Chi Tauri, Latinised from χ Tauri, is a star system in the constellation of Taurus. Parallax measurements made by the Hipparcos spacecraft put it at a distance of about 291 light-years (89 parsecs) from Earth. The primary component has an apparent magnitude of about 5.4,[2] meaning it is visible with the naked eye.
  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Taurus |
| χ Tau A | |
| Right ascension | 04h 22m 34.944s[1] |
| Declination | +25° 37′ 45.53″[1] |
| Apparent magnitude (V) | 5.378[2] |
| χ Tau B | |
| Right ascension | 04h 22m 35.550s[3] |
| Declination | +25° 38′ 03.22″[3] |
| Apparent magnitude (V) | 8.423[4] |
| Characteristics | |
| χ Tau A | |
| Spectral type | B9V[4] |
| U−B color index | -0.12[5] |
| B−V color index | -0.04[5] |
| χ Tau B | |
| Spectral type | F8 + G6 + K4 + K4[4] |
| U−B color index | +0.10[5] |
| B−V color index | +0.63[5] |
| Astrometry | |
| χ Tau A | |
| Radial velocity (Rv) | +15.3 ± 3.4[4] km/s |
| Proper motion (μ) | RA: 20.953[1] mas/yr Dec.: -16.495[1] mas/yr |
| Parallax (π) | 11.0472 ± 0.1599 mas[1] |
| Distance | 295 ± 4 ly (91 ± 1 pc) |
| Absolute magnitude (MV) | 0.82 ± 0.18[4] |
| χ Tau B | |
| Radial velocity (Rv) | +14.694 ± 0.081[4] km/s |
| Proper motion (μ) | RA: 15.766[3] mas/yr Dec.: −20.396[3] mas/yr |
| Parallax (π) | 11.5348 ± 0.0857 mas[3] |
| Distance | 283 ± 2 ly (86.7 ± 0.6 pc) |
| Absolute magnitude (MV) | 3.85 ± 0.18 (total) 4.20 ± 0.18 (Ba) 5.27 ± 0.18 (Bb) 7.87 / 7.87 (Bc)[4] |
| Orbit[4] | |
| Primary | χ Tau Ba |
| Companion | χ Tau Bb |
| Period (P) | 17.602309 ± 0.000036 d |
| Eccentricity (e) | 0.2938 ± 0.0013 |
| Inclination (i) | 53.3 ± 0.5° |
| Periastron epoch (T) | 2,448,891.649 ± 0.014 |
| Argument of periastron (ω) (secondary) | 249.43 ± 0.33° |
| Semi-amplitude (K1) (primary) | 41.287 ± 0.080 km/s |
| Semi-amplitude (K2) (secondary) | 48.133 ± 0.080 km/s |
| Orbit[4] | |
| Primary | χ Tau Bab |
| Companion | χ Tau Bc |
| Period (P) | 3,450.6 ± 6.1 d |
| Eccentricity (e) | 0.3560 ± 0.0068 |
| Inclination (i) | 73 ± 6° |
| Periastron epoch (T) | 2,447,546.5 ± 9.7 |
| Argument of periastron (ω) (secondary) | 250.3 ± 1.5° |
| Semi-amplitude (K1) (primary) | 8.625 ± 0.067 km/s |
| Details | |
| Age | 200 ± 50[4] Myr |
| χ Tau A | |
| Mass | 2.60 ± 0.05[4] M☉ |
| Radius | 2.15[6] R☉ |
| Surface gravity (log g) | 4.15 ± 0.14[7] cgs |
| Temperature | 10,300 ± 300[4] K |
| Rotational velocity (v sin i) | 263[7] km/s |
| χ Tau Ba | |
| Mass | 1.19[4] M☉ |
| Surface gravity (log g) | 4.5[4] cgs |
| Temperature | 6,180 ± 150[4] K |
| Rotational velocity (v sin i) | 1 ± 3[4] km/s |
| χ Tau Bb | |
| Mass | 1.02[4] M☉ |
| Surface gravity (log g) | 4.5[4] cgs |
| Temperature | 5,620 ± 150[4] K |
| Rotational velocity (v sin i) | 1 ± 3[4] km/s |
| χ Tau Bc | |
| Mass | ~0.70 / 0.70[4] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | χ Tau A |
| χ Tau B | |
The main component of the system is Chi Tauri A. It is a B-type main-sequence star. Its mass is 2.6 times that of the Sun and its surface glows with an effective temperature of 10,300 K. It may be a binary star itself, as suggested from astrometric data from Hipparcos, although no orbit could be derived.[4]
The secondary component of the system is Chi Tauri B, separated about 19″[4] from Chi Tauri A. It was thought to be a post-T Tauri star from its unusual spectrum,[8] but later studies ruled this out.[4] It is a double-lined spectroscopic binary—the two stars are not resolved but their spectra have periodic Doppler shifts indicating orbital motion. The two stars are an F-type star and a G-type star, respectively, and are designated Ba and Bb.[4]
The radial velocity of Chi Tauri B has a slow drift indicating the presence of another star in the system. Designated Chi Tauri Bc, this massive object is too dim to be detected, but it appears in Chi Tauri B's spectrum as an infrared excess. Because of this infrared excess, this unseen component is thought to be a pair of K-type main-sequence stars both with masses 70% of the Sun's. The stars within the system appear to be dynamically interacting.[4]
Naming
edit- With φ, κ1, κ2 and υ, it composed the Arabic were the Arabs' Al Kalbain, the Two Dogs.[9] According to the catalogue of stars in the Technical Memorandum 33-507 - A Reduced Star Catalog Containing 537 Named Stars, Al Kalbain were the title for five stars: φ as Alkalbain I, this star (χ) as Alkalbain II, κ1 as Alkalbain III, κ2 as Alkalbain IV and υ as Alkalbain V.[10][clarification needed]
- In Chinese, 礪石 (Lì Dàn), meaning Whetstone, refers to an asterism consisting of χ Tauri, ψ Tauri, 44 Tauri and φ Tauri. Consequently, the Chinese name for χ Tauri itself is 礪石三 (Lì Dàn sān, English: the Third Star of Whetstone).[11]
References
edit- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ 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.
- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b c d e f g h i j k l m n o p q r s t u v w x y z Torres, Guillermo (2006). "The Multiple System HD 27638". The Astronomical Journal. 131 (3): 1702–1711. arXiv:astro-ph/0512254. Bibcode:2006AJ....131.1702T. doi:10.1086/500355. S2CID 119106287.
- ^ a b c d Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
- ^ Pasinetti Fracassini, L. E.; et al. (2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics". Astronomy & Astrophysics. 367 (2): 521–24. arXiv:astro-ph/0012289. Bibcode:2001A&A...367..521P. doi:10.1051/0004-6361:20000451. S2CID 425754.
- ^ a b David, Trevor J.; Hillenbrand, Lynne A. (2015). "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets". The Astrophysical Journal. 804 (2): 146. arXiv:1501.03154. Bibcode:2015ApJ...804..146D. doi:10.1088/0004-637X/804/2/146. S2CID 33401607.
- ^ Lindroos, K. P. (1986). "A study of visual double stars with early-type primaries. V - Post-T Tauri secondaries". Astronomy and Astrophysics. 156 (1–2): 223–233. Bibcode:1986A&A...156..223L.
- ^ Allen, Richard Hinckley (1899). Star-Names and Their Meanings. New York: G. E. Stechert. p. 413.
- ^ Rhoads, Jack W. (November 15, 1971). "Technical Memorandum 33-507-A Reduced Star Catalog Containing 537 Named Stars" (PDF). Jet Propulsion Laboratory, California Institute of Technology.
{{cite journal}}: Cite journal requires|journal=(help) - ^ "天文教育資訊網" [AEEA (Activities of Exhibition and Education in Astronomy)] (in Chinese). 2006-05-22. Archived from the original on 2011-09-28. Retrieved 2019-06-20.