Gliese 105

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Gliese 105
Gliese 105.gif
Gliese 105 A (left) and C (right).
Observation data
Epoch J2000       Equinox J2000
Constellation Cetus
Gliese 105 A
Right ascension 02h 36m 04.89466s [1]
Declination +06° 53′ 12.7466″ [1]
Apparent magnitude  (V)5.83 [2]
Gliese 105 B
Right ascension 02h 36m 15.357s [3]
Declination +06° 52′ 19.14″ [3]
Apparent magnitude  (V)11.670 [4]
Gliese 105 C
Right ascension 02h 36m 04.66s [5]
Declination +06° 53′ 14.8″ [5]
Apparent magnitude  (V)16.77 [5]
Characteristics
Gliese 105 AC
Spectral type K3 V [2] + M7 V [6]
U−B color index +0.800 [7]
B−V color index +0.972 [7]
Gliese 105 B
Spectral type M4.0 V
U−B color index +1.10 [8]
B−V color index +1.61 [8]
Variable type BY Dra
Astrometry
Gliese 105 A
Radial velocity (Rv)25.8 ± 0.1 [9]  km/s
Proper motion (μ)RA: 1778.585±0.430 [10]   mas/yr
Dec.: 1477.306±0.248 [10]   mas/yr
Parallax (π)138.3400 ± 0.3177  mas [10]
Distance 23.58 ± 0.05  ly
(7.23 ± 0.02  pc)
Absolute magnitude  (MV)6.50 [11]
Gliese 105 B
Proper motion (μ)RA: 1801.671±0.043 [12]   mas/yr
Dec.: 1450.487±0.038 [12]   mas/yr
Parallax (π)138.4371 ± 0.0420  mas [12]
Distance 23.560 ± 0.007  ly
(7.223 ± 0.002  pc)
Orbit [13]
Period (P)76.107 ± 1.820 yr
Semi-major axis (a)17.0 ± 0.7 au
Eccentricity (e)0.641 ± 0.004
Inclination (i)45.5 ± 2.8°
Longitude of the node (Ω)122.5 ± 3.4°
Periastron epoch (T)JD 2430414 ± 669
Argument of periastron (ω)
(primary)		133.4 ± 0.6°
Semi-amplitude (K1)
(primary)		711.7 ± 2.2 km/s
Details
Gliese 105 A
Mass 0.70 ± 0.10 [14]   M☉
Radius 0.650 ± 0.053 [2]   R☉
Luminosity (bolometric)0.26 [14]   L☉
Surface gravity (log g)4.40 ± 0.24 [15]   cgs
Temperature 4777 ± 91 [15]   K
Metallicity [Fe/H]−0.03 ± 0.09 [15]   dex
Gliese 105 B
Mass 0.246 ± 0.025 [4]   M☉
Radius 0.278 ± 0.010 [4]   R☉
Temperature 3284 ± 60 [4]   K
Metallicity [Fe/H]−0.12 ± 0.03 [4]   dex
Other designations
268 G. Cet, Gl  105, CCDM  J02361+0653, BD+06° 398
Gliese 105 AC: HR  753, HD  16160, LHS  15, LTT  10858, SAO  110636, FK5  1073, G  73-70, G 76-11, LFT  217, HIP  12114
Gliese 105 B: BX  Cet, LHS  16, LTT  10859, G  73-71, G 76-12, LFT  217
Database references
SIMBAD Gl 105
Gl 105 A
Gl 105 B
Gl 105 C
Cetus constellation map.svg
Red circle.svg
Gliese 105
Location of Gliese 105 in the constellation Cetus

Gliese 105 (also known as 268 G. Ceti) is a triple star system in the constellation of Cetus. It is located relatively near the Sun at a distance of 23.6 light-years (7.2 parsecs). [10] [12] Despite this, even the brightest component is barely visible with the unaided eye (see Bortle scale). No planets have yet been detected around any of the stars in this system.

This is a triple system with three stars that are all less massive than the Sun. The brightest component is designated HD 16160, and is known as Gliese 105 A. It is a K-type main-sequence star, [2] about 70% the mass of the Sun. [14] This star is unusual because its eruptions appear to not conform to the Waldmeier effect—i.e., the strongest eruptions of HD 16160 are not the ones characterized by the fast eruption onset. [16]

A nearby star has a similar proper motion to Gliese 105 A, so it is assumed to be physically associated with the primary, and is known as Gliese 105 B. The two have an estimated separation of 1,200 astronomical units (au). It is a BY Draconis variable star whose brightness varies between 11.64 and 11.68 magnitudes; for that reason it has been given the designation BX Ceti. [17]

A third companion, known as Gliese 105 C, lies much closer to A, currently at a distance of approximately 24 au. [6] The pair A-C have an estimated orbital period of about 70 years. [13] While detected directly, Gliese 105 C has also been observed to perturb Gliese 105 A from its usual position; [6] from that, its orbit is estimated to have a high eccentricity of around 0.64 and a semimajor axis of 17 au. [13] Gliese 105 C is an extremely faint red dwarf. [6] It is roughly 8 to 9 percent the mass of the Sun, and it is about 20,000 times fainter than its parent star in visible light—at a distance of 1 au (the distance from the Earth to the Sun) it would only be four times brighter than the full moon. [18]

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References

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  2. 1 2 3 4 van Belle, Gerard T.; von Braun, Kaspar (2009). "Directly Determined Linear Radii and Effective Temperatures of Exoplanet Host Stars". The Astrophysical Journal. 694 (2): 1085–1098. arXiv: 0901.1206 . Bibcode:2009ApJ...694.1085V. doi:10.1088/0004-637X/694/2/1085. S2CID   18370219.
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  5. 1 2 3 "GJ 105 C". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 4 June 2017.
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  7. 1 2 González-Hernández, J. I.; Bonifacio, P. (2009). "A new implementation of the infrared flux method using the 2MASS catalogue". Astronomy & Astrophysics. 497 (2): 497. arXiv: 0901.3034 . Bibcode:2009A&A...497..497G. doi:10.1051/0004-6361/200810904. S2CID   16026032.
  8. 1 2 Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
  9. ↑ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID   119231169.
  10. 1 2 3 4 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  11. ↑ Cardini, D. (January 2005), "Mg II chromospheric radiative loss rates in cool active and quiet stars", Astronomy and Astrophysics, 430: 303–311, arXiv: astro-ph/0409683 , Bibcode:2005A&A...430..303C, doi:10.1051/0004-6361:20041440, S2CID   12136256.
  12. 1 2 3 4 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
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  15. 1 2 3 Paletou, F.; Böhm, T.; Watson, V.; Trouilhet, J.-F. (2015). "Inversion of stellar fundamental parameters from ESPaDOnS and Narval high-resolution spectra". Astronomy & Astrophysics. 573: A67. arXiv: 1411.4859 . Bibcode:2015A&A...573A..67P. doi:10.1051/0004-6361/201424741. S2CID   118466868.
  16. ↑ Garg, Suyog; Karak, Bidya Binay; Egeland, Ricky; Soon, Willie; Baliunas, Sallie (2019), "Waldmeier Effect in Stellar Cycles", The Astrophysical Journal, 886 (2): 132, arXiv: 1909.12148 , Bibcode:2019ApJ...886..132G, doi: 10.3847/1538-4357/ab4a17 , S2CID   202888617
  17. ↑ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  18. ↑ "A Really Cool Star: The Dim, Low-Temperature GL 105C". HubbleSite. 14 September 1995. Retrieved 4 June 2017.
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