40 Aurigae

In today's article we are going to delve into the fascinating world of 40 Aurigae. Whether you are an expert in the field or are seeking information for the first time, this article is designed to leave you with a deeper understanding of this topic. From its impact on society to its real-world applications, we will explore all the relevant aspects that make 40 Aurigae a topic of interest to people of all ages and backgrounds. Get ready to dive into a complete and detailed analysis that will leave you with a broader understanding of 40 Aurigae.

40 Aurigae
Observation data
Epoch J2000      Equinox J2000
Constellation Auriga
Right ascension 06h 06m 35.09702s[1]
Declination +38° 28′ 57.5204″[1]
Apparent magnitude (V) 5.345[2]
Characteristics
Spectral type A4m[3]
U−B color index +0.11[4]
B−V color 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
Periastron epoch (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 +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 a binary star in the constellation Auriga. Its apparent magnitude is 5.345,[2] meaning it can just barely be seen with the naked eye. Based on parallax estimates made by the Hipparcos spacecraft, the system is located some 340 light-years (104 parsecs) away.[1]

40 Aurigae is a spectroscopic binary, meaning the two stars are too close to be individually resolved, but periodic Doppler shifts in their spectra indicate there must be orbital motion. In this case, light from both stars can be detected and it is a double-lined spectroscopic binary.[3] The two have an orbital period of 28.28 days and a fairly high eccentricity of 0.56.[3] The primary star is an A-type main-sequence star and shows unusual absorption lines in its spectrum, so it is an Am star[3] with an effective temperature of 7,838 K.[6]

References

  1. ^ a b c d e f van 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. ^ a b Høg, 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. ^ a b c d e Pourbaix, 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. ^ a b Mermilliod, 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. ^ a b Koleva, 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.