al. (2007)."Validation of the new Hipparcos reduction".Astronomy and Astrophysics.474 (2):653–664.arXiv:0708.1752.Bibcode:2007A&A...474..653V.doi:10.1051/0004-6361:20078357.S2CID 18759600.
  2. ^abHøg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars".Astronomy and Astrophysics.355:L27 –L30.Bibcode:2000A&A...355L..27H.
  3. ^abcdePourbaix, D.; et al. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits".Astronomy and Astrophysics.424 (2):727–732.arXiv:astro-ph/0406573.Bibcode:2004A&A...424..727P.doi:10.1051/0004-6361:20041213.S2CID 119387088.
  4. ^abMermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)".Catalogue of Eggen's UBV Data.Bibcode:1986EgUBV........0M.
  5. ^Kharchenko, N. V.; et al. (2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ~55000 stars and mean radial velocities of 516 Galactic open clusters and associations".Astronomische Nachrichten.328 (9): 889.arXiv:0705.0878.Bibcode:2007AN....328..889K.doi:10.1002/asna.200710776.S2CID 119323941.
  6. ^abKoleva, M.; Vazdekis, A. (2012). "Stellar population models in the UV. I. Characterisation of the New Generation Stellar Library".Astronomy & Astrophysics.538: A143.arXiv:1111.5449.Bibcode:2012A&A...538A.143K.doi:10.1051/0004-6361/201118065.S2CID 53999614.

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