Zeta Tucanae
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 Location of ζ Tucanae (near center). |
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| Observation data Epoch J2000 Equinox J2000 |
|
|---|---|
| Constellation | Tucana |
| Right ascension | 00h 20m 04.25995s[1] |
| Declination | –64° 52′ 29.2549″[1] |
| Apparent magnitude (V) | 4.23 |
| Characteristics | |
| Spectral type | F9.5 V[2] |
| U−B color index | 0.02[3] |
| B−V color index | 0.58[3] |
| Variable type | None[4] |
| Astrometry | |
| Radial velocity (Rv) | 8.8 ± 0.02[5] km/s |
| Proper motion (μ) | RA: 1,707.42[1] mas/yr Dec.: 1,164.30[1] mas/yr |
| Parallax (π) | 116.46 ± 0.16[1] mas |
| Distance | 28.01 ± 0.04 ly (8.59 ± 0.01 pc) |
| Absolute magnitude (MV) | 4.56 |
| Details | |
| Mass | 0.99 ± 0.02[6] M☉ |
| Radius | 0.90 ± 0.08[7] R☉ |
| Luminosity | 1.3[citation needed] L☉ |
| Surface gravity (log g) | 4.48[8] |
| Temperature | 5,970[8] K |
| Metallicity | [Fe/H] = –0.07[8] |
| Rotational velocity (v sin i) | 3.0[9] km/s |
| Age | 2.1–3.02[10][11] Gyr |
| Other designations | |
Zeta Tucanae (ζ Tuc, ζ Tucanae) is a star in the constellation Tucana. It is a spectral class F9.5 main sequence star with an apparent magnitude of +4.23. Despite having a slightly lower mass, this star is more luminous than the Sun.[6] Based upon parallax measurements by the Hipparcos spacecraft, it is approximately 28.0 light years from Earth.[1] This is one of the least variable stars observed during the Hipparcos mission.[4][13]
The composition and mass of this star are very similar to the Sun, with a slightly lower mass and an estimated age of three billion years. The solar-like qualities make it a target of interest for investigating the possible existence of a life-bearing planet.[13]
Based upon an excess emission of infrared radiation at 70 micrometres, this system is believed to have a debris disk. The disk is orbiting the star at a minimum radius of 2.3 astronomical units. It is radiating with a maximum temperature of 218 K.[10] As of 2009, no planet has been discovered in orbit around this star.[14]
The components of this star's space velocity are U = −60, V = −4 and W = −38 km/s. These correspond to the velocity toward the galactic center, the velocity along the direction of galactic rotation, and the velocity toward the north galactic pole, respectively.[15] It is orbiting through the galaxy at a mean distance of 8.4 kpc from the galactic center and with an orbital eccentricity of 0.16.[13]
[edit] References
- ^ a b c d e f van Leeuwen, Floor (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, arXiv:0708.1752v1, Bibcode 2007A&A...474..653V, doi:10.1051/0004-6361:20078357 Note: see VizieR catalogue I/311.
- ^ 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, Bibcode 2006AJ....132..161G, doi:10.1086/504637
- ^ a b Johnson, H. L.; Iriarte, B.; Mitchell, R. I.; Wisniewskj, W. Z. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory 4 (99). Bibcode 1966CoLPL...4...99J.
- ^ a b Adelman, S. J. (February 2001). "Research Note Hipparcos photometry: The least variable stars". Astronomy and Astrophysics 367 (1): 297–298. Bibcode 2001A&A...367..297A. doi:10.1051/0004-6361:20000567.
- ^ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick. Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. University of Toronto: International Astronomical Union. pp. 57–63. Bibcode 1967IAUS...30...57E.
- ^ a b Santos, N. C.; Israelian, G.; Mayor, M. (July 2001). "The metal-rich nature of stars with planets". Astronomy and Astrophysics 373 (3): 1019–1031. arXiv:astro-ph/0105216. Bibcode 2001A&A...373.1019S. doi:10.1051/0004-6361:20010648.
- ^ Perrin, M.-N.; Karoji, H. (1987). "Stellar radius determination from IRAS 12-micron fluxes". Astronomy and Astrophysics 172: 235–240. Bibcode 1987A&A...172..235P.
- ^ a b c Castro, S.; Porto de Mello, G. F.; da Silva, L. (May 1999). "Copper and barium abundances in the Ursa Major Moving Group". Monthly Notices of the Royal Astronomical Society 305 (3): 693–700. arXiv:astro-ph/9901209. Bibcode 1999MNRAS.305..693C. doi:10.1046/j.1365-8711.1999.02455.x.
- ^ O'Toole, S. J. et al (2009). "The Frequency of Low-mass Exoplanets". The Astrophysical Journal 701 (2): 1732–1741. arXiv:0906.4619. Bibcode 2009ApJ...701.1732O. doi:10.1088/0004-637X/701/2/1732.
- ^ a b Trilling, D. E.; et al. (2008). "Debris Disks around Sun-like Stars". The Astrophysical Journal 674 (2): 1086–1105. Bibcode 2008ApJ...674.1086T. doi:10.1086/525514.
- ^ Mamajek, Eric E.; Hillenbrand, Lynne A. (2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". The Astrophysical Journal 687 (2): 1264–1293. Bibcode 2008ApJ...687.1264M. doi:10.1086/591785.
- ^ "LHS 5 -- High proper-motion Star". SIMBAD. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Zeta+Tucanae. Retrieved 2010-05-21.
- ^ a b c Porto de Mello, Gustavo; del Peloso, Eduardo F.; Ghezzi, Luan (2006). "Astrobiologically Interesting Stars Within 10 Parsecs of the Sun". Astrobiology 6 (2): 308–331. arXiv:astro-ph/0511180. Bibcode 2006AsBio...6..308P. doi:10.1089/ast.2006.6.308. PMID 16689649.
- ^ Kóspál, Ágnes; Ardila, David R.; Moór, Attila; Ábrahám, Péter (August 2009). "On the Relationship Between Debris Disks and Planets". The Astrophysical Journal Letters 700 (2): L73–L77. Bibcode 2009ApJ...700L..73K. doi:10.1088/0004-637X/700/2/L73.
- ^ Woolley, Richard van der Riet (1970). "Catalogue of Stars within 25 Parsecs of the Sun". Royal Observatory Annals (Herstmonceux, Royal Greenwich Observatory) 5. http://heasarc.gsfc.nasa.gov/W3Browse/all/woolley.html. Retrieved 2009-09-02.
[edit] External links
- Zeta Tucanae at SolStation.
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