HD 83443

HD 83443 is an orange dwarf star approximately 134 light-years away[1] in the constellation of Vela. As of 2000, at least one extrasolar planet has been confirmed to be orbiting the star.[11]

HD 83443
Observation data
Epoch J2000.0 (ICRS)      Equinox J2000.0 (ICRS)
Constellation Vela
Right ascension 9h 37m 11.8276s[1]
Declination –43° 16′ 19.9326″[1]
Apparent magnitude (V) 8.23[2]
Characteristics
Spectral type K0 V[3]
U−B color index +0.50[4]
B−V color index +0.811[2]
Variable type Constant[5]
Astrometry
Radial velocity (Rv)+29.21±0.08[6] km/s
Proper motion (μ) RA: 21.742[1] mas/yr
Dec.: −120.183[1] mas/yr
Parallax (π)24.4215 ± 0.0372[1] mas
Distance133.6 ± 0.2 ly
(40.95 ± 0.06 pc)
Absolute magnitude (MV)5.04[2]
Details
Mass0.79±0.07 M☉[7]
0.98±0.07 M☉[8]
1.004±0.031[9] M☉
Radius0.94±0.02[7] R☉
Luminosity0.88[2] L☉
Surface gravity (log g)4.43±0.08[8] cgs
Temperature5,511±45[8] K
Metallicity [Fe/H]0.34±0.03[8] dex
Rotation35.3 d[2]
Rotational velocity (v sin i)1.4[2] km/s
Age3.2 Gyr[2]
2.638±2.489[9] Gyr
Other designations
Kalausi, CD–42°5452, GC 13300, HD 83443, HIP 47202, SAO 221348[10]
Database references
SIMBADdata

The star HD 83443 is named Kalausi. The name was selected in the NameExoWorlds campaign by Kenya, during the 100th anniversary of the IAU. The word Kalausi means a very strong whirling column of wind in the Dholuo language.[12][13]

Planetary system

The planet HD 83443 b was discovered in 2000 by the Geneva Extrasolar Planet Search Team led by Michel Mayor.[11] It has a minimum mass comparable to Saturn's, and its orbit at the time of discovery was one of the shortest known taking only three days to complete one revolution around the star. This hot Jupiter is likely to be slightly larger than Jupiter in radius.

In 2000, the same year that planet b was found, another planet around HD 83443 was announced by the Geneva Team. The new planet was designated as "HD 83443 c". It had a mass smaller than planet b and a short, very eccentric orbit.[14] Its orbital period, 28.9 days, was especially interesting, because it indicated a 10:1 orbital resonance between the planets. However, a team led by astronomer Paul Butler did not detect any signal indicating the existence of the second planet.[5] New observations by the Geneva team could not detect the signal either and the discovery claim had to be retracted. The origin of the signal, which was "highly significant" in the earlier data is not yet clear.[2]

The HD 83443 planetary system[2]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b >0.38 MJ 0.039 2.98565 ± 0.00003 0.013 ± 0.013 — —

References
  1. 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.
  2. Mayor, M.; et al. (2004). "The CORALIE survey for southern extra-solar planets XII. Orbital solutions for 16 extra-solar planets discovered with CORALIE". Astronomy and Astrophysics. 415 (1): 391–402. arXiv:astro-ph/0310316. Bibcode:2004A&A...415..391M. doi:10.1051/0004-6361:20034250. S2CID 5233877.
  3. Houk, N. (1978). "Michigan Catalogue of two dimensional spectral types for the HD stars". Michigan Spectral Survey. 2. Bibcode:1978mcts.book.....H.
  4. Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Bibcode:1986EgUBV........0M. Cite journal requires |journal= (help)
  5. Butler, R. Paul; et al. (2002). "On the Double-Planet System around HD 83443". The Astrophysical Journal. 578 (1): 565–572. arXiv:astro-ph/0206178. Bibcode:2002ApJ...578..565B. doi:10.1086/342471. hdl:2299/167. S2CID 15659545.
  6. Nidever, David L.; et al. (2013). "Radial Velocities for 889 Late-Type Stars". The Astrophysical Journal Supplement Series. 141 (2): 503–522. arXiv:astro-ph/0112477. Bibcode:2002ApJS..141..503N. doi:10.1086/340570. S2CID 51814894.
  7. Stassun, Keivan G.; et al. (2016). "Accurate Empirical Radii and Masses of Planets and Their Host Stars with Gaia Parallaxes". The Astronomical Journal. 153 (3): 136. arXiv:1609.04389. Bibcode:2017AJ....153..136S. doi:10.3847/1538-3881/aa5df3. S2CID 119219062.
  8. Santos, N. C.; et al. (August 2013). "SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs. I. New atmospheric parameters and masses for 48 stars with planets". Astronomy & Astrophysics. 556: 11. arXiv:1307.0354. Bibcode:2013A&A...556A.150S. doi:10.1051/0004-6361/201321286. S2CID 55237847. A150.
  9. Delgado Mena, E.; et al. (April 2019), "Abundance to age ratios in the HARPS-GTO sample with Gaia DR2. Chemical clocks for a range of [Fe/H]", Astronomy & Astrophysics, 624: 24, arXiv:1902.02127, Bibcode:2019A&A...624A..78D, doi:10.1051/0004-6361/201834783, A78
  10. "HD 83443". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 28 August 2017.
  11. "Exoplanets Galore!" (Press release). Garching, Germany: European Southern Observatory. April 15, 2000. Retrieved December 30, 2012.
  12. "Approved names". NameExoworlds. IAU. Retrieved 2020-01-02.
  13. "iau1912 — Press Release". www.iau.org. =International Astronomical Union. Retrieved 2020-01-02.
  14. "European Southern Observatory: Six Extrasolar Planets Discovered". SpaceRef Interactive Inc. 7 August 2000. Retrieved 2 August 2009.
  • "HD 83443". The Extrasolar Planets Encyclopaedia. Retrieved 2008-06-11.

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