Astronomy:Iota Chamaeleontis

From HandWiki
Short description: Star in the constellation Chamaeleon
Iota Chamaeleontis
Location of ι Chamaeleontis (circled)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Chamaeleon
Right ascension  09h 24m 09.224s[1]
Declination –80° 47′ 12.758″[1]
Apparent magnitude (V) 5.34[2]
Characteristics
Spectral type F3/5 III/V[3]
U−B color index +0.01[4]
B−V color index +0.454±0.003[2]
Astrometry
Radial velocity (Rv)−3.57±0.66[5] km/s
Proper motion (μ) RA: –138.717[1] mas/yr
Dec.: +134.880[1] mas/yr
Parallax (π)17.3133 ± 0.0528[1] mas
Distance188.4 ± 0.6 ly
(57.8 ± 0.2 pc)
Absolute magnitude (MV)+1.52[2]
Details
Mass1.88[6] M☉
Radius3.4[7] R☉
Luminosity19.1[7] L☉
Temperature6,514[7] K
Metallicity [Fe/H]−0.04[8] dex
Rotational velocity (v sin i)129.7[9] km/s
Age1.2±0.1[2] Gyr
Other designations
ι Cha, CD−80°329, FK5 2753, GC 13066, HD 82554, HIP 46107, HR 3795, SAO 258530[10]
Database references
SIMBADdata

Iota Chamaeleontis is a single[11] star in the southern circumpolar constellation of Chamaeleon. Its name is a Bayer designation that is Latinized from ι Chamaeleontis, and abbreviated Iota Cha or ι Cha. This star is visible to the naked eye as a dim, yellow-white hued point of light, having an apparent magnitude of about 5.3.[2] Based upon parallax measurements,[5] this star is 188.4 light-years (57.8 pc) away from the Sun, but it is drifting closer with a radial velocity of −4 km/s.[5]

Spectra of this star taken in different years have been given types of F3IV/V and F5III, leading to a mean published type of F3/5 III/V, with the suspicion that the spectrum is variable. It is an F-type star, likely an evolving subgiant.[12]

Iota Cha has 1.9[6] times the mass of the Sun with 3.4[7] times the Sun's radius. It is 1.2[2] billion years old with a high rate of spin, showing a projected rotational velocity of 130 km/s.[9] This is giving it an oblate shape with an equatorial bulge some 9% larger than the polar radius.[13] The star is radiating 19.1 times the Sun's luminosity from its photosphere at an effective temperature of 6,514 K.[7] An infrared excess suggests a circumstellar disk of dust is orbiting at a distance of 8.3 astronomical unit|AU from the star with a mean temperature of 200 K.[14]

References

  1. ↑ 1.0 1.1 1.2 1.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A  XHIP record for this object at VizieR.
  3. ↑ Houk, N.; Cowley, A. P. (1975). University of Michigan Catalogue of two-dimensional spectral types for the HD stars. Volume I. Declinations -90_ to -53_ƒ0. Bibcode: 1975mcts.book.....H. 
  4. ↑ Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode: 1986EgUBV........0M. 
  5. ↑ 5.0 5.1 5.2 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  6. ↑ 6.0 6.1 Bochanski, John J. (April 2018). "Fundamental Properties of Co-moving Stars Observed by Gaia". The Astronomical Journal 155 (4): 17. doi:10.3847/1538-3881/aaaebe. 149. Bibcode: 2018AJ....155..149B. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 Schofield, Mathew (2019), "The Asteroseismic Target List for Solar-like Oscillators Observed in 2 minute Cadence with the Transiting Exoplanet Survey Satellite", The Astrophysical Journal Supplement Series 241 (1): 12, doi:10.3847/1538-4365/ab04f5, Bibcode: 2019ApJS..241...12S 
  8. ↑ Nordström, B. (2004). "The Geneva-Copenhagen survey of the Solar neighbourhood. Ages, metallicities, and kinematic properties of ˜14 000 F and G dwarfs". Astronomy and Astrophysics 418: 989–1019. doi:10.1051/0004-6361:20035959. Bibcode: 2004A&A...418..989N. 
  9. ↑ 9.0 9.1 Reiners, Ansgar (January 2006), "Rotation- and temperature-dependence of stellar latitudinal differential rotation", Astronomy and Astrophysics 446 (1): 267–277, doi:10.1051/0004-6361:20053911, Bibcode: 2006A&A...446..267R 
  10. ↑ "iot Cha". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=iot+Cha. 
  11. ↑ Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society 389 (2): 869–879. doi:10.1111/j.1365-2966.2008.13596.x. Bibcode: 2008MNRAS.389..869E. 
  12. ↑ Allen, J. S.. "The Classification of Stellar Spectra". http://www.star.ucl.ac.uk/~pac/spectral_classification.html. Retrieved 1 January 2014. 
  13. ↑ van Belle, Gerard T. (March 2012). "Interferometric observations of rapidly rotating stars". The Astronomy and Astrophysics Review 20 (1): 51. doi:10.1007/s00159-012-0051-2. Bibcode: 2012A&ARv..20...51V. 
  14. ↑ Cotten, Tara H.; Song, Inseok (July 2016). "A Comprehensive Census of Nearby Infrared Excess Stars". The Astrophysical Journal Supplement Series 225 (1): 24. doi:10.3847/0067-0049/225/1/15. 15. Bibcode: 2016ApJS..225...15C. 



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:Iota_Chamaeleontis&oldid=4390535"