Zeta Tucanae

Zeta Tucanae
Location of ζ Tucanae (near center).
Observation data
Epoch J2000      Equinox J2000
Constellation Tucana
Right ascension 00h 20m 04.2586334956s[1]
Declination −64° 52′ 29.257190108″[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)9.280±0.0003[5] km/s
Proper motion (μ) RA: 1706.747±0.162[1] mas/yr
Dec.: 1164.959±0.156[1] mas/yr
Parallax (π)116.1826±0.1334 mas[1]
Distance28.07 ± 0.03 ly
(8.607 ± 0.010 pc)
Absolute magnitude (MV)4.67[6]
Details
Mass0.985±0.033[7] M☉
Radius1.044±0.010[7] R☉
Luminosity1.232±0.039[7] L☉
Surface gravity (log g)4.394±0.007[7] cgs
Temperature5,924±130[7] K
Metallicity [Fe/H]−0.21±0.09[7] dex
Rotation15.6534±0.0066[8] days
Rotational velocity (v sin i)3.295±0.259[9] km/s
Age5.3±0.5[7] Gyr
Other designations
ζ Tuc, FK5 10, GC 401, GJ 17, HD 1581, HIP 1599, HR 77, SAO 248163, LHS 5, LTT 167[10]
Database references
SIMBADdata

Zeta Tucanae, Latinized from ζ Tucanae, is a star in the constellation Tucana. It is a spectral class F9.5 main sequence star. Based upon parallax measurements by the Hipparcos spacecraft, it is approximately 28.0 light years from Earth.[11] This is one of the least variable stars observed during the Hipparcos mission.[4][12] The star is faintly visible to the naked eye, at an apparent magnitude of +4.23.

Characteristics

Zeta Tucanae is a solar-type star, with similar mass, radius, luminosity, and effective temperature as the Sun, and has an estimated age of 5.3 billion years. Despite having a slightly lower mass, this star is more luminous than the Sun.[7] It is slightly metal-poor,[7] which means the portion of elements heavier than helium is smaller relative to the Sun. The solar-like qualities make it a target of interest for investigating the possible existence of a life-bearing planet.[12]

Zeta Tucanae has a rotation period of 15.65 days,[13][8] and possesses a magnetic activity cycle with period of approximately 950 days.[8][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.[12]

Based upon an excess emission of infrared radiation at 70 micrometres, this system is believed to have a debris disk. It is radiating with a maximum temperature of 218 K, corresponding to a minimum distance from the star of 2.3 astronomical units.[16]

As of 2025, no planet has been discovered in orbit around this star.[8]

See also

References

  1. ^ a b c d e 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.
  2. ^ 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.
  3. ^ 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): 99. Bibcode:1966CoLPL...4...99J.
  4. ^ 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.
  5. ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  6. ^ Elgarøy, Øystein; Engvold, Oddbjørn; Lund, Niels (March 1999). "The Wilson-Bappu effect of the MgII K line - dependence on stellar temperature, activity and metallicity". Astronomy and Astrophysics. 343: 222–228. Bibcode:1999A&A...343..222E.
  7. ^ a b c d e f g h i Huber, Daniel; et al. (2022-02-01). "A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c". The Astronomical Journal. 163 (2): 79. arXiv:2108.09109. doi:10.3847/1538-3881/ac3000. ISSN 0004-6256.
  8. ^ a b c d Harada, Caleb K.; Dressing, Courtney D.; Kane, Stephen R.; Blunt, Sarah; Dietrich, Jamie; Hinkel, Natalie R.; Li, Zhexing; Mamajek, Eric; Rice, Malena; Tuchow, Noah W.; Turtelboom, Emma V.; Wittenmyer, Robert A. (2024-09-16). "SPORES-HWO. II. Limits on Planetary Companions of Future High-contrast Imaging Targets from $>$20 Years of HIRES and HARPS Radial Velocities". arXiv.org. Retrieved 2025-08-13.
  9. ^ Perdelwitz, V.; Trifonov, T.; Teklu, J. T.; Sreenivas, K. R.; Tal-Or, L. (2024). "Analysis of the public HARPS/ESO spectroscopic archive" (PDF). Astronomy & Astrophysics. 683. EDP Sciences: A125. arXiv:2311.12438. Bibcode:2024A&A...683A.125P. doi:10.1051/0004-6361/202348263. ISSN 0004-6361. Retrieved 2025-08-13.
  10. ^ "zet Tuc -- High Proper Motion Star". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2025-08-13.
  11. ^ 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, S2CID 18759600 Note: see VizieR catalogue I/311.
  12. ^ 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. S2CID 119459291.
  13. ^ Laliotis, Katherine; Burt, Jennifer A.; Mamajek, Eric E.; Li, Zhexing; Perdelwitz, Volker; Zhao, Jinglin; Butler, R. Paul; Holden, Bradford; Rosenthal, Lee; Fulton, B. J.; Feng, Fabo; Kane, Stephen R.; Bailey, Jeremy; Carter, Brad; Crane, Jeffrey D.; Furlan, Elise; Gnilka, Crystal L.; Howell, Steve B.; Laughlin, Gregory; Shectman, Stephen A.; Teske, Johanna K.; Tinney, C. G.; Vogt, Steven S.; Wang, Sharon Xuesong; Wittenmyer, Robert A. (2023-04-01). "Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions". The Astronomical Journal. 165 (4): 176. doi:10.3847/1538-3881/acc067. ISSN 0004-6256.
  14. ^ Lovis, C.; Dumusque, X.; Santos, N. C.; Bouchy, F.; Mayor, M.; Pepe, F.; Queloz, D.; Ségransan, D.; Udry, S. (2011-07-26). "The HARPS search for southern extra-solar planets. XXXI. Magnetic activity cycles in solar-type stars: statistics and impact on precise radial velocities". arXiv.org. Retrieved 2025-08-13.
  15. ^ Woolley, Richard van der Riet (1970). "Catalogue of Stars within 25 Parsecs of the Sun". Royal Observatory Annals. 5. Herstmonceux, Royal Greenwich Observatory. Retrieved 2009-09-02.
  16. ^ Trilling, D. E.; et al. (2008). "Debris Disks around Sun-like Stars". The Astrophysical Journal. 674 (2): 1086–1105. arXiv:0710.5498. Bibcode:2008ApJ...674.1086T. doi:10.1086/525514. S2CID 54940779.
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