Xi2 Ceti
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Cetus |
| Right ascension | 02h 28m 09.543s[1] |
| Declination | +08° 27′ 36.20″[1] |
| Apparent magnitude (V) | +4.279[2] |
| Characteristics | |
| Spectral type | A0III-[3] |
| B−V color index | -0.056[2] |
| Astrometry | |
| Proper motion (μ) | RA: 23.707±0.844[1] mas/yr Dec.: −4.787±0.778[1] mas/yr |
| Parallax (π) | 16.5681 ± 0.4608 mas[4] |
| Distance | 197 ± 5 ly (60 ± 2 pc) |
| Absolute magnitude (MV) | +0.639[5] |
| Details | |
| Mass | 2.45[6] M☉ |
| Radius | 2.6[5] R☉ |
| Luminosity | 74[5] L☉ |
| Surface gravity (log g) | 4.11[6] cgs |
| Temperature | 10630 ± 400[7] K |
| Rotational velocity (v sin i) | 55[6] km/s |
| Age | 127[6] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
Xi2 Ceti (ξ2 Ceti) is a star located in the constellation Cetus, approximately 60 parsecs from Earth.
Xi2 Ceti is a spectrophotometric standard star.[2] It has exhausted its core hydrogen, evolved away from the main sequence, and expanded to become a giant star, although still only 127 million years old.
In Chinese, 天囷 (Tiān Qūn), meaning Circular Celestial Granary, refers to an asterism consisting of α Ceti, κ1 Ceti, λ Ceti, μ Ceti, ξ1 Ceti, ξ2 Ceti, ν Ceti, γ Ceti, δ Ceti, 75 Ceti, 70 Ceti, 63 Ceti and 66 Ceti. Consequently, the Chinese name for Xi2 Ceti itself is "the Sixth Star of Circular Celestial Granary", Tiān Qūn Liù.[8]
References
- ^ a b c d van Leeuwen, F. (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.Vizier catalog entry
- ^ a b c Bessell, Michael S. (1999). "Spectrophotometry: Revised Standards and Techniques". Publications of the Astronomical Society of the Pacific. 111 (765): 1426–1433. Bibcode:1999PASP..111.1426B. doi:10.1086/316454.
- ^ Gray, R. O.; Garrison, R. F. (1987). "The Early A-Type Stars: Refined MK Classification, Confrontation with Stroemgren Photometry, and the Effects of Rotation". The Astrophysical Journal Supplement Series. 65: 581. Bibcode:1987ApJS...65..581G. doi:10.1086/191237.
- ^ 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 Jim Kaler (Dec 17, 2007). "Xi-2 Ceti".
- ^ a b c d 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.
- ^ Zorec, J.; et al. (2009). "Fundamental parameters of B supergiants from the BCD system. I. Calibration of the (λ_1, D) parameters into Teff". Astronomy and Astrophysics. 501 (1): 297–320. arXiv:0903.5134. Bibcode:2009A&A...501..297Z. doi:10.1051/0004-6361/200811147.
- ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日
External links
- http://server3.wikisky.org/starview?object_type=1&object_id=889
- http://www.alcyone.de/cgi-bin/search.pl?object=HR0718
