Iota Chamaeleontis

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Iota Chamaeleontis
Diagram showing star positions and boundaries of the Chamaeleon constellation and its surroundings
Cercle rouge 100%.svg

Location of ι Chamaeleontis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Chamaeleon
Right ascension 09h 24m 09.22492s[1]
Declination −80° 47′ 12.7567″[1]
Apparent magnitude (V) 5.36[2]
Characteristics
Spectral type F3/5 III/V[2]
U−B color index +0.01[3]
B−V color index +0.445[3]
Astrometry
Radial velocity (Rv) 7.00[4] km/s
Proper motion (μ) RA: -138.46[1] mas/yr
Dec.: 135.06[1] mas/yr
Parallax (π) 17.20 ± 0.20[1] mas
Distance 190 ± 2 ly
(58.1 ± 0.7 pc)
Absolute magnitude (MV) +1.32[5]
Details
Temperature 6272[5] K
Metallicity [Fe/H] -0.04[6] dex
Rotational velocity (v sin i) 129.7[5] km/s
Other designations
ι Cha, CD-80° 329, HD 82554, HIP 46107, SAO 258530, HR 3795, GC 13066[2]
Database references
SIMBAD data

Iota Chamaeleontis (ι Cha, ι Chamaeleontis) is a star in the constellation Chamaeleon. It has an apparent magnitude of about 5.3, meaning that it is just barely visible to the naked eye. Based upon parallax measurements made by the Hipparcos spacecraft, this star is around 190 light years away from the Sun.[1] Its spectral type is F3/5 III/IV, meaning it is an F-type star, likely a subgiant;[7] its proper motion is relatively high.[2]

References[edit]

  1. ^ a b c d e f van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. Bibcode:2007A&A...474..653V. arXiv:0708.1752Freely accessible. doi:10.1051/0004-6361:20078357. 
  2. ^ a b c d "iot Cha". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 25 January 2016. 
  3. ^ a b Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Bibcode:1986EgUBV........0M. 
  4. ^ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. Bibcode:2006AstL...32..759G. arXiv:1606.08053Freely accessible. doi:10.1134/S1063773706110065. Retrieved 12 December 2016. 
  5. ^ a b c Reiners, A. (January 2006). "Rotation- and temperature-dependence of stellar latitudinal differential rotation". Astronomy and Astrophysics. 446 (1): 267–277. Bibcode:2006A&A...446..267R. arXiv:astro-ph/0509399Freely accessible. doi:10.1051/0004-6361:20053911. 
  6. ^ 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. Bibcode:2004A&A...418..989N. arXiv:astro-ph/0405198Freely accessible. doi:10.1051/0004-6361:20035959. 
  7. ^ Allen, J. S. "The Classification of Stellar Spectra". UCL Department of Physics and Astronomy: Astrophysics Group. Retrieved 1 January 2014.