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{{short description|Star in the constellation Reticulum}} {{short description|Binary star system in the constellation Reticulum}}
{{Starbox begin {{Starbox begin
| name=ζ Reticuli | name=ζ Reticuli
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}} }}
{{Starbox character {{Starbox character
| class={{nowrap|G3−5V + G2V}}<ref name="aaa358" /> | class={{nowrap|G3−5V + G2V}}<ref name="aaa358"/>
| r-i=+0.34 / +0.34<ref name="aaa358" /> | r-i=+0.34 / +0.34<ref name="aaa358"/>
| v-r= <!--V-R color--> | v-r= <!--V-R color-->
| b-v=+0.63 / +0.58<ref name=ibsh8_30/> | b-v=+0.63 / +0.58<ref name=ibsh8_30/>
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}} }}
{{Starbox detail {{Starbox detail
| source=<!----> | source=<ref name=Fuhrmann/>
| component1=ζ<sup>1</sup> Ret | component1=ζ<sup>1</sup> Ret
| mass=0.958<ref name=apjss168/> | mass=0.94
| radius=0.92<ref name=apjss168/> | radius={{val|0.90|0.03}}
| temperature={{Val|5720|13|fmt=commas}}<ref name=adibekyan/> | temperature={{Val|5729|60|fmt=commas}}
| gravity={{Val|4.54|0.03}}<ref name=adibekyan/> | gravity={{Val|4.5|0.1}}
| luminosity = 0.761<ref name=eiroa/> | luminosity = 0.761<ref name=eiroa/>
| metal_fe=−0.206<ref name=adibekyan/> | metal_fe={{val|-0.25|0.06}}
| rotational_velocity=1.98<ref name=aaa425/> | rotational_velocity={{val|2.2|0.8}}
| age_gyr=1.5–3.0<ref name="apj687"/> | age_gyr=1.5–3.0<ref name="apj687"/>
| component2=ζ<sup>2</sup> Ret | component2=ζ<sup>2</sup> Ret
| mass2=0.985<ref name=apjss168/> | mass2=0.96
| radius2=0.99<ref name=apjss168/> | radius2={{val|0.98|0.03}}
| gravity2={{Val|4.53|0.02}}<ref name=adibekyan/> | gravity2={{val|4.43|0.10}}
| luminosity2=0.972<ref name=eiroa/> | luminosity2=0.972<ref name=eiroa/>
| temperature2={{Val|5861|12|fmt=commas}}<ref name=adibekyan/> | temperature2={{Val|5861|12|fmt=commas}}<ref name=adibekyan/>
| metal2_fe=−0.215<ref name=adibekyan/> | metal2_fe={{val|-0.26|0.03}}
| rotational_velocity2=1.74<ref name=aaa425/> | rotational_velocity2=1.74<ref name=aaa425/>
| age_gyr2=1.5–3.0<ref name="apj687" /> | age_gyr2=1.5–3.0<ref name="apj687"/>
}}<!-- }}<!--
-->{{Starbox catalog -->{{Starbox catalog
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{{Starbox end}} {{Starbox end}}


'''Zeta&nbsp;Reticuli''', ] from '''ζ&nbsp;Reticuli''', is a wide ] system in the southern ] of ]. From the southern hemisphere the pair can be seen with the naked eye as a ] in ]. Based upon ] measurements, this system is located at a distance of about {{convert|39.3|ly|pc|abbr=off|lk=on}} from ]. Both stars are ]s that have characteristics similar to those of the Sun. They belong to the ] of stars that share a common origin. '''Zeta&nbsp;Reticuli''', ] from '''ζ&nbsp;Reticuli''', is a wide ] system in the ] ] of ]. From the southern hemisphere the pair can be seen with the naked eye as a ] in ]. Based upon ] measurements, this system is located at a distance of about {{convert|39.3|ly|pc|abbr=off|lk=on|0}} from ]. Both stars are ]s that have characteristics similar to those of the ]. They belong to the ] of co-moving stars that share a common origin.


==Nomenclature== ==Nomenclature==
At a declination of −62°, the system is not visible from Britain's latitude of +53°, so it never received a ] in ]'s 1712 ''Historia Coelestis Britannica''. The ] for this star system, Zeta (ζ) Reticuli, originated in a 1756 star map by the French astronomer Abbé ].<ref name=ridpath1989/> Subsequently, the two stars received separate designations in the ], which was processed between 1859 and 1903, then in the ], published between 1918 and 1924.<ref name=IAU_NAO/> At a declination of −62°, the system is not visible from Britain's latitude of +53°, so it never received a ] in ]'s 1712 ''Historia Coelestis Britannica''. The ] for this star system, Zeta (ζ) Reticuli, originated in a 1756 star map by the French astronomer Abbé ].<ref name=ridpath1989/> Subsequently, the two stars received separate designations in the ], which was processed between 1859 and 1903, then in the ], published between 1918 and 1924.<ref name=IAU_NAO/>


== Characteristics == == Characteristics ==
]
The double star Zeta Reticuli is located in the western part of the small ] constellation, about 25] from the constellation's border with ]. In dark southern skies, the two stars can be viewed separately with the naked eye, or with a pair of binoculars.<ref name=mnassa68_11_242/> ζ<sup>1</sup> Reticuli has an ] of 5.52,<ref name=ibsh8_30/> placing it on the border between 5th and 6th magnitude stars. ζ<sup>2</sup> Reticuli is slightly brighter at magnitude 5.22.<ref name=ibsh8_30/> The double star ζ Reticuli is located in the western part of the small ] constellation, about 25] from the constellation's border with ]. In dark southern skies, the two stars can be viewed separately with the naked eye, or with a pair of binoculars.<ref name=mnassa68_11_242/> ζ<sup>1</sup> Reticuli has an ] of 5.52,<ref name=ibsh8_30/> placing it on the border between 5th- and 6th-magnitude stars. ζ<sup>2</sup> Reticuli is slightly brighter at magnitude 5.22.<ref name=ibsh8_30/>


The two stars are located at similar distances from the Sun and share the same motion through space,<ref name="aaa177"/> confirming that they are gravitationally bound and form a wide binary star system. They have an angular separation of 309.2&nbsp;]s (5.2 ]s);<ref name="apj687_1_566"/> far enough apart to appear as a close pair of separate stars to the naked eye under ]. The distance between the two stars is at least 3,750 ] (0.06 light-years, or almost a hundred times the average distance between ] and the Sun), so their orbital period is 170,000 years or more.<ref name=kaler_stars/> The two stars are located at similar distances from the Sun and share the same motion through space,<ref name="aaa177"/> confirming that they are gravitationally bound and form a wide binary star system. They have an angular separation of 309.2&nbsp;] (5.2 ]);<ref name="apj687_1_566"/> far enough apart to appear as a close pair of separate stars to the naked eye under ]. The distance between the two stars is at least {{Val|3750|fmt=commas|ul=AU}} (0.06 light-year, or almost a hundred times the average distance between ] and the Sun), so their orbital period is 170,000 years or more.<ref name=kaler_stars/>


Both stars share similar physical characteristics to the Sun,<ref name="aaa177" /> so they are considered ]s. Their ] is nearly identical to that of the Sun. ζ<sup>1</sup> has 96% of the ] and 84% of the ]. ζ<sup>2</sup> is slightly larger and more luminous than ζ<sup>1</sup>, with 99% of the Sun's mass and 88% of the Sun's radius.<ref name=apjss168/><ref name="cadars"/> The two stars are somewhat deficient in ], having only 60% of the proportion of elements other than hydrogen and helium as compared to the Sun.<ref name="aaa358" /><ref name=metal/> For reasons that remain uncertain, ζ<sup>1</sup> has an anomalously low abundance of ].<ref name=aaa425/> 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.<ref name=aa546_A113/> Both stars share similar physical characteristics to the Sun,<ref name="aaa177"/> so they are considered ]s. Their ] is nearly identical to that of the Sun. ζ<sup>1</sup> has 96% of the ] and 84% of the ]. ζ<sup>2</sup> is slightly larger and more luminous than ζ<sup>1</sup>, with 99% of the Sun's mass and 88% of the Sun's radius.<ref name=apjss168/><ref name="cadars"/> The two stars are somewhat deficient in ], having only 60% of the proportion of elements other than hydrogen and helium as compared to the Sun.<ref name="aaa358"/><ref name=metal/> For reasons that remain uncertain, ζ<sup>1</sup> has an anomalously low abundance of ].<ref name=aaa425/> 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.<ref name=aa546_A113/>


Both stars were considered unusual because they were thought to have had a lower ] than is normal for ] stars of their age and surface temperature. That is, they lie below the main sequence curve on the ] 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.<ref name="aaa358"/> Most stars will evolve above this curve as they age.<ref name="apj687_1_566"/> ζ<sup>1</sup> has an intermediate level of magnetic activity in its ]<ref name=aaa441_2/> with an erratic variability. ζ<sup>2</sup> is more sedate, showing a much lower level of activity with a 10-year ].<ref name=Flores2018/> Although the kinematics of this system suggest that they belong to a population of older stars, the properties of their stellar ]s suggests that they are only about 2 billion years old.<ref name=aaa384/> Both stars were considered unusual because they were thought to have had a lower ] than is normal for ]s of their age and surface temperature. That is, they lie below the main-sequence curve on the ] for newly formed stars. However, this was challenged, after using the much more accurate parallaxes from the '']'' catalogue (ESA, 1997), it was calculated that the stars actually have higher luminosities and so are shifted upwards, putting them in the main sequence.<ref name="aaa358"/> Most stars will evolve above this curve as they age.<ref name="apj687_1_566"/>


ζ<sup>1</sup> has an intermediate level of magnetic activity in its ]<ref name=aaa441_2/> with an erratic variability. A long-term activity cycle of ~4.2&nbsp;years has been tentatively identified.<ref name=Flores_et_al_2021/> ζ<sup>2</sup> is more sedate, showing a much lower level of activity<ref name=Flores2018/> with a ~7.9-year ], which may indicate it is in a ] state.<ref name=Flores_et_al_2021/> Although the kinematics of this system suggest that they belong to a population of older stars, the properties of their stellar ]s suggests that they are only about 2 billion years old.<ref name=aaa384/>
⚫ This star system belongs to the ] of stars that share a common motion through space, suggesting that they have a common origin. In the ], the {{nowrap|}} components of the ] for this system are equal to {{nowrap| km/s}} for ζ<sup>1</sup> and {{nowrap| km/s}} for ζ<sup>2</sup>.<ref name="aaa358" /> They are currently following an orbit through the ] galaxy that has an ] of 0.24. This orbit will carry the system as close as {{Convert|17.4|kly|kpc|abbr=on|sigfig=3|lk=on}} and as far as {{Convert|28.6|kly|kpc|sigfig=3|abbr=on}} from the ]. The ] of this orbit will carry the stars as much as {{Convert|1.3|kly|kpc|sigfig=1|abbr=on}} from the plane of the galactic disk.<ref name=cgssn09/> This likely puts them outside the ] population of stars.<ref name=apj687_1_566/>


⚫ This star system belongs to the ] of stars that share a common motion through space, suggesting that they have a common origin. In the ], the {{nowrap|}} components of the ] for this system are equal to {{nowrap| km/s}} for ζ<sup>1</sup> and {{nowrap| km/s}} for ζ<sup>2</sup>.<ref name="aaa358"/> They are currently following an orbit through the ] ] that has an ] of 0.24. This orbit will carry the system as close as {{cvt|17.4|kly|kpc|3|lk=on}} and as far as {{cvt|28.6|kly|kpc|3}} from the ]. The ] of this orbit will carry the stars as much as {{cvt|1.3|kly|kpc|1}} from the plane of the galactic disk.<ref name=cgssn09/> This likely puts them outside the ] population of stars.<ref name=apj687_1_566/>
== See also ==

* ] in the story of the purported ] by ]s (])
==Alleged debris disk==
* ]
Zeta Reticuli has no known ]s. In 2002, ζ<sup>1</sup> was examined at an infrared wavelength of 25&nbsp;μm, but no indication of an ] was found.<ref name=aaa387/>
* ]

In 2007, the ] was used to find an apparent infrared excess at a wavelength of 70&nbsp;μm around ζ<sup>2</sup>. This radiation was attributed to emission by a ] with a mean temperature of {{cvt|150|K|C}}, theorized to be orbiting the host star at a distance of 4.3&nbsp;].<ref name=apj674_2/> In 2010, the ], a telescope with a comparatively superior spatial resolution and, unlike Spitzer, able to resolve radiation excesses beyond the wavelength of 70&nbsp;μm, determined the infrared excess as coming from a two-lobed structure that looked like a debris disk seen edge-on. This debris disk interpreted as an analogy to the ] with a ] of 100&nbsp;AU and a temperature of 30–40 K.<ref name=aaa518/>

However, observations with ] from October and November 2017 revealed that the structure observed by Herschel shows no common proper motion with Zeta Reticuli. In these observations, no significant flux has been detected around ζ<sup>2</sup>, showing that the alleged debris disk is not real, but rather a case of background confusion. The observations demonstrate the need to follow up ''Herschel'' observations of debris disks.<ref name=Faramaz2018/>

==In UFO folklore==
{{main|UFO conspiracy theories}}
The 1966 bestseller ''The Interrupted Journey'' about ] reproduced a "star map" drawn by Betty, allegedly based on one she saw aboard an alien spaceship. Based on the map, a fan of the book named Marjorie Fish speculated that the aliens might originate from Zeta Reticuli. By 1974, the Hill case was referred to as the Zeta Reticuli incident.<ref>{{cite journal |last1=Terence Dickinso |title=The Zeta Reticuli incident |journal=Astronomy |date=December 1974 |url=https://astronomy.com/issues/1974/december-1974 |access-date=October 10, 2021 |archive-date=October 10, 2021 |archive-url=https://web.archive.org/web/20211010072434/https://astronomy.com/issues/1974/december-1974 |url-status=live }}. See also , Halloween, 2016.</ref> In a 1980 episode of '']'' , ] demonstrated that the Hill map bore no resemblance to the real-life map.

In the 1988 broadcast '']'', alleged government informant "Falcon" (Richard Doty) spread tales of ], a hidden cabal that has made a secret treaty with gray aliens from Zeta Reticuli who operate out of ]. Alleged Area 51 worker ] similarly spread tales of aliens from Zeta Reticuli.


== References == == References ==
{{Reflist|30em|refs= {{Reflist|30em|refs=

<ref name=Fuhrmann>{{cite journal|bibcode=2015ApJ...809..107F|doi=10.1088/0004-637X/809/1/107|title=Multiplicity Among F-Type Stars. II|journal=The Astrophysical Journal|volume=809|pages=107|year=2015|last1=Fuhrmann|first1=K.|last2=Chini|first2=R.|issue=1 |s2cid=126218052 |doi-access=}}</ref>


<ref name=GaiaDR2a>{{Cite DR2|4722111590409480064}}</ref> <ref name=GaiaDR2a>{{Cite DR2|4722111590409480064}}</ref>
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}}</ref> }}</ref>


<ref name=adibekyan>{{cite journal|bibcode=2016A&A...591A..34A|title=Ζ<SUP>2</SUP> Reticuli, its debris disk, and its lonely stellar companion ζ<SUP>1</SUP> Ret. Different T<SUB>c</SUB> trends for different spectra|journal=Astronomy and Astrophysics|volume=591|pages=A34|last1=Adibekyan|first1=V.|last2=Delgado-Mena|first2=E.|last3=Figueira|first3=P.|last4=Sousa|first4=S. G.|last5=Santos|first5=N. C.|last6=Faria|first6=J. P.|last7=González Hernández|first7=J. I.|last8=Israelian|first8=G.|last9=Harutyunyan|first9=G.|last10=Suárez-Andrés|first10=L.|last11=Hakobyan|first11=A. A.|year=2016|arxiv=1605.01918|doi=10.1051/0004-6361/201628453|s2cid=119313511}}</ref> <ref name=adibekyan>{{cite journal|bibcode=2016A&A...591A..34A|title=Ζ<SUP>2</SUP> Reticuli, its debris disk, and its lonely stellar companion ζ<SUP>1</SUP> Ret. Different T<SUB>c</SUB> trends for different spectra|journal=Astronomy and Astrophysics|volume=591|pages=A34|last1=Adibekyan|first1=V.|last2=Delgado-Mena|first2=E.|last3=Figueira|first3=P.|last4=Sousa|first4=S. G.|last5=Santos|first5=N. C.|last6=Faria|first6=J. P.|last7=González Hernández|first7=J. I.|last8=Israelian|first8=G.|last9=Harutyunyan|first9=G.|last10=Suárez-Andrés|first10=L.|last11=Hakobyan|first11=A. A. | display-authors=1 |year=2016|arxiv=1605.01918|doi=10.1051/0004-6361/201628453|s2cid=119313511}}</ref>


<ref name=eiroa>{{cite journal|bibcode=2013A&A...555A..11E|title=DUst around NEarby Stars. The survey observational results|journal=Astronomy and Astrophysics|volume=555|pages=A11|last1=Eiroa|first1=C.|last2=Marshall|first2=J. P.|last3=Mora|first3=A.|last4=Montesinos|first4=B.|last5=Absil|first5=O.|last6=Augereau|first6=J. Ch.|last7=Bayo|first7=A.|last8=Bryden|first8=G.|last9=Danchi|first9=W.|last10=Del Burgo|first10=C.|last11=Ertel|first11=S.|last12=Fridlund|first12=M.|last13=Heras|first13=A. M.|last14=Krivov|first14=A. V.|last15=Launhardt|first15=R.|last16=Liseau|first16=R.|last17=Löhne|first17=T.|last18=Maldonado|first18=J.|last19=Pilbratt|first19=G. L.|last20=Roberge|first20=A.|last21=Rodmann|first21=J.|last22=Sanz-Forcada|first22=J.|last23=Solano|first23=E.|last24=Stapelfeldt|first24=K.|last25=Thébault|first25=P.|last26=Wolf|first26=S.|last27=Ardila|first27=D.|last28=Arévalo|first28=M.|last29=Beichmann|first29=C.|last30=Faramaz|first30=V.|display-authors=29|year=2013|arxiv=1305.0155|doi=10.1051/0004-6361/201321050|s2cid=377244}}</ref> <ref name=eiroa>{{cite journal|bibcode=2013A&A...555A..11E|title=DUst around NEarby Stars. The survey observational results|journal=Astronomy and Astrophysics|volume=555|pages=A11|last1=Eiroa|first1=C.|last2=Marshall|first2=J. P.|last3=Mora|first3=A.|last4=Montesinos|first4=B.|last5=Absil|first5=O.|last6=Augereau|first6=J. Ch.|last7=Bayo|first7=A.|last8=Bryden|first8=G.|last9=Danchi|first9=W.|last10=Del Burgo|first10=C.|last11=Ertel|first11=S.|last12=Fridlund|first12=M.|last13=Heras|first13=A. M.|last14=Krivov|first14=A. V.|last15=Launhardt|first15=R.|last16=Liseau|first16=R.|last17=Löhne|first17=T.|last18=Maldonado|first18=J.|last19=Pilbratt|first19=G. L.|last20=Roberge|first20=A.|last21=Rodmann|first21=J.|last22=Sanz-Forcada|first22=J.|last23=Solano|first23=E.|last24=Stapelfeldt|first24=K.|last25=Thébault|first25=P.|last26=Wolf|first26=S.|last27=Ardila|first27=D.|last28=Arévalo|first28=M.|last29=Beichmann|first29=C.|last30=Faramaz|first30=V.|display-authors=1|year=2013|arxiv=1305.0155|doi=10.1051/0004-6361/201321050|s2cid=377244}}</ref>


<ref name=aaa474_2_653>{{citation | last1=van Leeuwen | first1=F. | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 |date=November 2007 | pages=653–664 | doi=10.1051/0004-6361:20078357 | bibcode=2007A&A...474..653V | arxiv=0708.1752 | s2cid=18759600 }}</ref> <ref name=aaa474_2_653>{{citation | last1=van Leeuwen | first1=F. | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 |date=November 2007 | pages=653–664 | doi=10.1051/0004-6361:20078357 | bibcode=2007A&A...474..653V | arxiv=0708.1752 | s2cid=18759600 }}</ref>
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<ref name="cadars">{{cite journal | display-authors=1 | last1=Pasinetti Fracassini | first1=L. E. | last2=Pastori | first2=L. | last3=Covino | first3=S. | last4=Pozzi | first4=A. | title=Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics | journal=Astronomy and Astrophysics | volume=367 | issue=2 | pages=521–524 |date=February 2001 | doi=10.1051/0004-6361:20000451 | bibcode=2001A&A...367..521P|arxiv = astro-ph/0012289 | s2cid=425754 }} Note: using the method of Perrin and Karoji (1987).</ref> <ref name="cadars">{{cite journal | display-authors=1 | last1=Pasinetti Fracassini | first1=L. E. | last2=Pastori | first2=L. | last3=Covino | first3=S. | last4=Pozzi | first4=A. | title=Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics | journal=Astronomy and Astrophysics | volume=367 | issue=2 | pages=521–524 |date=February 2001 | doi=10.1051/0004-6361:20000451 | bibcode=2001A&A...367..521P|arxiv = astro-ph/0012289 | s2cid=425754 }} Note: using the method of Perrin and Karoji (1987).</ref>


<ref name="aaa358">{{cite journal | last1=del Peloso | first1=E. F. | last2=da Silva | first2=L. | last3=Porto de Mello | first3=G. F. | title=zeta<sup>1</sup> and zeta<sup>2</sup> Reticuli and the existence of the zeta Herculis group | journal=Astronomy and Astrophysics | volume=358 | pages=233–241 |date=June 2000 | bibcode=2000A&A...358..233D }}</ref> <ref name="aaa358">{{cite journal | last1=del Peloso | first1=E. F. | last2=da Silva | first2=L. | last3=Porto de Mello | first3=G. F. | display-authors=1 | title=zeta<sup>1</sup> and zeta<sup>2</sup> Reticuli and the existence of the zeta Herculis group | journal=Astronomy and Astrophysics | volume=358 | pages=233–241 |date=June 2000 | bibcode=2000A&A...358..233D }}</ref>


<ref name="apj687">{{cite journal | last1=Mamajek | first1=Eric E. | last2=Hillenbrand | first2=Lynne A. | title=Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics | journal=The Astrophysical Journal | volume=687 | issue=2 | pages=1264–1293 |date=November 2008 | doi=10.1086/591785 | bibcode=2008ApJ...687.1264M |arxiv = 0807.1686 | s2cid=27151456 }}</ref> <ref name="apj687">{{cite journal | last1=Mamajek | first1=Eric E. | last2=Hillenbrand | first2=Lynne A. | title=Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics | journal=The Astrophysical Journal | volume=687 | issue=2 | pages=1264–1293 |date=November 2008 | doi=10.1086/591785 | bibcode=2008ApJ...687.1264M |arxiv = 0807.1686 | s2cid=27151456 }}</ref>


<ref name=apj687_1_566>{{cite journal
<ref name="apj687_1_566">{{cite journal | last1=Makarov | first1=V. V. | last2=Zacharias | first2=N. | last3=Hennessy | first3=G. S. | title=Common Proper Motion Companions to Nearby Stars: Ages and Evolution | journal=The Astrophysical Journal | volume=687 | issue=1 | pages=566–578 |date=November 2008 | doi=10.1086/591638 | bibcode=2008ApJ...687..566M |arxiv = 0808.3414 | s2cid=17811620 }}</ref>
| title=Common Proper Motion Companions to Nearby Stars: Ages and Evolution
| last1=Makarov | first1=V. V. | last2=Zacharias | first2=N.
| last3=Hennessy | first3=G. S. | display-authors=1
| journal=The Astrophysical Journal
| volume=687 | issue=1 | pages=566–578 | date=November 2008
| doi=10.1086/591638 | bibcode=2008ApJ...687..566M
| arxiv=0808.3414 | s2cid=17811620 }}</ref>


<ref name=metal>A ] of −0.22 indicates that they have the following proportion of metals compared to the Sun: 10<sup>−0.22</sup> = 0.603, or 60%.</ref> <ref name=metal>A ] of −0.22 indicates that they have the following proportion of metals compared to the Sun: 10<sup>−0.22</sup> = 0.603, or 60%.</ref>


<ref name=aaa441_2>{{cite journal | last1=Vieytes | first1=M. | last2=Mauas | first2=P. | last3=Cincunegui | first3=C. | title=Chromospheric models of solar analogues with different activity levels | journal=Astronomy and Astrophysics | volume=441 | issue=2 |date=October 2005 | pages=701–709 | doi=10.1051/0004-6361:20052651 | bibcode=2005A&A...441..701V | doi-access=free }}</ref> <ref name=aaa441_2>{{cite journal | last1=Vieytes | first1=M. | last2=Mauas | first2=P. | last3=Cincunegui | first3=C. | display-authors=1 | title=Chromospheric models of solar analogues with different activity levels | journal=Astronomy and Astrophysics | volume=441 | issue=2 |date=October 2005 | pages=701–709 | doi=10.1051/0004-6361:20052651 | bibcode=2005A&A...441..701V | doi-access=free | hdl=11336/22051 | hdl-access=free }}</ref>


<ref name=aaa384>{{cite journal | last1=Rocha-Pinto | first1=Helio J. | last2=Maciel | first2=Walter J. | last3=Castilho | first3=Bruno V. | title=Chromospherically young, kinematically old stars | journal=Astronomy and Astrophysics | volume=384 | issue=3 | pages=912–924 |date=March 2002 | doi=10.1051/0004-6361:20011815 | bibcode=2002A&A...384..912R |arxiv = astro-ph/0112452 | s2cid=16982360 }}</ref> <ref name=aaa384>{{cite journal | last1=Rocha-Pinto | first1=Helio J. | last2=Maciel | first2=Walter J. | last3=Castilho | first3=Bruno V. | display-authors=1 | title=Chromospherically young, kinematically old stars | journal=Astronomy and Astrophysics | volume=384 | issue=3 | pages=912–924 |date=March 2002 | doi=10.1051/0004-6361:20011815 | bibcode=2002A&A...384..912R |arxiv = astro-ph/0112452 | s2cid=16982360 }}</ref>

<ref name=zetatalk>{{cite web | title=Life on Zeta Reticuli? | work=ZetaTalk | url=http://www.zetatalk.com/usenet/use90200.htm | access-date=2010-02-10 }}</ref>


<ref name="aaa177">{{cite journal | last1=da Silva | first1=L. | last2=Foy | first2=R. | title=Zeta-1 and Zeta-2 RETICULI - A puzzling solar-type twin system | journal=Astronomy and Astrophysics | volume=177 | issue=1–2 |date=May 1987 | pages=204–216 | bibcode=1987A&A...177..204D }}</ref> <ref name="aaa177">{{cite journal | last1=da Silva | first1=L. | last2=Foy | first2=R. | title=Zeta-1 and Zeta-2 RETICULI - A puzzling solar-type twin system | journal=Astronomy and Astrophysics | volume=177 | issue=1–2 |date=May 1987 | pages=204–216 | bibcode=1987A&A...177..204D }}</ref>
Line 150: Line 168:
<ref name=aaa387>{{cite journal | display-authors=1 | last1=Laureijs | first1=R. J. | last2=Jourdain de Muizon | first2=M. | last3=Leech | first3=K. | last4=Siebenmorgen | first4=R. | last5=Dominik | first5=C. | last6=Habing | first6=H. J. | last7=Trams | first7=N. | last8=Kessler | first8=M. F. | title=A 25 micron search for Vega-like disks around main-sequence stars with ISO | journal=Astronomy and Astrophysics | pages=285–293 |date=May 2002 | issue=1 | doi=10.1051/0004-6361:20020366 | bibcode=2002A&A...387..285L | volume=387 | url=https://pure.uva.nl/ws/files/3745204/19625_102289y.pdf | access-date=2018-10-24 | hdl=1887/7333 | doi-access=free }}</ref> <ref name=aaa387>{{cite journal | display-authors=1 | last1=Laureijs | first1=R. J. | last2=Jourdain de Muizon | first2=M. | last3=Leech | first3=K. | last4=Siebenmorgen | first4=R. | last5=Dominik | first5=C. | last6=Habing | first6=H. J. | last7=Trams | first7=N. | last8=Kessler | first8=M. F. | title=A 25 micron search for Vega-like disks around main-sequence stars with ISO | journal=Astronomy and Astrophysics | pages=285–293 |date=May 2002 | issue=1 | doi=10.1051/0004-6361:20020366 | bibcode=2002A&A...387..285L | volume=387 | url=https://pure.uva.nl/ws/files/3745204/19625_102289y.pdf | access-date=2018-10-24 | hdl=1887/7333 | doi-access=free }}</ref>


<ref name=cgssn09>{{cite journal | last1=Holmberg | first1=J. | last2=Nordström | first2=B. | last3=Andersen | first3=J. | title=The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics | volume=501 | issue=3 |date=July 2009 | pages=941–947 | doi=10.1051/0004-6361/200811191 | journal=Astronomy and Astrophysics | bibcode=2009A&A...501..941H|arxiv = 0811.3982 | s2cid=118577511 }}</ref> <ref name=cgssn09>{{cite journal | last1=Holmberg | first1=J. | last2=Nordström | first2=B. | last3=Andersen | first3=J. | display-authors=1 | title=The Geneva-Copenhagen survey of the solar neighbourhood. III. Improved distances, ages, and kinematics | volume=501 | issue=3 |date=July 2009 | pages=941–947 | doi=10.1051/0004-6361/200811191 | journal=Astronomy and Astrophysics | bibcode=2009A&A...501..941H|arxiv = 0811.3982 | s2cid=118577511 }}</ref>


<ref name=apj674_2>{{cite journal | display-authors=1 | last1=Trilling | first1=D. E. | last2=Bryden | first2=G. | last3=Beichman | first3=C. A. | last4=Rieke | first4=G. H. | last5=Su | first5=K. Y. L. | last6=Stansberry | first6=J. A. | last7=Blaylock | first7=M. | last8=Stapelfeldt | first8=K. R. | last9=Beeman | first9=J. W. | title=Debris Disks around Sun-like Stars | journal=The Astrophysical Journal | volume=674 | issue=2 | pages=1086–1105 |date=February 2008 | doi=10.1086/525514 | bibcode=2008ApJ...674.1086T |arxiv = 0710.5498 | s2cid=54940779 }} See table 6.</ref> <ref name=apj674_2>{{cite journal | display-authors=1 | last1=Trilling | first1=D. E. | last2=Bryden | first2=G. | last3=Beichman | first3=C. A. | last4=Rieke | first4=G. H. | last5=Su | first5=K. Y. L. | last6=Stansberry | first6=J. A. | last7=Blaylock | first7=M. | last8=Stapelfeldt | first8=K. R. | last9=Beeman | first9=J. W. | title=Debris Disks around Sun-like Stars | journal=The Astrophysical Journal | volume=674 | issue=2 | pages=1086–1105 |date=February 2008 | doi=10.1086/525514 | bibcode=2008ApJ...674.1086T |arxiv = 0710.5498 | s2cid=54940779 }} See table 6.</ref>
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<ref name=aaa425>{{cite journal | display-authors=1 | last1=Santos | first1=N. C. | last2=Israelian | first2=G. | last3=Randich | first3=S. | last4=García López | first4=R. J. | last5=Rebolo | first5=R. | title=Beryllium anomalies in solar-type field stars | journal=Astronomy and Astrophysics | volume=425 | issue=3 | pages=1013–1027 |date=October 2004 | doi=10.1051/0004-6361:20040510 | bibcode=2004A&A...425.1013S |arxiv = astro-ph/0408109 | s2cid=17279966 }}</ref> <ref name=aaa425>{{cite journal | display-authors=1 | last1=Santos | first1=N. C. | last2=Israelian | first2=G. | last3=Randich | first3=S. | last4=García López | first4=R. J. | last5=Rebolo | first5=R. | title=Beryllium anomalies in solar-type field stars | journal=Astronomy and Astrophysics | volume=425 | issue=3 | pages=1013–1027 |date=October 2004 | doi=10.1051/0004-6361:20040510 | bibcode=2004A&A...425.1013S |arxiv = astro-ph/0408109 | s2cid=17279966 }}</ref>

<ref name=apj687_1_566>{{cite journal | last1=Makarov | first1=V. V. | last2=Zacharias | first2=N. | last3=Hennessy | first3=G. S. | title=Common Proper Motion Companions to Nearby Stars: Ages and Evolution | journal=The Astrophysical Journal | volume=687 | issue=1 | pages=566–578 |date=November 2008 | doi=10.1086/591638 | bibcode=2008ApJ...687..566M |arxiv = 0808.3414 | s2cid=17811620 }}</ref>


<ref name=aaa518>{{cite journal | display-authors=1 | last1=Eiroa | first1=C. | last2=Fedele | first2=D. | last3=Maldonado | first3=J. | last4=González-García | first4=B. M. | last5=Rodmann | first5=J. | last6=Heras | first6=A. M. | last7=Pilbratt | first7=G. L. | last8=Augereau | first8=J.-Ch. | last9=Mora | first9=A. | title=Cold DUst around NEarby Stars (DUNES). First results. A resolved exo-Kuiper belt around the solar-like star ζ<sup>2</sup> Ret | journal=Astronomy and Astrophysics | volume=518 | pages=L131 |date=July 2010 | doi=10.1051/0004-6361/201014594 | bibcode=2010A&A...518L.131E |arxiv = 1005.3151 | s2cid=1662394 }}</ref> <ref name=aaa518>{{cite journal | display-authors=1 | last1=Eiroa | first1=C. | last2=Fedele | first2=D. | last3=Maldonado | first3=J. | last4=González-García | first4=B. M. | last5=Rodmann | first5=J. | last6=Heras | first6=A. M. | last7=Pilbratt | first7=G. L. | last8=Augereau | first8=J.-Ch. | last9=Mora | first9=A. | title=Cold DUst around NEarby Stars (DUNES). First results. A resolved exo-Kuiper belt around the solar-like star ζ<sup>2</sup> Ret | journal=Astronomy and Astrophysics | volume=518 | pages=L131 |date=July 2010 | doi=10.1051/0004-6361/201014594 | bibcode=2010A&A...518L.131E |arxiv = 1005.3151 | s2cid=1662394 }}</ref>
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<ref name=ridpath1989>{{cite book | first1=Ian | last1=Ridpath | title=Star tales | publisher=James Clarke & Co. | date=1989 | isbn=0-7188-2695-7 | page=11 | url=https://books.google.com/books?id=gFrdcTdeVaEC }}</ref> <ref name=ridpath1989>{{cite book | first1=Ian | last1=Ridpath | title=Star tales | publisher=James Clarke & Co. | date=1989 | isbn=0-7188-2695-7 | page=11 | url=https://books.google.com/books?id=gFrdcTdeVaEC }}</ref>


<ref name=ibsh8_30>{{cite journal | last1=Feinstein | first1=A. | title=Photoelectric observations of Southern late-type stars | journal=Informational Bulletin of the Southern Hemisphere | volume=8 | page=30 | date=1966 | bibcode=1966IBSH....8...30F }}</ref> <ref name=ibsh8_30>{{cite journal | last=Feinstein | first=A. | author-link=Alejandro Feinstein | title=Photoelectric observations of Southern late-type stars | journal=Informational Bulletin of the Southern Hemisphere | volume=8 | page=30 | date=1966 | bibcode=1966IBSH....8...30F }}</ref>


<ref name=rgcrv>{{cite journal | last1=Evans | first1=D. S. | date=June 20–24, 1966 | editor1-last=Batten | editor1-first=Alan Henry | editor2-last=Heard | editor2-first=John Frederick | title=The Revision of the General Catalogue of Radial Velocities | journal=Determination of Radial Velocities and Their Applications | volume=30 | pages=57 | book-title=Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30 | location=University of Toronto | publisher=International Astronomical Union | bibcode=1967IAUS...30...57E }}</ref> <ref name=rgcrv>{{cite journal | last=Evans | first=D. S. | author-link=David Stanley Evans | date=20–24 June 1966 | editor1-last=Batten | editor1-first=Alan Henry | editor2-last=Heard | editor2-first=John Frederick | title=The Revision of the General Catalogue of Radial Velocities | volume=30 | pages=57 | journal=Determination of Radial Velocities and Their Applications, Proceedings from IAU Symposium No. 30 | location=University of Toronto | publisher=International Astronomical Union | bibcode=1967IAUS...30...57E }}</ref>


<ref name=kaler_stars>{{cite web | first1=James B. | last1=Kaler | work=Stars | title=ZETA RET (Zeta Reticuli) | publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/zetaret.html | access-date=2011-11-16 }}</ref> <ref name=kaler_stars>{{cite web | first=James B. | last=Kaler | author-link=James B. Kaler | work=Stars | title=ZETA RET (Zeta Reticuli) | publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/zetaret.html | access-date=2011-11-16 }}</ref>


<ref name="Faramaz2018">{{cite journal <ref name="Faramaz2018">{{cite journal
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| date=November 2018 | date=November 2018
| doi=10.1093/mnras/sty2304 | doi=10.1093/mnras/sty2304
|arxiv = 1809.00645 }}</ref> | doi-access=free |arxiv = 1809.00645 }}</ref>


<ref name=aa546_A113>{{cite journal <ref name=aa546_A113>{{cite journal
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| journal=Monthly Notices of the Royal Astronomical Society | journal=Monthly Notices of the Royal Astronomical Society
| volume=476 | issue=2 | pages=2751–2759 | date=May 2018 | volume=476 | issue=2 | pages=2751–2759 | date=May 2018
| doi=10.1093/mnras/sty234 | arxiv=1801.08104 | doi=10.1093/mnras/sty234 | doi-access=free | arxiv=1801.08104
| bibcode=2018MNRAS.476.2751F }}</ref> | bibcode=2018MNRAS.476.2751F }}</ref>

<ref name=Flores_et_al_2021>{{cite journal
| title=Detecting prolonged activity minima in binary stars. The case of ζ<sub>2</sub> Reticuli
| last1=Flores | first1=M. | last2=Jaque Arancibia | first2=M.
| last3=Ibañez Bustos | first3=R. V. | last4=Buccino | first4=A. P.
| last5=Yana Galarza | first5=J. | last6=Nuñez | first6=N. E.
| last7=Miquelarena | first7=P. | last8=Alacoria | first8=J.
| last9=Saffe | first9=C. | last10=Mauas | first10=P. J. D.
| display-authors=1 | journal=Astronomy & Astrophysics
| volume=645 | id=L6 | pages=5 | date=January 2021
| doi=10.1051/0004-6361/202039902 | arxiv=2012.08983
| bibcode=2021A&A...645L...6F | s2cid=229219969 }}</ref>


}} <!-- End: refs= --> }} <!-- End: refs= -->

== External links ==
* {{cite web |url=http://www.solstation.com/stars2/zeta-ret.htm |title=Zeta Reticuli |access-date=2008-08-31 |work=SolStation }}
* {{cite web |url=http://www.stellar-database.com/Scripts/search_star.exe?ID=23900 |title=Zeta(1) Reticuli |access-date=2008-08-31 |work=The Internet Stellar Database }}
* {{cite web |url=http://www.stellar-database.com/Scripts/search_star.exe?ID=24100 |title=Zeta(2) Reticuli |access-date=2008-08-31 |work=The Internet Stellar Database }}
* {{cite web |url=http://hatirlabeni.net/index.php?option=com_content&view=article&id=401:zeta-reticulideki-uzayllar&catid=25:proje&Itemid=53 |title=Zeta(3) Reticuli |access-date=2008-08-31 |work=Hatirla Beni Belgesel |url-status=dead |archive-url=https://web.archive.org/web/20110723142621/http://hatirlabeni.net/index.php?option=com_content&view=article&id=401:zeta-reticulideki-uzayllar&catid=25:proje&Itemid=53 |archive-date=2011-07-23 }}


{{Stars of Reticulum}} {{Stars of Reticulum}}
{{Portal bar|Astronomy|Stars|Spaceflight|Outer space|Solar System}} {{Portal bar|Astronomy|Stars|Spaceflight|Outer space|Solar System}}

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{{DEFAULTSORT:Zeta Reticuli}} {{DEFAULTSORT:Zeta Reticuli}}
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Latest revision as of 00:25, 19 December 2024

Binary star system in the constellation Reticulum
ζ Reticuli
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
Distance39.27 ± 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
Distance39.29 ± 0.09 ly
(12.05 ± 0.03 pc)
Absolute magnitude (MV)4.83
Absolute bolometric
magnitude (Mbol)		4.79±0.03
Details
ζ Ret
Mass0.94 M☉
Radius0.90±0.03 R☉
Luminosity0.761 L☉
Surface gravity (log g)4.5±0.1 cgs
Temperature5,729±60 K
Metallicity −0.25±0.06 dex
Rotational velocity (v sin i)2.2±0.8 km/s
Age1.5–3.0 Gyr
ζ Ret
Mass0.96 M☉
Radius0.98±0.03 R☉
Luminosity0.972 L☉
Surface gravity (log g)4.43±0.10 cgs
Temperature5,861±12 K
Metallicity −0.26±0.03 dex
Rotational velocity (v sin i)1.74 km/s
Age1.5–3.0 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
SIMBADζ 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 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 co-moving 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

Zeta Reticuli A and B

The double star ζ 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 arcseconds (5.2 arcminutes); 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-year, 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, putting them in 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. A long-term activity cycle of ~4.2 years has been tentatively identified. ζ is more sedate, showing a much lower level of activity with a ~7.9-year cycle, which may indicate it is in a Maunder Minimum state. 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 (5.335 kpc) and as far as 28.6 kly (8.769 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.

Alleged debris disk

Zeta Reticuli has no known planets. In 2002, ζ was examined at an infrared wavelength of 25 μm, but no indication of an excess of infrared radiation was found.

In 2007, the Spitzer Space Telescope was used to find an apparent infrared excess at a wavelength of 70 μm around ζ. This radiation was attributed to emission by a debris disk with a mean temperature of 150 K (−123 °C), theorized to be orbiting the host star at a distance of 4.3 AU. In 2010, the Herschel Space Observatory, a telescope with a comparatively superior spatial resolution and, unlike Spitzer, able to resolve radiation excesses beyond the wavelength of 70 μm, determined the infrared excess as coming from a two-lobed structure that looked like a debris disk seen edge-on. This debris disk interpreted as an analogy to the Kuiper belt with a semi-major axis of 100 AU and a temperature of 30–40 K.

However, observations with ALMA from October and November 2017 revealed that the structure observed by Herschel shows no common proper motion with Zeta Reticuli. In these observations, no significant flux has been detected around ζ, showing that the alleged debris disk is not real, but rather a case of background confusion. The observations demonstrate the need to follow up Herschel observations of debris disks.

In UFO folklore

Main article: UFO conspiracy theories

The 1966 bestseller The Interrupted Journey about Barney and Betty Hill reproduced a "star map" drawn by Betty, allegedly based on one she saw aboard an alien spaceship. Based on the map, a fan of the book named Marjorie Fish speculated that the aliens might originate from Zeta Reticuli. By 1974, the Hill case was referred to as the Zeta Reticuli incident. In a 1980 episode of Cosmos , Carl Sagan demonstrated that the Hill map bore no resemblance to the real-life map.

In the 1988 broadcast UFO Cover Up? Live, alleged government informant "Falcon" (Richard Doty) spread tales of Majestic 12, a hidden cabal that has made a secret treaty with gray aliens from Zeta Reticuli who operate out of Area 51. Alleged Area 51 worker Bob Lazar similarly spread tales of aliens from Zeta Reticuli.

References

  1. ^ 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.
  2. ^ Feinstein, A. (1966). "Photoelectric observations of Southern late-type stars". Informational Bulletin of the Southern Hemisphere. 8: 30. Bibcode:1966IBSH....8...30F.
  3. ^ 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
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  21. A metallicity of −0.22 indicates that they have the following proportion of metals compared to the Sun: 10 = 0.603, or 60%.
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  25. 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.
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  29. Eiroa, C.; et al. (July 2010). "Cold DUst around NEarby Stars (DUNES). First results. A resolved exo-Kuiper belt around the solar-like star ζ Ret". Astronomy and Astrophysics. 518: L131. arXiv:1005.3151. Bibcode:2010A&A...518L.131E. doi:10.1051/0004-6361/201014594. S2CID 1662394.
  30. Faramaz, V.; et al. (November 2018). "Is there really a debris disc around zeta2 Reticuli?". Monthly Notices of the Royal Astronomical Society. 481: 44–48. arXiv:1809.00645. doi:10.1093/mnras/sty2304.
  31. Terence Dickinso (December 1974). "The Zeta Reticuli incident". Astronomy. Archived from the original on October 10, 2021. Retrieved October 10, 2021.. See also The Zeta Reticuli (or Ridiculi) Incident, Halloween, 2016.
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