Iota Draconis (ι Draconis, abbreviated Iota Dra, ι Dra), also named Edasich /ˈɛdəsɪk/,[11][12] is a star in the northern circumpolar constellation of Draco. A visually unremarkable star of apparent magnitude 3.3,[2] in 2002 it was discovered to have a planet orbiting it[13] (designated Iota Draconis b, later named Hypatia). From parallax measurements, this star is located at a distance of about 101.2 light-years (31.0 parsecs) from the Sun.[1]
  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Draco |
| Right ascension | 15h 24m 55.77463s[1] |
| Declination | +58° 57′ 57.8344″[1] |
| Apparent magnitude (V) | 3.290[2] |
| Characteristics | |
| Evolutionary stage | Red giant branch[3] |
| Spectral type | K2III[4] |
| U−B color index | +1.230[2] |
| B−V color index | +1.160[2] |
| Variable type | Suspected[5] |
| Astrometry | |
| Radial velocity (Rv) | −10.71[6] km/s |
| Proper motion (μ) | RA: −8.36[1] mas/yr Dec.: +17.08[1] mas/yr |
| Parallax (π) | 32.23 ± 0.10 mas[1] |
| Distance | 101.2 ± 0.3 ly (31.03 ± 0.10 pc) |
| Absolute magnitude (MV) | 0.99±0.007[7] |
| Details | |
| Mass | 1.56±0.08[3] M☉ |
| Radius | 11.99±0.06[3] R☉ |
| Luminosity | 52.8±2.1[3] L☉ |
| Surface gravity (log g) | 2.52+0.007 −0.07[3] cgs |
| Temperature | 4,504±62[8] K |
| Metallicity [Fe/H] | +0.03±0.08[3] dex |
| Rotation | 434 days[5] |
| Rotational velocity (v sin i) | 1.5[5] km/s |
| Age | 2.49+0.64 −0.62[3] Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Nomenclature
editι Draconis (Latinised to Iota Draconis) is the star's Bayer designation. On discovery the planet was designated Iota Draconis b (or Edasich b).
It bore the traditional name Edasich, derived from the Arabic Al Ḍhiba' of Ulug Beg and the Dresden Globe, or Al dhīlī 'Male hyena' by Kazwini, with Eldsich being recorded in the Century Cyclopedia.[9] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[14] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[15] included a table of the first two batches of names approved by the WGSN; which included Edasich for this star.
In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars.[16] The process involved public nomination and voting for the new names.[17] In December 2015, the IAU announced the winning name was Hypatia for this planet.[18] The winning name was submitted by Hypatia, a student society of the Physics Faculty of the Universidad Complutense de Madrid, Spain. Hypatia was a famous Greek astronomer, mathematician, and philosopher.[19]
In Chinese, 紫微左垣 (Zǐ Wēi Zuǒ Yuán), meaning Left Wall of Purple Forbidden Enclosure, refers to an asterism consisting of Iota Draconis, Theta Draconis, Eta Draconis, Zeta Draconis, Upsilon Draconis, 73 Draconis, Gamma Draconis and 23 Cassiopeiae.[20] Consequently, the Chinese name for Iota Draconis itself is 紫微左垣一 (Zǐ Wēi Zuǒ Yuán yī, English: the First Star of Left Wall of Purple Forbidden Enclosure.),[21] representing 左樞 (Zuǒshū), meaning Left Pivot.[22] 左樞 (Zuǒshū) is westernized into Tsao Choo by R.H. Allen with the same meaning [23]
Properties
editIota Draconis is larger and more massive than the Sun, with 1.6 times the mass and nearly 12 times the radius.[3] The spectrum matches a stellar classification of K2 III,[4] indicating this is an evolved star that has exhausted the supply of hydrogen at its core and left the main sequence. It is currently on the red giant branch, fusing hydrogen in a shell around its helium core. With an expanded outer envelope, it is radiating over 50 times the luminosity of the Sun at an effective temperature of 4,504 K.[8] This temperature gives it an orange hue that is a characteristic of K-type stars.[24] It is rotating at a leisurely rate, with a period of around 434 days.[5] It is about 2.5 billion years old.[3]
In the past Iota Draconis has been suspected of variability. However, the star has been found to have a constant luminosity to within about 0.004 magnitudes. Hence, as of 2010, the variability remains unconfirmed.[5] An excess emission of infrared radiation at a wavelength of 70μm suggests the presence of a circumstellar disk of dust; what astronomers term a debris disk.[25]
Edasich is the faintest star of which a color has been reported in pre-telescopic times, and was classified as a orange-red star.[26]
Planetary system
edit| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b (Hypatia) | 11.67+0.45 −0.46 MJ |
1.448+0.028 −0.029 |
510.855±0.014 | 0.7008±0.0018 | 46+27 −19° |
— |
| c | 17.0+13 −5.4 MJ |
19.4+10 −7.7 |
68+60 −36 years |
0.455+0.12 −0.084 |
86+19 −19° |
— |
| Dust disk | ? AU | — | — | |||
The planetary companion discovered in 2002 was the first planet known to orbit a giant star.[13] The habitable zone for this star lies in the range of 6.8–13.5 Astronomical Units, placing this planet well inside.[8] The alignment of this planet's orbit may make it directly detectable via the transit method.[5] Another long-period planet or brown dwarf was discovered in 2021, and the true masses of both planets were measured via astrometry.[27]
References
edit- ^ a b c d e f van Leeuwen, F. (November 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
- ^ a b c d Jennens, P. A.; Helfer, H. L. (September 1975), "A new photometric metal abundance and luminosity calibration for field G and K giants", Monthly Notices of the Royal Astronomical Society, 172 (3): 667–679, Bibcode:1975MNRAS.172..667J, doi:10.1093/mnras/172.3.667
- ^ a b c d e f g h i Campante, Tiago L.; Li, Tanda; Ong, J. M. Joel; Corsaro, Enrico; Cunha, Margarida S.; Bedding, Timothy R.; Bossini, Diego; Breton, Sylvain N.; Buzasi, Derek L.; Chaplin, William J.; Deal, Morgan; García, Rafael A.; Hill, Michelle L.; Hon, Marc; Huber, Daniel; Jiang, Chen; Kane, Stephen R.; Kayhan, Cenk; Kuszlewicz, James S.; Lillo-Box, Jorge; Mathur, Savita; Monteiro, Mário J. P. F. G.; Pereira, Filipe; Santos, Nuno C.; Serenelli, Aldo; Stello, Dennis (2023), "Revisiting the Red Giant Branch Hosts KOI-3886 and ι Draconis. Detailed Asteroseismic Modeling and Consolidated Stellar Parameters", The Astronomical Journal, 165 (5): 214, arXiv:2304.01570, Bibcode:2023AJ....165..214C, doi:10.3847/1538-3881/acc9c1, S2CID 257921759
- ^ a b Morgan, W. W.; Keenan, P. C. (1973), "Spectral Classification", Annual Review of Astronomy and Astrophysics, 11: 29–50, Bibcode:1973ARA&A..11...29M, doi:10.1146/annurev.aa.11.090173.000333
- ^ a b c d e f Kane, Stephen R.; et al. (September 2010), "On the Transit Potential of the Planet Orbiting Iota Draconis", The Astrophysical Journal, 720 (2): 1644–1649, arXiv:1007.3501, Bibcode:2010ApJ...720.1644K, doi:10.1088/0004-637X/720/2/1644, S2CID 15944824
- ^ Famaey, B.; et al. (January 2005), "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters", Astronomy and Astrophysics, 430 (1): 165–186, arXiv:astro-ph/0409579, Bibcode:2005A&A...430..165F, doi:10.1051/0004-6361:20041272, S2CID 17804304
- ^ Park, Sunkyung; et al. (2013), "Wilson-Bappu Effect: Extended to Surface Gravity", The Astronomical Journal, 146 (4): 73, arXiv:1307.0592, Bibcode:2013AJ....146...73P, doi:10.1088/0004-6256/146/4/73, S2CID 119187733
- ^ a b c Baines, Ellyn K.; et al. (December 2011), "Fundamental Parameters of the Exoplanet Host K Giant Star ι Draconis from the CHARA Array", The Astrophysical Journal, 743 (2): 130, arXiv:1109.4950, Bibcode:2011ApJ...743..130B, doi:10.1088/0004-637X/743/2/130, S2CID 16119580
- ^ a b Allen, Richard Hinckley (1899), Star-names and Their Meanings, New York: G. E. Stechert, p. 210
- ^ "iot Dra -- Variable Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2012-01-11
- ^ Kunitzsch, Paul; Smart, Tim (2006), A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.), Cambridge, Massachusetts: Sky Pub, ISBN 978-1-931559-44-7
- ^ IAU Catalog of Star Names, retrieved 28 July 2016
- ^ a b Frink, Sabine; et al. (2002), "Discovery of a Substellar Companion to the K2 III Giant Iota Draconis", The Astrophysical Journal, 576 (1): 478–484, Bibcode:2002ApJ...576..478F, CiteSeerX 10.1.1.6.5332, doi:10.1086/341629, S2CID 12778096
- ^ IAU Working Group on Star Names (WGSN), retrieved 22 May 2016
- ^ Bulletin of the IAU Working Group on Star Names, No. 1 (PDF), retrieved 28 July 2016
- ^ NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars. IAU.org. 9 July 2014
- ^ NameExoWorlds The Process, archived from the original on 2015-08-15, retrieved 2015-09-05
- ^ Final Results of NameExoWorlds Public Vote Released, International Astronomical Union, 15 December 2015.
- ^ NameExoWorlds The Approved Names, archived from the original on 2018-02-01, retrieved 2016-01-02
- ^ (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) 香港太空館 - 研究資源 - 亮星中英對照表 Archived 2011-01-30 at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
- ^ (in Chinese) English-Chinese Glossary of Chinese Star Regions, Asterisms and Star Name Archived 2008-09-24 at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
- ^ Star Name - R.H. Allen p. 210
- ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on March 18, 2012, retrieved 2012-01-16
- ^ Kóspál, Ágnes; et al. (August 2009), "On the Relationship Between Debris Disks and Planets", The Astrophysical Journal Letters, 700 (2): L73–L77, arXiv:0907.0028, Bibcode:2009ApJ...700L..73K, doi:10.1088/0004-637X/700/2/L73, S2CID 16636256
- ^ Joyce, Meridith; Leung, Shing-Chi; Molnár, László; Ireland, Michael; Kobayashi, Chiaki; Nomoto, Ken'ichi (2020-10-01). "Standing on the Shoulders of Giants: New Mass and Distance Estimates for Betelgeuse through Combined Evolutionary, Asteroseismic, and Hydrodynamic Simulations with MESA". The Astrophysical Journal. 902 (1): 63. arXiv:2006.09837. Bibcode:2020ApJ...902...63J. doi:10.3847/1538-4357/abb8db. ISSN 0004-637X.
- ^ a b Hill, Michelle L.; Kane, Stephen R.; Campante, Tiago L.; Li, Zhexing; Dalba, Paul A.; Brandt, Timothy D.; White, Timothy R.; Pope, Benjamin J. S.; Stassun, Keivan G.; Fulton, Benjamin J.; Corsaro, Enrico; Li, Tanda; Joel Ong, J. M.; Bedding, Timothy R.; Bossini, Diego; Buzasi, Derek L.; Chaplin, William J.; Cunha, Margarida S.; Garcia, Rafael A.; Breton, Sylvain N.; Hon, Marc; Huber, Daniel; Jiang, Chen; Kayhan, Cenk; Kuszlewicz, James S.; Mathur, Savita; Serenelli, Aldo; Stello, Dennis (2021), "Asteroseismology of iota Draconis and Discovery of an Additional Long-period Companion", The Astronomical Journal, 162 (5): 211, arXiv:2107.13583, Bibcode:2021AJ....162..211H, doi:10.3847/1538-3881/ac1b31, S2CID 236493583