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Revision as of 21:11, 12 July 2021 by CigaretteNightmares (talk | contribs)(diff) ← Previous revision | Latest revision (diff) | Newer revision → (diff) Star in the constellation Reticulum
Location of ζ Reticuli (circled) | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Reticulum |
| ζ Ret | |
| Right ascension | 03 17 46.16331 |
| Declination | −62° 34′ 31.1541″ |
| Apparent magnitude (V) | 5.52 |
| ζ Ret | |
| Right ascension | 03 18 12.81853 |
| Declination | −62° 30′ 22.9048″ |
| Apparent magnitude (V) | 5.22 |
| Characteristics | |
| Spectral type | G3−5V + G2V |
| U−B color index | +0.08 / +0.01 |
| B−V color index | +0.63 / +0.58 |
| R−I color index | +0.34 / +0.34 |
| Astrometry | |
| ζ Ret | |
| Radial velocity (Rv) | +12.21±0.17 km/s |
| Proper motion (μ) | RA: +1,337.591 mas/yr Dec.: +649.930 mas/yr |
| Parallax (π) | 83.0625 ± 0.0739 mas |
| Distance | 39.27 ± 0.03 ly (12.04 ± 0.01 pc) |
| Absolute magnitude (MV) | 5.11±0.01 |
| Absolute bolometric magnitude (Mbol) | 5.03±0.03 |
| ζ Ret | |
| Radial velocity (Rv) | +11.5 km/s |
| Proper motion (μ) | RA: +1,331.151 mas/yr Dec.: +648.523 mas/yr |
| Parallax (π) | 83.0122 ± 0.1888 mas |
| Distance | 39.29 ± 0.09 ly (12.05 ± 0.03 pc) |
| Absolute magnitude (MV) | 4.83 |
| Absolute bolometric magnitude (Mbol) | 4.79±0.03 |
| Details | |
| ζ Ret | |
| Mass | 0.958 M☉ |
| Radius | 0.92 R☉ |
| Luminosity | 0.761 L☉ |
| Surface gravity (log g) | 4.54±0.03 cgs |
| Temperature | 5,720±13 K |
| Metallicity | −0.206 dex |
| Rotational velocity (v sin i) | 1.98 km/s |
| Age | 1.5–3.0 Gyr |
| ζ Ret | |
| Mass | 0.985 M☉ |
| Radius | 0.99 R☉ |
| Luminosity | 0.972 L☉ |
| Surface gravity (log g) | 4.53±0.02 cgs |
| Temperature | 5,861±12 K |
| Metallicity | −0.215 dex |
| Rotational velocity (v sin i) | 1.74 km/s |
| Age | 1.5–3.0 Gyr |
| Other designations | |
| ζ Reticuli, WDS J03182-6230 | |
| ζ Reticuli: ζ Ret, Zeta Ret, CPD−63°217, GJ 136, HD 20766, HIP 15330, HR 1006, SAO 248770, LFT 275, LHS 171, LTT 1573 | |
| ζ Reticuli: ζ Ret, Zeta Ret, CPD−62°265, GJ 138, HD 20807, HIP 15371, HR 1010, SAO 248774, LFT 276, LHS 172, LTT 1576 | |
| Database references | |
| SIMBAD | ζ Ret |
| ζ Ret | |
Zeta Reticuli, Latinized from ζ Reticuli, is a wide binary star system in the southern constellation of Reticulum. From the southern hemisphere the pair can be seen with the naked eye as a double star in very dark skies. Based upon parallax measurements, this system is located at a distance of about 39.3 light-years (12.0 parsecs) from Earth. Both stars are solar analogs that have characteristics similar to those of the Sun. They belong to the Zeta Herculis Moving Group of stars that share a common origin.
Nomenclature
At a declination of −62°, the system is not visible from Britain's latitude of +53°, so it never received a Flamsteed designation in John Flamsteed's 1712 Historia Coelestis Britannica. The Bayer designation for this star system, Zeta (ζ) Reticuli, originated in a 1756 star map by the French astronomer Abbé Nicolas Louis de Lacaille. Subsequently, the two stars received separate designations in the Cape Photographic Durchmusterung, which was processed between 1859 and 1903, then in the Henry Draper Catalogue, published between 1918 and 1924.
Characteristics
The double star Zeta Reticuli is located in the western part of the small Reticulum constellation, about 25′ from the constellation's border with Horologium. In dark southern skies, the two stars can be viewed separately with the naked eye, or with a pair of binoculars. ζ Reticuli has an apparent magnitude of 5.52, placing it on the border between 5th and 6th magnitude stars. ζ Reticuli is slightly brighter at magnitude 5.22.
The two stars are located at similar distances from the Sun and share the same motion through space, confirming that they are gravitationally bound and form a wide binary star system. They have an angular separation of 309.2 arc seconds (5.2 arc minutes); far enough apart to appear as a close pair of separate stars to the naked eye under suitable viewing conditions. The distance between the two stars is at least 3,750 AU (0.06 light-years, or almost a hundred times the average distance between Pluto and the Sun), so their orbital period is 170,000 years or more.
Both stars share similar physical characteristics to the Sun, so they are considered solar analogs. Their stellar classification is nearly identical to that of the Sun. ζ has 96% of the Sun's mass and 84% of the Sun's radius. ζ is slightly larger and more luminous than ζ, with 99% of the Sun's mass and 88% of the Sun's radius. The two stars are somewhat deficient in metals, having only 60% of the proportion of elements other than hydrogen and helium as compared to the Sun. For reasons that remain uncertain, ζ has an anomalously low abundance of beryllium. Two possible explanations are: during the star's formation it underwent multiple intense bursts of mass accretion from a rapidly rotating protostellar cloud, or else the star underwent rotational mixing brought on by a period of rapid rotation during the star's youth.
Both stars were considered unusual because they were thought to have had a lower luminosity than is normal for main sequence stars of their age and surface temperature. That is, they lie below the main sequence curve on the Hertzsprung-Russell diagram for newly formed stars. However, this was challenged, after using the much more accurate parallaxes from the Hipparcos catalogue (ESA, 1997), it was calculated that the stars actually have higher luminosities and so are shifted upwards, crossing them into the main sequence. Most stars will evolve above this curve as they age. ζ has an intermediate level of magnetic activity in its chromosphere with an erratic variability. ζ is more sedate, showing a much lower level of activity with a 10-year cycle. Although the kinematics of this system suggest that they belong to a population of older stars, the properties of their stellar chromospheres suggests that they are only about 2 billion years old.
This star system belongs to the Zeta Herculis Moving Group of stars that share a common motion through space, suggesting that they have a common origin. In the galactic coordinate system, the components of the space velocity for this system are equal to km/s for ζ and km/s for ζ. They are currently following an orbit through the Milky Way galaxy that has an eccentricity of 0.24. This orbit will carry the system as close as 17.4 kly (5.33 kpc) and as far as 28.6 kly (8.77 kpc) from the Galactic Center. The inclination of this orbit will carry the stars as much as 1.3 kly (0.4 kpc) from the plane of the galactic disk. This likely puts them outside the thick disk population of stars.
Stop.
See also
- Role of Zeta Reticuli in the story of the purported Betty and Barney Hill abduction by space aliens (Greys)
- Zeta Reticuli in fiction
- Project Serpo
References
- ^ 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.
- ^ Feinstein, A. (1966). "Photoelectric observations of Southern late-type stars". Informational Bulletin of the Southern Hemisphere. 8: 30. Bibcode:1966IBSH....8...30F.
- ^ 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
- ^ del Peloso, E. F.; da Silva, L.; Porto de Mello, G. F. (June 2000). "zeta and zeta Reticuli and the existence of the zeta Herculis group". Astronomy and Astrophysics. 358: 233–241. Bibcode:2000A&A...358..233D.
- ^ Holmberg, J.; Nordström, B.; Andersen, J. (July 2009). "The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics". Astronomy and Astrophysics. 501 (3): 941–947. arXiv:0811.3982. Bibcode:2009A&A...501..941H. doi:10.1051/0004-6361/200811191. S2CID 118577511.
- Evans, D. S. (June 20–24, 1966). Batten, Alan Henry; Heard, John Frederick (eds.). "The Revision of the General Catalogue of Radial Velocities". Determination of Radial Velocities and Their Applications. 30. University of Toronto: International Astronomical Union: 57. Bibcode:1967IAUS...30...57E.
{{cite journal}}: Unknown parameter|book-title=ignored (help) - ^ 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.
- ^ Takeda, G.; et al. (2007). "Stellar parameters of nearby cool stars. II. Physical properties of ~1000 cool stars from the SPOCS catalog". Astrophysical Journal Supplement Series. 168 (2): 297–318. arXiv:astro-ph/0607235. Bibcode:2007ApJS..168..297T. doi:10.1086/509763. S2CID 18775378. Note: see VizieR catalogue J/ApJS/168/297.
- ^ Eiroa, C.; Marshall, J. P.; Mora, A.; Montesinos, B.; Absil, O.; Augereau, J. Ch.; Bayo, A.; Bryden, G.; Danchi, W.; Del Burgo, C.; Ertel, S.; Fridlund, M.; Heras, A. M.; Krivov, A. V.; Launhardt, R.; Liseau, R.; Löhne, T.; Maldonado, J.; Pilbratt, G. L.; Roberge, A.; Rodmann, J.; Sanz-Forcada, J.; Solano, E.; Stapelfeldt, K.; Thébault, P.; Wolf, S.; Ardila, D.; Arévalo, M.; Beichmann, C.; et al. (2013). "DUst around NEarby Stars. The survey observational results". Astronomy and Astrophysics. 555: A11. arXiv:1305.0155. Bibcode:2013A&A...555A..11E. doi:10.1051/0004-6361/201321050. S2CID 377244.
- ^ Adibekyan, V.; Delgado-Mena, E.; Figueira, P.; Sousa, S. G.; Santos, N. C.; Faria, J. P.; González Hernández, J. I.; Israelian, G.; Harutyunyan, G.; Suárez-Andrés, L.; Hakobyan, A. A. (2016). "Ζ Reticuli, its debris disk, and its lonely stellar companion ζ Ret. Different Tc trends for different spectra". Astronomy and Astrophysics. 591: A34. arXiv:1605.01918. Bibcode:2016A&A...591A..34A. doi:10.1051/0004-6361/201628453. S2CID 119313511.
- ^ Santos, N. C.; et al. (October 2004). "Beryllium anomalies in solar-type field stars". Astronomy and Astrophysics. 425 (3): 1013–1027. arXiv:astro-ph/0408109. Bibcode:2004A&A...425.1013S. doi:10.1051/0004-6361:20040510. S2CID 17279966.
- ^ Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008). "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics". The Astrophysical Journal. 687 (2): 1264–1293. arXiv:0807.1686. Bibcode:2008ApJ...687.1264M. doi:10.1086/591785. S2CID 27151456.
- Ridpath, Ian (1989). Star tales. James Clarke & Co. p. 11. ISBN 0-7188-2695-7.
- "Naming astronomical objects". International Astronomical Union. Retrieved 2011-12-16.
- Streicher, Magda (December 2009). "Reticulum: The Celestial Crosshairs". Monthly Notes of the Astronomical Society of South Africa. 68 (11/12): 242–246. Bibcode:2009MNSSA..68..242S.
- ^ da Silva, L.; Foy, R. (May 1987). "Zeta-1 and Zeta-2 RETICULI - A puzzling solar-type twin system". Astronomy and Astrophysics. 177 (1–2): 204–216. Bibcode:1987A&A...177..204D.
- ^ Makarov, V. V.; Zacharias, N.; Hennessy, G. S. (November 2008). "Common Proper Motion Companions to Nearby Stars: Ages and Evolution". The Astrophysical Journal. 687 (1): 566–578. arXiv:0808.3414. Bibcode:2008ApJ...687..566M. doi:10.1086/591638. S2CID 17811620.
- Kaler, James B. "ZETA RET (Zeta Reticuli)". Stars. University of Illinois. Retrieved 2011-11-16.
- Pasinetti Fracassini, L. E.; et al. (February 2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics". Astronomy and Astrophysics. 367 (2): 521–524. arXiv:astro-ph/0012289. Bibcode:2001A&A...367..521P. doi:10.1051/0004-6361:20000451. S2CID 425754. Note: using the method of Perrin and Karoji (1987).
- A metallicity of −0.22 indicates that they have the following proportion of metals compared to the Sun: 10 = 0.603, or 60%.
- Viallet, M.; Baraffe, I. (October 2012). "Scenarios to explain extreme Be depletion in solar-like stars: accretion or rotation effects?". Astronomy & Astrophysics. 546: 7. arXiv:1209.1812. Bibcode:2012A&A...546A.113V. doi:10.1051/0004-6361/201219445. S2CID 55593554. A113.
- Vieytes, M.; Mauas, P.; Cincunegui, C. (October 2005). "Chromospheric models of solar analogues with different activity levels". Astronomy and Astrophysics. 441 (2): 701–709. Bibcode:2005A&A...441..701V. doi:10.1051/0004-6361:20052651.
- Flores, M.; et al. (May 2018). "ζ + ζ Reticuli binary system: a puzzling chromospheric activity pattern". Monthly Notices of the Royal Astronomical Society. 476 (2): 2751–2759. arXiv:1801.08104. Bibcode:2018MNRAS.476.2751F. doi:10.1093/mnras/sty234.
{{cite journal}}: CS1 maint: unflagged free DOI (link) - Rocha-Pinto, Helio J.; Maciel, Walter J.; Castilho, Bruno V. (March 2002). "Chromospherically young, kinematically old stars". Astronomy and Astrophysics. 384 (3): 912–924. arXiv:astro-ph/0112452. Bibcode:2002A&A...384..912R. doi:10.1051/0004-6361:20011815. S2CID 16982360.
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External links
- "Zeta Reticuli". SolStation. Retrieved 2008-08-31.
- "Zeta(1) Reticuli". The Internet Stellar Database. Retrieved 2008-08-31.
- "Zeta(2) Reticuli". The Internet Stellar Database. Retrieved 2008-08-31.
- "Zeta(3) Reticuli". Hatirla Beni Belgesel. Archived from the original on 2011-07-23. Retrieved 2008-08-31.
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