Astronomy:HD 23079

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Short description: Star in the constellation Reticulum
HD 23079 / Tupi
Observation data
Equinox J2000.0]] (ICRS)
Constellation Reticulum
Right ascension  03h 39m 43.09600s[1]
Declination −52° 54′ 57.0174″[1]
Apparent magnitude (V) 7.12[2]
Characteristics
Spectral type F9.5V[3]
B−V color index 0.583±0.009[2]
Astrometry
Radial velocity (Rv)+0.648±0.0004[4] km/s
Proper motion (μ) RA: −192.838[1] mas/yr
Dec.: −92.021[1] mas/yr
Parallax (π)29.8633 ± 0.0194[1] mas
Distance109.22 ± 0.07 ly
(33.49 ± 0.02 pc)
Absolute magnitude (MV)4.47[2]
Details
Mass1.01±0.02[5] M☉
Radius1.08±0.02[5] R☉
Luminosity1.372±0.005[5] L☉
Surface gravity (log g)4.37±0.02[6] cgs
Temperature6,003±36[5] K
Metallicity [Fe/H]−0.12±0.01[2] dex
Rotation15.0±2.6[6] days
Rotational velocity (v sin i)1.281±0.160[7] km/s
Age5.1±1.0[5] Gyr
Other designations
Tupi, CD–53°738, GC 4401, HD 23079, HIP 17096, SAO 233208, LTT 1739[8]
Database references
SIMBADdata
Exoplanet Archivedata

HD 23079, also named Tupi, is a star in the southern constellation of Reticulum. Since the star has an apparent visual magnitude of 7.12,[2] it is not visible to the naked eye, but at least in binoculars it should be easily visible. Parallax measurements give a distance estimate of 109 light-years from the Sun. It is slowly drifting further away with a radial velocity of +0.65 km/s.[4]

This object is an inactive F-type main sequence star with a stellar classification of F9.5V;[3] in between F8 and G0. This indicates it is generating energy through core hydrogen fusion. The star is similar to the Sun, but is slightly hotter and more massive.[9] It is about 5.1 billion years old[5] and it is spinning slowly with a projected rotational velocity of 1.3 km/s.[7] The metallicity of this star is below solar, meaning the abundance of elements other than hydrogen and helium is lower than in the Sun.[2]

Nomenclature

This was one of the systems selected to be named in the 2019 NameExoWorlds campaign during the 100th anniversary of the IAU, which assigned each country a star and planet to be named. This system was assigned to Brazil. The approved names were Tupi for the star and Guarani for planet b, named after the Tupi and Guarani indigenous peoples of Brazil.[10][11]

Planetary system

In October 2001, a giant planet orbiting the star was announced, detected by the radial velocity method.[12] The orbit of this object is similar to that of Mars, and the presence of such a large planet would have a strong impact on an Earth-like planet in the habitable zone of this Star.[9] Any Earthlike planet would have to exist either as an exomoon or Trojan planet of HD 23079 b.

With additional observations, the discovery of a second planet, HD 23079 c, was announced in 2025. This is a sub-Neptune mass planet orbiting closer to the star, with a period of only 5.75 days.[6]

The HD 23079 planetary system[6]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
c ≥8.1±0.8 M⊕ — 5.74894+0.00022
−0.00021 		0.07+0.09
−0.05 		— —
b / Guarani ≥2.66±0.05 MJ 1.586±0.003[13] 735.7±0.4 0.072+0.012
−0.011 		— —

References

  1. ↑ 1.0 1.1 1.2 1.3 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A. 
  3. ↑ 3.0 3.1 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. doi:10.1086/504637. Bibcode: 2006AJ....132..161G. 
  4. ↑ 4.0 4.1 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 Bonfanti, A. et al. (2015). "Revising the ages of planet-hosting stars". Astronomy and Astrophysics 575: A18. doi:10.1051/0004-6361/201424951. Bibcode: 2015A&A...575A..18B. http://www.aanda.org/articles/aa/full_html/2015/03/aa24951-14/aa24951-14.html. 
  6. ↑ 6.0 6.1 6.2 6.3 Delisle, J.-B. et al. (September 2025). "Architecture of planetary systems with and without outer giant planets I. Inner planet detections around HD 23079, HD 196067, and HD 86226". Astronomy & Astrophysics. 
  7. ↑ 7.0 7.1 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. doi:10.1051/0004-6361/201731533. A76. Bibcode: 2018A&A...615A..76S. 
  8. ↑ "HD 23079". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+23079. 
  9. ↑ 9.0 9.1 Eberle, J.; Cuntz, M.; Quarles, B.; Musielak, Z. E. (October 2011). "Case studies of habitable Trojan planets in the system of HD 23079". International Journal of Astrobiology 10 (4): 325–334. doi:10.1017/S1473550411000176. Bibcode: 2011IJAsB..10..325E. 
  10. ↑ "International Astronomical Union | IAU". https://www.iau.org/news/pressreleases/detail/iau1912/. 
  11. ↑ "Approved names" (in en). http://www.nameexoworlds.iau.org/final-results. 
  12. ↑ Tinney, C. G. et al. (2002). "Two Extrasolar Planets from the Anglo-Australian Planet Search". The Astrophysical Journal 571 (1): 528–531. doi:10.1086/339916. Bibcode: 2002ApJ...571..528T. 
  13. ↑ Wittenmyer, Robert A. et al. (2020). "Cool Jupiters greatly outnumber their toasty siblings: occurrence rates from the Anglo-Australian Planet Search". Monthly Notices of the Royal Astronomical Society 492 (1): 377–383. doi:10.1093/mnras/stz3436. Bibcode: 2020MNRAS.492..377W. 

Coordinates: Sky map 03h 39m 43.0952s, −52° 54′ 57.017″



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