French
DeutschLambda2 Fornacis
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Fornax |
| Right ascension | 02h 36m 58.60775s[1] |
| Declination | −34° 34′ 40.7113″[1] |
| Apparent magnitude (V) | 5.78[2] |
| Characteristics | |
| Spectral type | G1V[3] |
| B−V color index | +0.653±0.005[2] |
| Astrometry | |
| Radial velocity (Rv) | +11.16±0.12[1] km/s |
| Proper motion (μ) | RA: −18.363 mas/yr[1] Dec.: −259.002 mas/yr[1] |
| Parallax (π) | 39.2946 ± 0.0305 mas[1] |
| Distance | 83.00 ± 0.06 ly (25.45 ± 0.02 pc) |
| Absolute magnitude (MV) | 3.74±0.04[4] |
| Details | |
| A | |
| Mass | 1.16±0.03[5] M☉ |
| Radius | 1.63±0.04[5] R☉ |
| Luminosity | 3.03[2] L☉ |
| Surface gravity (log g) | 4.12±0.03[5] cgs |
| Temperature | 5,829±80[5] K |
| Metallicity [Fe/H] | 0.10±0.08[5] dex |
| Rotational velocity (v sin i) | 1.4 or 3.2[6] km/s |
| Age | 6.3±0.9[5] Gyr |
| B | |
| Mass | 0.11[7] M☉ |
| Other designations | |
| Database references | |
| SIMBAD | data |
| Exoplanet Archive | data |
| ARICNS | data |
λ2 Fornacis, Latinized as Lambda2 Fornacis, is the primary of a binary star system in the southern constellation of Fornax. It is just visible to the naked eye as a dim, yellow-hued point of light with an apparent visual magnitude of 5.78.[2] It is located 83 light years distant from the Sun, based on stellar parallax, and is drifting further away with a radial velocity of +11.1 km/s.[1]
This object is a G-type main-sequence star with a stellar classification of G1V.[3] It is considered a solar analog, being photometrically-similar to the Sun.[9] The star is an estimated 6.4 billion years old with 1.16 times the mass of the Sun and 1.63 times the Sun's radius.[5] It is radiating three[2] times the luminosity of the Sun from its photosphere at an effective temperature of 5,829 K.[5] The abundance of elements with more mass than helium is 55% higher than in the Sun.[4][10]
There is a faint co-moving companion star located to the east of the main star at an angular separation of 45″. This is most likely an M5–M6 class red dwarf with 0.11 times the Sun's mass. The projected separation between the pair is about 1,000 AU.[7]
Planetary system
[edit]Precision Doppler spectroscopy from an intensive 48 night observing campaign on the Anglo-Australian Telescope has revealed the presence of a low-mass extrasolar planet orbiting the star.[11] This object has an orbital period of 17.25 days and an eccentricity of 0.14. It has a minimum (baseline) mass of 16.8 M🜨.[5]
| Companion (in order from star) | Mass | Semimajor axis (AU) | Orbital period (days) | Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | ≥16.8+1.2 −1.3 M🜨 | 0.14±0.01[11] | 17.251+0.002 −0.003 | 0.35±0.05 | — | — |
References
[edit]- ^ a b c d e f 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.
- ^ a b c d e 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.
- ^ a b Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: spectroscopy of stars earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
- ^ a b da Silva, L.; et al. (November 2006). "Basic physical parameters of a selected sample of evolved stars". Astronomy and Astrophysics. 458 (2): 609–623. arXiv:astro-ph/0608160. Bibcode:2006A&A...458..609D. doi:10.1051/0004-6361:20065105. S2CID 9341088.
- ^ a b c d e f g h i j Nielsen, M. B.; Ball, W. H.; Standing, M. R.; Triaud, A. H. M. J.; Buzasi, D.; Carboneau, L.; Stassun, K. G.; Kane, S. R.; Chaplin, W. J.; Bellinger, E. P.; Mosser, B.; Roxburgh, I. W.; Çelik Orhan, Z.; Yıldız, M.; Örtel, S. (September 2020). "TESS asteroseismology of the known planet host star λ2 Fornacis". Astronomy & Astrophysics. 641: A25. arXiv:2007.00497. doi:10.1051/0004-6361/202037461. ISSN 0004-6361.
- ^ Soto, M. G.; Jenkins, J. S. (July 2018). "Spectroscopic Parameters and atmosphEric ChemIstriEs of Stars (SPECIES). I. Code description and dwarf stars catalogue". Astronomy & Astrophysics. 615: 28. arXiv:1801.09698. Bibcode:2018A&A...615A..76S. doi:10.1051/0004-6361/201731533. S2CID 119107228. A76.
- ^ a b Mugrauer, M.; et al. (March 2014). "New wide stellar companions of exoplanet host stars". Monthly Notices of the Royal Astronomical Society. 439 (1): 1063–1070. Bibcode:2014MNRAS.439.1063M. doi:10.1093/mnras/stu044.
- ^ "lam02 For". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-09-23.
- ^ Datson, Juliet; et al. (February 2015). "Spectroscopic study of solar twins and analogues". Astronomy & Astrophysics. 574: 12. arXiv:1412.8168. Bibcode:2015A&A...574A.124D. doi:10.1051/0004-6361/201425000. S2CID 53708062. A124.
- ^ 10+0.19 = 1.55
- ^ a b O’Toole, Simon; et al. (2009). "A Neptune-mass Planet Orbiting the Nearby G Dwarf HD16417". The Astrophysical Journal. 697 (2): 1263–1268. arXiv:0902.4024. Bibcode:2009ApJ...697.1263O. doi:10.1088/0004-637X/697/2/1263. S2CID 16341718.
