Theta Antliae
In this article, we will explore in detail Theta Antliae, a topic of great relevance in contemporary society. Theta Antliae has captured the attention of numerous experts and academics due to its significant impact on various aspects of daily life. Through meticulous analysis and the collection of empirical evidence, we will seek to shed light on the different nuances and facets that characterize Theta Antliae, in order to provide a comprehensive and enriching vision on this topic. In addition, the practical and theoretical implications of Theta Antliae will be examined, in order to promote a deeper and more detailed understanding of its importance in the current landscape.
  | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Antlia[1] |
| Right ascension | 09h 44m 12.09512s[2] |
| Declination | −27° 46′ 10.1011″[2] |
| Apparent magnitude (V) | 4.79[3] |
| Characteristics | |
| Spectral type | G7 III + A8 Vm[4] |
| U−B color index | +0.35[3] |
| B−V color index | +0.50[3] |
| Astrometry | |
| Radial velocity (Rv) | +24.0[5] km/s |
| Proper motion (μ) | RA: −53.23[2] mas/yr Dec.: +37.24[2] mas/yr |
| Parallax (π) | 9.61±0.46 mas[2] |
| Distance | 340 ± 20 ly (104 ± 5 pc) |
| Absolute magnitude (MV) | −0.30[1] |
| Orbit[6] | |
| Companion | θ Ant B |
| Period (P) | 18.266±0.185 yr |
| Semi-major axis (a) | 0.110±0.002″ |
| Eccentricity (e) | 0.404±0.005 |
| Inclination (i) | 123.6±1.0° |
| Longitude of the node (Ω) | 3.5±1.0° |
| Periastron epoch (T) | 2020.143±0.200 |
| Argument of periastron (ω) (secondary) | 141.2±3.0° |
| Details[6] | |
| θ Ant A | |
| Mass | 1.8±0.1 M☉ |
| θ Ant B | |
| Mass | 2.1±0.5 M☉ |
| Other designations | |
| θ Antliae, Tet Ant, θ Ant, CD−27 6881, FK5 366, HD 84367, HIP 47758, HR 3871, SAO 177908, PPM 256646[7] | |
| Database references | |
| SIMBAD | data |
Theta Antliae is a binary star system in the southern constellation of Antlia. Its identifier is a Bayer designation that was Latinized from θ Antliae, and is abbreviated Tet Ant or θ Ant, respectively. The pair have a combined apparent visual magnitude of +4.78,[3] which is bright enough to be faintly visible to the naked eye. The brighter component is magnitude +5.30 while the secondary is +6.18.[8] Based upon parallax measurements, it is located at a distance of around 340 light-years (104 parsecs) from Earth. The system is receding with a heliocentric radial velocity of +24 km/s.[5]
The binary nature of this system was discovered by W. S. Finsen in 1952.[6] The primary component of this system, θ Antliae A, has a stellar classification of A8 Vm,[4] indicating that it is an A-type main sequence star with enhanced metallic lines in its spectrum. The companion, θ Antliae B, is a giant star with a classification of G7 III.[4] The pair have an orbital period of 18.3 years, a significant eccentricity of 0.4, and an angular separation of 0.1 arcseconds.[6]
References
- ^ a b 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.
- ^ a b c d e van Leeuwen, F. (November 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.
- ^ a b c d Johnson, H. L.; et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory, 4 (99): 99, Bibcode:1966CoLPL...4...99J.
- ^ a b c Ginestet, N.; Carquillat, J. M. (December 2002), "Spectral Classification of the Hot Components of a Large Sample of Stars with Composite Spectra, and Implication for the Absolute Magnitudes of the Cool Supergiant Components", The Astrophysical Journal Supplement Series, 143 (2): 513–537, Bibcode:2002ApJS..143..513G, doi:10.1086/342942.
- ^ a b Wilson, Ralph Elmer (1953), "General catalogue of stellar radial velocities", Washington, Carnegie Institution of Washington, Bibcode:1953GCRV..C......0W.
- ^ a b c d Docobo, J. A.; Andrade, M. (January 2013), "Dynamical and physical properties of 22 binaries discovered by W. S. Finsen", Monthly Notices of the Royal Astronomical Society, 428 (1): 321–339, Bibcode:2013MNRAS.428..321D, doi:10.1093/mnras/sts045.
- ^ "tet Ant", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2012-06-28.
- ^ 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.
