HD 66141

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HD 66141
Canis Minor constellation map.svg
Red circle.svg
Location of HD 66141 (circled)
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Canis Minor
Right ascension 08h 02m 15.93692s [1]
Declination +02° 20′ 04.4588″ [1]
Apparent magnitude  (V)+4.39 [2]
Characteristics
Spectral type K2IIIbFe-0.5: [3]
B−V color index 1.252±0.008 [2]
Astrometry
Radial velocity (Rv)+71.57±0.01 [2]  km/s
Proper motion (μ)RA: −28.194  mas/yr [1]
Dec.: 105.65  mas/yr [1]
Parallax (π)12.5234 ± 0.1142  mas [1]
Distance 260 ± 2  ly
(79.9 ± 0.7  pc)
Absolute magnitude  (MV)−0.07 [2]
Details [4]
Mass 0.98±0.06  M☉
Radius 23.57±0.40 [5]   R☉
Luminosity 209±9 [5]   L☉
Habitable zone inner limit13.45±0.41 [5] AU
Habitable zone outer limit26.38±0.77 [5] AU
Surface gravity (log g)2.09±0.06  cgs
Temperature 4,521±53 [5]   K
Metallicity [Fe/H]−0.52±0.05  dex
Rotational velocity (v sin i)1.91±0.45 km/s
Age 9.18±2.09  Gyr
Other designations
G Canis Minoris, G CMi, 13 Puppis (obsolete), NSV  17713, BD+02°1854, FK5  2623, GC  10891, HD  66141, HIP  39311, HR  3145, SAO  116260, CCDM 08022+0221, WDS J08023+0220A [6] [7]
Database references
SIMBAD data
Exoplanet Archive data

HD 66141 is a single [8] star in the equatorial constellation of Canis Minor. It has the Bayer designation G Canis Minoris, [6] the Gould designation 50 G. Canis Minoris, [7] and has the HR 3145 identifier from the Bright Star Catalogue . [6] When first catalogued it was in the Puppis constellation and was designated "13 Puppis", but it subsequently migrated to Canis Minor. [9] Bode gave it the Bayer designation of Lambda Canis Minoris. [10]

Contents

Properties

This star has an orange hue and is bright enough to be faintly visible to the naked eye on a dark night, having an apparent visual magnitude of +4.39. [2] It is located at a distance of approximately 260 light years from the Sun based on parallax, [1] and is drifting further away with a radial velocity of +71.6 km/s. [2] The star is considered a member of the thin disk population. [4] It has one known substellar companion, previously believed to be a planet, [11] but now thought to be a likely brown dwarf, with some caveats. [12]

The stellar classification of HD 66141 is K2IIIbFe-0.5:, [3] which indicates an evolved K-type giant star with a mild underabundance of iron. It is an estimated nine billion years old with 0.98 times the mass of the Sun [4] and has expanded to 23.5 times the Sun's radius. [5] Over 2003 to 2012 a starspot was periodically dimming its light. [11] The star is radiating 209 times the luminosity of the Sun from its photosphere at an effective temperature of 4,521 K. [5]

A magnitude 10.32 visual companion was reported by J. Glaisher in 1842. As of 2015, it was located at an angular separation of 224.90  arcseconds along a position angle of 315°. [13]

Planetary system

From December 2003 to January 2012, the team B.-C. Lee, I. Han, and M.-G. Park observed HD 66141 with "the fiber-fed Bohyunsan Observatory Echelle Spectrograph (BOES) at Bohyunsan Optical Astronomy Observatory (BOAO)". [11]

In 2012, a long-period, wide-orbiting exoplanet was deduced by radial velocity. This was published in November.

However, in 2024, a study using astrometry from the Gaia spacecraft suggest that HD 66141 b is actually a brown dwarf, with a maximum mass estimated at 23.9+7.2
−6.4  MJ , based on a large RUWE in the astrometric solution (which could imply that there is a brown dwarf orbiting HD 66141), but they also note that mechanisms such as calibration errors could also explain the large RUWE. A bayesian analysis combining astrometry and radial velocity also measure an orbital inclination of 17 degrees and an orbital period of 480.7 days (1.316 years). [12]

The HD 66141 planetary system
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b≤23.9+7.2
−6.4 [12]   MJ 		1.2 ± 0.1 [11] 480.7±0.1 [11] 0.07 ± 0.03 [11] 17+3
−4 [12] ° 		—

Related Research Articles

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<span class="mw-page-title-main">HD 47536</span> Star in the constellation Canis Major

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<span class="mw-page-title-main">HD 81040 b</span>

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HD 179079 is a star with an exoplanetary companion in the equatorial constellation of Aquila. It has an apparent visual magnitude of approximately 7.96, making it too faint to be readily visible to the naked eye. The distance to this star can be determine using parallax measurements, which yields an estimate of approximately 228 light years. It is drifting further away with a radial velocity of +20 km/s.

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HD 175167 is a star with an exoplanet companion in the southern constellation of Pavo. It is too faint to be visible with the naked eye at an apparent visual magnitude of 8.01. The system is located at a distance of 232 light-years from the Sun based on parallax measurements, and it is drifting further away with a radial velocity of 5 km/s. It shows a high proper motion, traversing the celestial sphere at an angular rate of 0.190 arcsec yr−1.

HD 27631 is a star with an orbiting exoplanet in the southern constellation of Horologium. It is too faint to be visible to the naked eye, having an apparent visual magnitude of 8.24. The distance to this system is 164 light years based on parallax measurements. It is drifting further away with a radial velocity of 21 km/s.

HD 156279 is a star with a pair of orbiting exoplanets located in the northern constellation of Draco. It has various alternate designations, including HIP 84171 and BD+63 1335. Parallax measurements yield a distance of 118 light years from the Sun, but it is drifting closer with a radial velocity of −20 km/s. Despite an absolute magnitude of 5.25, at that distance the star is too faint to be visible to the naked eye with an apparent visual magnitude of 8.17. It is presumed to be a single star, as in 2019 all imaging surveys have failed to find any stellar companions.

HD 121056, or HIP 67851, is an aging giant star with a pair of orbiting exoplanets located in the southern constellation of Centaurus. This star is dimly visible to the naked eye with an apparent visual magnitude of 6.17. It is located at a distance of 209 light years from the Sun, based on parallax measurements, and is drifting further away with a radial velocity of 5.6 km/s.

HD 42618 is a well-studied star with an exoplanetary companion in the equatorial constellation of Orion. With an apparent visual magnitude of 6.85 it is too faint to be readily visible to the naked eye. This system is located at a distance of 79.6 light years from the Sun based on parallax measurements. It has a relatively high proper motion, traversing the celestial sphere at an angular rate of 0.321″ per year. HD 42618 is drifting closer with a radial velocity of −53.5 km/s and is predicted to come as near as 42.6 light-years in around 297,000 years.

References

  1. 1 2 3 4 5 6 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.
  2. 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. S2CID   119257644.
  3. 1 2 Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". The Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  4. 1 2 3 Jofré, E.; et al. (2015). "Stellar parameters and chemical abundances of 223 evolved stars with and without planets". Astronomy & Astrophysics. 574: A50. arXiv: 1410.6422 . Bibcode:2015A&A...574A..50J. doi:10.1051/0004-6361/201424474. S2CID   53666931.
  5. 1 2 3 4 5 6 7 Baines, Ellyn K.; Jones, Jeremy; Clark, James H.; Schmitt, Henrique R.; Stone, Jordan M. (January 2025). "Eighteen Exoplanet Host Stars from the NPOI Data Archive". The Astronomical Journal. 169 (2): 83. doi: 10.3847/1538-3881/ad9bb1 . ISSN   1538-3881.
  6. 1 2 3 "G CMi". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2021-01-27.
  7. 1 2 Gould, Benjamin Apthorp (1879). "Uranometria Argentina catalog of bright southern stars". Resultados del Observatorio Nacional Argentino en Cordoba. 1. Buenos Aires. Bibcode:1879RNAO....1.....G . Retrieved 2021-01-27.
  8. ↑ 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.
  9. ↑ Griffin, R. F. (1999). "Spectroscopic binary orbits from photoelectric radial velocities. Paper 148: HR 7955". The Observatory. 119: 272–283. Bibcode:1999Obs...119..272G.
  10. ↑ Wagman, Morton (2003). Lost Stars: Lost, Missing and Troublesome Stars from the Catalogues of Johannes Bayer, Nicholas Louis de Lacaille, John Flamsteed, and Sundry Others. Blacksburg, VA: The McDonald & Woodward Publishing Company. p. 460. Bibcode:2003lslm.book.....W. ISBN   978-0-939923-78-6.{{cite book}}: |journal= ignored (help)
  11. 1 2 3 4 5 6 Lee, B.-C.; et al. (2012). "Detection of an exoplanet around the evolved K giant HD 66141". Astronomy & Astrophysics. 548: A118. arXiv: 1211.2054 . Bibcode:2012A&A...548A.118L. doi:10.1051/0004-6361/201118014. S2CID   54984721.
  12. 1 2 3 4 Wallace, A. L.; Casey, A. R.; Brown, A. G. A.; Castro-Ginard, A. (2024-11-10). "Detection and Characterisation of Giant Planets with Gaia Astrometry". Monthly Notices of the Royal Astronomical Society. 536 (3): 2485. arXiv: 2411.06705 . Bibcode:2025MNRAS.536.2485W. doi: 10.1093/mnras/stae2769 .
  13. ↑ Mason, B. D.; et al. (2014). "The Washington Visual Double Star Catalog". The Astronomical Journal. 122 (6): 3466–3471. Bibcode:2001AJ....122.3466M. doi: 10.1086/323920 .
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