Iota Chamaeleontis
  | |
| Observation data Epoch J2000 Equinox 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 mas/yr[1] Dec.: +134.880 mas/yr[1] |
| Parallax (π) | 17.3133±0.0528 mas[1] |
| Distance | 188.4 ± 0.6 ly (57.8 ± 0.2 pc) |
| Absolute magnitude (MV) | +1.52[2] |
| Details | |
| Mass | 1.88[6] M☉ |
| Radius | 3.4[7] R☉ |
| Luminosity | 19.1[7] L☉ |
| Temperature | 6,514[7] K |
| Metallicity [Fe/H] | −0.04[8] dex |
| Rotational velocity (v sin i) | 129.7[9] km/s |
| Age | 1.2±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 | |
| SIMBAD | data |
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 AU from the star with a mean temperature of 200 K.[14]
References
[edit]- 1 2 3 4 5 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- 1 2 3 4 5 6 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. XHIP record for this object at VizieR.
- ↑ 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.
- ↑ Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
- 1 2 3 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.
- 1 2 Bochanski, John J.; et al. (April 2018). "Fundamental Properties of Co-moving Stars Observed by Gaia". The Astronomical Journal. 155 (4): 17. arXiv:1801.00537. Bibcode:2018AJ....155..149B. doi:10.3847/1538-3881/aaaebe. S2CID 119256051. 149.
- 1 2 3 4 5 Schofield, Mathew; et al. (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, arXiv:1901.10148, Bibcode:2019ApJS..241...12S, doi:10.3847/1538-4365/ab04f5
- ↑ Nordström, B.; et al. (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. arXiv:astro-ph/0405198. Bibcode:2004A&A...418..989N. doi:10.1051/0004-6361:20035959. S2CID 11027621.
- 1 2 Reiners, Ansgar (January 2006), "Rotation- and temperature-dependence of stellar latitudinal differential rotation", Astronomy and Astrophysics, 446 (1): 267–277, arXiv:astro-ph/0509399, Bibcode:2006A&A...446..267R, doi:10.1051/0004-6361:20053911, S2CID 8642707
- ↑ "iot Cha". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 25 January 2016.
- ↑ 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. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID 14878976.
- ↑ Allen, J. S. "The Classification of Stellar Spectra". UCL Department of Physics and Astronomy: Astrophysics Group. Retrieved 1 January 2014.
- ↑ van Belle, Gerard T. (March 2012). "Interferometric observations of rapidly rotating stars". The Astronomy and Astrophysics Review. 20 (1): 51. arXiv:1204.2572. Bibcode:2012A&ARv..20...51V. doi:10.1007/s00159-012-0051-2. S2CID 119273474.
- ↑ Cotten, Tara H.; Song, Inseok (July 2016). "A Comprehensive Census of Nearby Infrared Excess Stars". The Astrophysical Journal Supplement Series. 225 (1): 24. arXiv:1606.01134. Bibcode:2016ApJS..225...15C. doi:10.3847/0067-0049/225/1/15. S2CID 118438871. 15.
