Astronomy:Iota Hydrae
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Hydra |
| Right ascension | 09h 39m 51.36145s[1] |
| Declination | −01° 08′ 34.1135″[1] |
| Apparent magnitude (V) | 3.91[2] |
| Characteristics | |
| Spectral type | K2.5 III[2] |
| B−V color index | 1.32 |
| Variable type | Suspected[3] |
| Astrometry | |
| Radial velocity (Rv) | +24.19±0.36[4] km/s |
| Proper motion (μ) | RA: +46.96[1] mas/yr Dec.: −62.39[1] mas/yr |
| Parallax (π) | 12.39 ± 0.14[1] mas |
| Distance | 263 ± 3 ly (80.7 ± 0.9 pc) |
| Absolute magnitude (MV) | −0.63[5] |
| Details | |
| Mass | 1.92[2] M☉ |
| Radius | 33[4] R☉ |
| Luminosity | 83[2] L☉ |
| Surface gravity (log g) | 2.2[4] cgs |
| Temperature | 4,244±32[2] K |
| Metallicity [Fe/H] | −0.05[2] dex |
| Rotational velocity (v sin i) | 4.5[4] km/s |
| Age | 2.47[2] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Iota Hydrae (ι Hydrae, abbreviated Iota Hya, ι Hya), formally named Ukdah /ˈʌkdə/,[7] is a star in the constellation of Hydra, about 8° to the north-northwest of Alphard (Alpha Hydrae)[8] and just to the south of the celestial equator.[9] Visible to the naked eye, it is a suspected variable star with an apparent visual magnitude that ranges between 3.87 and 3.91.[3] Based upon an annual parallax shift of 12.39 mas measured during the Hipparcos mission,[1] it is located around 263 light-years from the Sun.
Nomenclature
ι Hydrae (Latinised to Iota Hydrae) is the star's Bayer designation.
This star along with Tau¹ Hydrae, Tau² Hydrae and 33 Hydrae (A Hydrae), were Ptolemy's Καμπή (Kampē); but Kazwini knew them as عقدة ʽuqdah (or ʽuḳdah) "knot".[10] According to a 1971 NASA memorandum,[11] Ukdah was the name of an asterism of four stars: Tau¹ Hydrae as Uḳdah I, Tau² Hydrae as Uḳdah II, 33 Hydrae as Uḳdah III and Iota Hydrae as Uḳdah IV. In 2016, the IAU organized a Working Group on Star Names (WGSN)[12] to catalog and standardize proper names for stars. The WGSN approved the name Ukdah for Iota Hydrae on 1 June 2018 and it is now so included in the List of IAU-approved Star Names.[7]
In Chinese, 星宿 (Xīng Sù), meaning Star or asterism, refers to an asterism consisting of ι Hydrae, Alphard, τ1 Hydrae, τ2 Hydrae, 26 Hydrae, 27 Hydrae, HD 82477 and HD 82428.[13] Consequently, ι Hydrae are known as 星宿四 (Xīng Sù sì, English: the Fourth Star of Star).[14]
Properties
This is an evolved K-type giant star with a stellar classification of K2.5 III.[2] It is a Barium star, which means that, for a giant star, it displays unusually strong absorption lines of singly-ionized barium and strontium.[15] Iota Hydrae has nearly twice[2] the mass of the Sun and has expanded to 33 times the Sun's radius.[4] It is around 2.5 billion years old and is spinning with a leisurely projected rotational velocity of 4.5[4] km/s. It may be a member of the Wolf 630 moving group of stars that share a common trajectory through space.[16]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 Luck, R. Earle (September 2015), "Abundances in the Local Region. I. G and K Giants", The Astronomical Journal 150 (3): 23, doi:10.1088/0004-6256/150/3/88, 88, Bibcode: 2015AJ....150...88L.
- ↑ 3.0 3.1 Samus, N. N. et al. (2009), "General Catalogue of Variable Stars", VizieR On-line Data Catalog 1, Bibcode: 2009yCat....102025S.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 Massarotti, Alessandro et al. (January 2008), "Rotational and radial velocities for a sample of 761 HIPPARCOS giants and the role of binarity", The Astronomical Journal 135 (1): 209–231, doi:10.1088/0004-6256/135/1/209, Bibcode: 2008AJ....135..209M.
- ↑ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ "iot Hya". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=iot+Hya.
- ↑ 7.0 7.1 "Naming Stars". IAU.org. https://www.iau.org/public/themes/naming_stars/.
- ↑ O'Meara, Steve (2007), Herschel 400 Observing Guide, Cambridge University Press, p. 84, ISBN 978-0521858939, https://books.google.com/books?id=Nyh9fAC_tpIC&pg=PA84.
- ↑ Moore, Patrick (2013), The Observer's Year: 366 Nights of the Universe, The Patrick Moore Practical Astronomy Series, Springer Science & Business Media, p. 71, ISBN 978-1447136132, https://books.google.com/books?id=p87TBwAAQBAJ&pg=PA71-IA11.
- ↑ Allen, R. H. (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York, NY: Dover Publications Inc. p. 250. ISBN 0-486-21079-0. https://archive.org/details/starnamestheirlo00alle/page/250. Retrieved 2010-12-12.
- ↑ Jack W. Rhoads - Technical Memorandum 33-507-A Reduced Star Catalog Containing 537 Named Stars, Jet Propulsion Laboratory, California Institute of Technology; November 15, 1971
- ↑ "IAU Working Group on Star Names (WGSN)". https://www.iau.org/science/scientific_bodies/working_groups/280/.
- ↑ (in Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN:978-986-7332-25-7.
- ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 29 日
- ↑ Lu, Phillip K. (June 1991), "Taxonomy of barium stars", Astronomical Journal 101: 2229–2254, doi:10.1086/115845, Bibcode: 1991AJ....101.2229L.
- ↑ McDonald, A. R. E.; Hearnshaw, J. B. (August 1983), "The Wolf 630 moving group of stars", Monthly Notices of the Royal Astronomical Society 204 (3): 841–852, doi:10.1093/mnras/204.3.841, Bibcode: 1983MNRAS.204..841M.
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