  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Auriga |
| Right ascension | 05h 32m 43.67437s [1] |
| Declination | +32° 11′ 31.2805″ [1] |
| Apparent magnitude (V) | 4.74 [2] |
| Characteristics | |
| Spectral type | B5 Iab [3] |
| U−B color index | –0.44 [2] |
| B−V color index | +0.32 [2] |
| Astrometry | |
| Radial velocity (Rv) | –0.2 [4] km/s |
| Proper motion (μ) |
RA: −0.812
mas/
yr
[1] Dec.: −3.15 mas/ yr [1] |
| Parallax (π) | 0.9087 ± 0.1906 mas [1] |
| Distance | 3910±420
ly (1,200±130 pc) [5] |
| Absolute magnitude (MV) | –6.4 [6] |
| Orbit [6] | |
| Period (P) | 676.85 ± 0.21 d |
| Eccentricity (e) | 0.116 ± 0.048 |
| Longitude of the node (Ω) | 181.7° ± 24.3° |
| Periastron epoch (T) | 2422754.2 ± 46.1 HJD |
|
Semi-amplitude (K1) (primary) | 22.0 ± 2.9 km/s |
| Details | |
| Mass | 21.1±0.2 [5] M☉ |
| Radius | 68±8 [5] R☉ |
| Luminosity | 190,500+49,300 −39,200 [5] L☉ |
| Surface gravity (log g) | 2.11±0.06 [5] cgs |
| Temperature | 14,600±300 [5] K |
| Rotational velocity (v sin i) | 40 [7] km/s |
| Age | 8.7 [5] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Chi Aurigae, Latinized from χ Aurigae, is the Bayer designation for a binary star system in the northern constellation of Auriga. It is visible to the naked eye with an apparent visual magnitude of 4.74. [2] The distance of Chi Aurigae is determined at 3,900 ly based on spectroscopic observations. [5] Parallax measurements by the Hipparcos spacecraft were unsuccessful because the parallax error was bigger than the value itself, [9] while the Gaia spacecraft measured the parallax with a 22% error, giving a distance of 3590±750 ly. [1] The brightness of the star is diminished by 1.26 in magnitude from extinction caused by intervening gas and dust. [6]
Chi Aurigae is a spectroscopic binary with an orbital period of 676.85 d and an eccentricity of 0.12. [10] The primary component of this system is a supergiant star with a stellar classification of B5 Iab. [3] It is over 190,000 times more luminous, around 20 times more massive and around 70 times larger. Its surface has an effective temperature of 14,600 K. [5] It has a stellar wind that is causing mass loss at the rate of 0.38–0.46 × 10−9 solar masses per year, or the equivalent of the Sun's mass every 2.4 billion years. [11]
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211. Bibcode: 2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d Crawford, D. L.; Barnes, J. V.; Golson, J. C. (1971), "Four-color, H-beta, and UBV photometry for bright B-type stars in the northern hemisphere", The Astronomical Journal, 76: 1058, Bibcode: 1971AJ.....76.1058C, doi: 10.1086/111220.
- ^ a b Lesh, Janet Rountree (December 1968), "The Kinematics of the Gould Belt: an Expanding Group?", Astrophysical Journal Supplement, 17: 371, Bibcode: 1968ApJS...17..371L, doi: 10.1086/190179.
- ^ Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Washington: Carnegie Institution of Washington, Bibcode: 1953GCRV..C......0W.
- ^ a b c d e f g h i Weßmayer, D.; Przybilla, N.; Butler, K. (2022-12-01), "Quantitative spectroscopy of B-type supergiants", Astronomy & Astrophysics, 668: A92, arXiv: 2208.02692, Bibcode: 2022A&A...668A..92W, doi: 10.1051/0004-6361/202243973, ISSN 0004-6361
- ^ a b c Raja, Tomas; Wolf, Marek (March 1998), "Hα variability of the B-type binary chi Aurigae", Astronomy and Astrophysics, 331: 550–556, Bibcode: 1998A&A...331..550R.
- ^ Abt, Helmut A.; Levato, Hugo; Grosso, Monica (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode: 2002ApJ...573..359A, doi: 10.1086/340590.
- ^ "* chi Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-23.
- ^ van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752v1, Bibcode: 2007A&A...474..653V, doi: 10.1051/0004-6361:20078357, S2CID 18759600. Note: see VizieR catalogue I/311.
- ^ 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.
- ^ Prinja, R. K.; Massa, D. L. (October 2010), "Signature of wide-spread clumping in B supergiant winds", Astronomy and Astrophysics, 521: L55, arXiv: 1007.2744, Bibcode: 2010A&A...521L..55P, doi: 10.1051/0004-6361/201015252, S2CID 59151633.
| Stars |
| ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| |||||||||||||
|
Star clusters |
| ||||||||||||
| Nebulae |
| ||||||||||||
| |||||||||||||
| |||||||||||||
| |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Auriga |
| Right ascension | 05h 32m 43.67437s [1] |
| Declination | +32° 11′ 31.2805″ [1] |
| Apparent magnitude (V) | 4.74 [2] |
| Characteristics | |
| Spectral type | B5 Iab [3] |
| U−B color index | –0.44 [2] |
| B−V color index | +0.32 [2] |
| Astrometry | |
| Radial velocity (Rv) | –0.2 [4] km/s |
| Proper motion (μ) |
RA: −0.812
mas/
yr
[1] Dec.: −3.15 mas/ yr [1] |
| Parallax (π) | 0.9087 ± 0.1906 mas [1] |
| Distance | 3910±420
ly (1,200±130 pc) [5] |
| Absolute magnitude (MV) | –6.4 [6] |
| Orbit [6] | |
| Period (P) | 676.85 ± 0.21 d |
| Eccentricity (e) | 0.116 ± 0.048 |
| Longitude of the node (Ω) | 181.7° ± 24.3° |
| Periastron epoch (T) | 2422754.2 ± 46.1 HJD |
|
Semi-amplitude (K1) (primary) | 22.0 ± 2.9 km/s |
| Details | |
| Mass | 21.1±0.2 [5] M☉ |
| Radius | 68±8 [5] R☉ |
| Luminosity | 190,500+49,300 −39,200 [5] L☉ |
| Surface gravity (log g) | 2.11±0.06 [5] cgs |
| Temperature | 14,600±300 [5] K |
| Rotational velocity (v sin i) | 40 [7] km/s |
| Age | 8.7 [5] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Chi Aurigae, Latinized from χ Aurigae, is the Bayer designation for a binary star system in the northern constellation of Auriga. It is visible to the naked eye with an apparent visual magnitude of 4.74. [2] The distance of Chi Aurigae is determined at 3,900 ly based on spectroscopic observations. [5] Parallax measurements by the Hipparcos spacecraft were unsuccessful because the parallax error was bigger than the value itself, [9] while the Gaia spacecraft measured the parallax with a 22% error, giving a distance of 3590±750 ly. [1] The brightness of the star is diminished by 1.26 in magnitude from extinction caused by intervening gas and dust. [6]
Chi Aurigae is a spectroscopic binary with an orbital period of 676.85 d and an eccentricity of 0.12. [10] The primary component of this system is a supergiant star with a stellar classification of B5 Iab. [3] It is over 190,000 times more luminous, around 20 times more massive and around 70 times larger. Its surface has an effective temperature of 14,600 K. [5] It has a stellar wind that is causing mass loss at the rate of 0.38–0.46 × 10−9 solar masses per year, or the equivalent of the Sun's mass every 2.4 billion years. [11]
- ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211. Bibcode: 2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d Crawford, D. L.; Barnes, J. V.; Golson, J. C. (1971), "Four-color, H-beta, and UBV photometry for bright B-type stars in the northern hemisphere", The Astronomical Journal, 76: 1058, Bibcode: 1971AJ.....76.1058C, doi: 10.1086/111220.
- ^ a b Lesh, Janet Rountree (December 1968), "The Kinematics of the Gould Belt: an Expanding Group?", Astrophysical Journal Supplement, 17: 371, Bibcode: 1968ApJS...17..371L, doi: 10.1086/190179.
- ^ Wilson, Ralph Elmer (1953), "General Catalogue of Stellar Radial Velocities", Carnegie Institute Washington D.C. Publication, Washington: Carnegie Institution of Washington, Bibcode: 1953GCRV..C......0W.
- ^ a b c d e f g h i Weßmayer, D.; Przybilla, N.; Butler, K. (2022-12-01), "Quantitative spectroscopy of B-type supergiants", Astronomy & Astrophysics, 668: A92, arXiv: 2208.02692, Bibcode: 2022A&A...668A..92W, doi: 10.1051/0004-6361/202243973, ISSN 0004-6361
- ^ a b c Raja, Tomas; Wolf, Marek (March 1998), "Hα variability of the B-type binary chi Aurigae", Astronomy and Astrophysics, 331: 550–556, Bibcode: 1998A&A...331..550R.
- ^ Abt, Helmut A.; Levato, Hugo; Grosso, Monica (July 2002), "Rotational Velocities of B Stars", The Astrophysical Journal, 573 (1): 359–365, Bibcode: 2002ApJ...573..359A, doi: 10.1086/340590.
- ^ "* chi Aur". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-08-23.
- ^ van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv: 0708.1752v1, Bibcode: 2007A&A...474..653V, doi: 10.1051/0004-6361:20078357, S2CID 18759600. Note: see VizieR catalogue I/311.
- ^ 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.
- ^ Prinja, R. K.; Massa, D. L. (October 2010), "Signature of wide-spread clumping in B supergiant winds", Astronomy and Astrophysics, 521: L55, arXiv: 1007.2744, Bibcode: 2010A&A...521L..55P, doi: 10.1051/0004-6361/201015252, S2CID 59151633.
| Stars |
| ||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| |||||||||||||
|
Star clusters |
| ||||||||||||
| Nebulae |
| ||||||||||||
| |||||||||||||
| |||||||||||||