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.
 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 | |
| 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 | |
  Gliese 105 Location of Gliese 105 in the constellation Cetus | |
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]
References
edit- ^ a b van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600. Archived from the original on 2019-12-07. Retrieved 2013-08-14. Vizier catalog entry Archived 2018-09-30 at the Wayback Machine
- ^ a b c d 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.
- ^ a b Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C. S2CID 115529446. Archived from the original on 2021-04-21. Retrieved 2021-11-16.
- ^ a b c d e Mann, Andrew W.; Feiden, Gregory A.; Gaidos, Eric; Boyajian, Tabetha; von Braun, Kaspar (2015). "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius". The Astrophysical Journal. 804 (1): 38. arXiv:1501.01635. Bibcode:2015ApJ...804...64M. doi:10.1088/0004-637X/804/1/64. S2CID 19269312.
- ^ a b c "GJ 105 C". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 4 June 2017.
- ^ a b c d Golimowski, David A.; et al. (2000). "The Very Low Mass Component of the Gliese 105 System". The Astronomical Journal. 120 (4): 2082–2088. arXiv:astro-ph/0006230. Bibcode:2000AJ....120.2082G. doi:10.1086/301567. S2CID 119505312.
- ^ a b 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.
- ^ a b Mermilliod, J.-C. (1986). "Compilation of Eggen's UBV data, transformed to UBV (unpublished)". Catalogue of Eggen's UBV Data. Bibcode:1986EgUBV........0M.
- ^ 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.
- ^ a b c d 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.
- ^ 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.
- ^ a b c d 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.
- ^ a b c Feng, Fabo; Butler, R Paul; Jones, Hugh R A.; Phillips, Mark W.; Vogt, Steven S.; Oppenheimer, Rebecca; Holden, Bradford; Burt, Jennifer; Boss, Alan P. (2021). "Optimized modelling of Gaia–Hipparcos astrometry for the detection of the smallest cold Jupiter and confirmation of seven low-mass companions". Monthly Notices of the Royal Astronomical Society. 507 (2): 2856–2868. arXiv:2107.14056. Bibcode:2021MNRAS.507.2856F. doi:10.1093/mnras/stab2225.
- ^ a b c Ghezzi, L.; Cunha, K.; Smith, V. V.; De Araújo, F. X.; Schuler, S. C.; de la Reza, R. (2010). "Stellar Parameters and Metallicities of Stars Hosting Jovian and Neptunian Mass Planets: A Possible Dependence of Planetary Mass on Metallicity". The Astrophysical Journal. 720 (2): 1290–1302. arXiv:1007.2681. Bibcode:2010ApJ...720.1290G. doi:10.1088/0004-637X/720/2/1290. S2CID 118565025.
- ^ a b c 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.
- ^ 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
- ^ 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.
- ^ "A Really Cool Star: The Dim, Low-Temperature GL 105C". HubbleSite. 14 September 1995. Retrieved 4 June 2017.
External links
edit- Gliese 105 / HR 753 ABC Archived 2006-03-16 at the Wayback Machine SolStation entry.
- Gliese 105 Archived 2008-01-08 at the Wayback Machine