Astronomy:Iota Draconis

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Short description: Star in the constellation Draco
Iota Draconis / Edasich
Draco constellation map.svg
Red circle.svg
Location of ι Draconis (circled)
Observation data
Equinox J2000.0]] (ICRS)
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[1] mas
Distance101.2 ± 0.3 ly
(31.03 ± 0.10 pc)
Absolute magnitude (MV)0.99±0.007[7]
Details
Mass1.56±0.08[3] M☉
Radius11.99±0.06[3] R☉
Luminosity52.8±2.1[3] L☉
Surface gravity (log g)2.52+0.007−0.07[3] cgs
Temperature4,504±62[8] K
Metallicity [Fe/H]+0.03±0.08[3] dex
Rotation434 days[5]
Rotational velocity (v sin i)1.5[5] km/s
Age2.49+0.64−0.62[3] Gyr
Other designations
Edasich, Eldsich,[9] 12 Draconis, BD+59 1654, FK5 425, FK5 571, HD 137759, HIP 75458, HR 5744, SAO 29520, 2MASS J15245578+5857577[10]
Database references
SIMBADdata

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]

Nomenclature

ι 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

Iota 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]

Planetary system

The Iota Draconis planetary system[26]
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.[26]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (November 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. ↑ 2.0 2.1 2.2 2.3 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, doi:10.1093/mnras/172.3.667, Bibcode: 1975MNRAS.172..667J 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 3.8 Campante, Tiago L.; Li, Tanda; Ong, J. M. Joel; Corsaro, Enrico; Cunha, Margarida S.; Bedding, Timothy R.; Bossini, Diego; Breton, Sylvain N. et al. (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, doi:10.3847/1538-3881/acc9c1, Bibcode: 2023AJ....165..214C 
  4. ↑ 4.0 4.1 Morgan, W. W.; Keenan, P. C. (1973), "Spectral Classification", Annual Review of Astronomy and Astrophysics 11: 29–50, doi:10.1146/annurev.aa.11.090173.000333, Bibcode: 1973ARA&A..11...29M 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Kane, Stephen R. et al. (September 2010), "On the Transit Potential of the Planet Orbiting Iota Draconis", The Astrophysical Journal 720 (2): 1644–1649, doi:10.1088/0004-637X/720/2/1644, Bibcode: 2010ApJ...720.1644K 
  6. ↑ 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, doi:10.1051/0004-6361:20041272, Bibcode: 2005A&A...430..165F 
  7. ↑ Park, Sunkyung et al. (2013), "Wilson-Bappu Effect: Extended to Surface Gravity", The Astronomical Journal 146 (4): 73, doi:10.1088/0004-6256/146/4/73, Bibcode: 2013AJ....146...73P 
  8. ↑ 8.0 8.1 8.2 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, doi:10.1088/0004-637X/743/2/130, Bibcode: 2011ApJ...743..130B 
  9. ↑ 9.0 9.1 Allen, Richard Hinckley (1899), Star-names and Their Meanings, New York: G. E. Stechert, p. 210, https://books.google.com/books?id=5xQuAAAAIAAJ&pg=PA210 
  10. ↑ "iot Dra -- Variable Star", SIMBAD (Centre de Données astronomiques de Strasbourg), http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Iota+Draconis, retrieved 2012-01-11 
  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 
  12. ↑ IAU Catalog of Star Names, http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt, retrieved 28 July 2016 
  13. ↑ 13.0 13.1 Frink, Sabine et al. (2002), "Discovery of a Substellar Companion to the K2 III Giant Iota Draconis", The Astrophysical Journal 576 (1): 478–484, doi:10.1086/341629, Bibcode: 2002ApJ...576..478F 
  14. ↑ IAU Working Group on Star Names (WGSN), https://www.iau.org/science/scientific_bodies/working_groups/280/, retrieved 22 May 2016 
  15. ↑ Bulletin of the IAU Working Group on Star Names, No. 1, http://www.pas.rochester.edu/~emamajek/WGSN/WGSN_bulletin1.pdf, retrieved 28 July 2016 
  16. ↑ NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars. IAU.org. 9 July 2014
  17. ↑ NameExoWorlds The Process, http://nameexoworlds.iau.org/process, retrieved 2015-09-05 
  18. ↑ Final Results of NameExoWorlds Public Vote Released, International Astronomical Union, 15 December 2015.
  19. ↑ NameExoWorlds The Approved Names, http://nameexoworlds.iau.org/names, retrieved 2016-01-02 
  20. ↑ (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.
  21. ↑ (in Chinese) 香港太空館 - 研究資源 - 亮星中英對照表 , Hong Kong Space Museum. Accessed on line November 23, 2010.
  22. ↑ (in Chinese) English-Chinese Glossary of Chinese Star Regions, Asterisms and Star Name , Hong Kong Space Museum. Accessed on line November 23, 2010.
  23. ↑ Star Name - R.H. Allen p. 210
  24. ↑ "The Colour of Stars", Australia Telescope, Outreach and Education (Commonwealth Scientific and Industrial Research Organisation), December 21, 2004, http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html, retrieved 2012-01-16 
  25. ↑ Kóspál, Ágnes et al. (August 2009), "On the Relationship Between Debris Disks and Planets", The Astrophysical Journal Letters 700 (2): L73–L77, doi:10.1088/0004-637X/700/2/L73, Bibcode: 2009ApJ...700L..73K 
  26. ↑ 26.0 26.1 Hill, Michelle L.; Kane, Stephen R.; Campante, Tiago L.; Li, Zhexing; Dalba, Paul A.; Brandt, Timothy D.; White, Timothy R.; Pope, Benjamin J. S. et al. (2021), "Asteroseismology of iota Draconis and Discovery of an Additional Long-period Companion", The Astronomical Journal 162 (5): 211, doi:10.3847/1538-3881/ac1b31, Bibcode: 2021AJ....162..211H 

External links

Coordinates: Sky map 15h 24m 55.7747s, +58° 57′ 57.836″



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