Astronomy:Iota Trianguli Australis
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Short description: Binary star in the constellation Triangulum Australe
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Triangulum Australe |
| Right ascension | 16h 27m 57.34498s[2] |
| Declination | −64° 03′ 28.5964″[2] |
| Apparent magnitude (V) | +5.27[3] |
| Characteristics | |
| Spectral type | F4 IV[4] |
| U−B color index | −0.02[3] |
| B−V color index | +0.36[3] |
| Variable type | γ Dor[5] |
| Astrometry | |
| Radial velocity (Rv) | −5.6±4.2[6] km/s |
| Proper motion (μ) | RA: +53.12[2] mas/yr Dec.: +25.45[2] mas/yr |
| Parallax (π) | 25.77 ± 0.51[2] mas |
| Distance | 127 ± 3 ly (38.8 ± 0.8 pc) |
| Absolute magnitude (MV) | +2.34[7] |
| Orbit[5] | |
| Period (P) | 39.880±0.002 d |
| Eccentricity (e) | 0.253±0.004 |
| Periastron epoch (T) | 54661.65 ± 0.11 HJD |
| Argument of periastron (ω) (secondary) | 93.1±1.1° |
| Semi-amplitude (K1) (primary) | 38.4±0.3 km/s |
| Semi-amplitude (K2) (secondary) | 43.9±0.3 km/s |
| Details | |
| ι TrA A | |
| Mass | 1.42[8] M☉ |
| Surface gravity (log g) | 4.28±0.14[8] cgs |
| Temperature | 7,045±240[8] K |
| Metallicity [Fe/H] | −0.16[9] dex |
| Rotational velocity (v sin i) | 13.0±0.9[7] km/s |
| Age | 735[8] Myr |
| ι TrA B | |
| Rotational velocity (v sin i) | 10.0±1.7[7] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Iota Trianguli Australis (ι Trianguli Australis) is a binary star[11] system in the constellation Triangulum Australe. It is visible to the naked eye with a combined apparent visual magnitude of +5.27.[3] Based upon an annual parallax shift of 25.77 mas as seen from the Earth, it is located around 127 light years from the Sun. The system appears to be moving closer to the Sun with a radial velocity of around −6 km/s.[6]
Iota Trianguli Australis is a double-lined spectroscopic binary system with an orbital period of 39.88 days and an eccentricity of 0.25. The brighter member, component A, is yellow-white hued F-type subgiant star and a Gamma Doradus type variable, pulsating by 0.12 magnitudes with a dominant period of 1.45 days.[5]
There a magnitude 9.42 visual companion, located 16.2 arcseconds away.[12] The pair show as a yellow and a white star when seen though a 7.5 cm telescope.[13]
References
- ↑ Light Curve, ESA, https://www.cosmos.esa.int/web/hipparcos/java-tools/light-curve, retrieved 22 August 2022.
- ↑ 2.0 2.1 2.2 2.3 2.4 van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V.
- ↑ 3.0 3.1 3.2 3.3 Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series 34: 1–49, Bibcode: 1978A&AS...34....1N.
- ↑ Malaroda, S. (August 1975), "Study of the F-type stars. I. MK spectral types", Astronomical Journal 80: 637–641, doi:10.1086/111786, Bibcode: 1975AJ.....80..637M.
- ↑ 5.0 5.1 5.2 De Cat, P. et al. (2009), "Is HD147787 a double-lined binary with two pulsating components? Preliminary results from a spectroscopic multi-site campaign", AIP Conference Proceedings 1170: 483–85, doi:10.1063/1.3246549, Bibcode: 2009AIPC.1170..483D.
- ↑ 6.0 6.1 de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics 546: 14, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D.
- ↑ 7.0 7.1 7.2 Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics 542: A116, doi:10.1051/0004-6361/201118724, Bibcode: 2012A&A...542A.116A.
- ↑ 8.0 8.1 8.2 8.3 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal 804 (2): 146, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
- ↑ Casagrande, L. et al. (June 2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy and Astrophysics 530: A138, doi:10.1051/0004-6361/201016276, Bibcode: 2011A&A...530A.138C.
- ↑ "iot TrA". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=iot+TrA.
- ↑ 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, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E.
- ↑ Mason, B. D. et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal 122 (6): 3466, doi:10.1086/323920, Bibcode: 2001AJ....122.3466M.
- ↑ Hartung, Ernst Johannes (1984), Astronomical Objects for Southern Telescopes, with an Addendum for Northern Observatories: A Handbook for Amateur Observers, CUP Archive, pp. 214, ISBN 0521318874, https://books.google.com/books?id=yWk5AAAAIAAJ&pg=PA214.
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