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{{Short description|Star in the constellation Ara}}
{{Starbox begin
{{Use dmy dates|date=April 2021}}
| name = Mu Arae
{{Starbox begin
}}
|name=Mu Arae / Cervantes}}
{{Starbox image
{{Starbox observe
| image = ]
| caption = Mu Arae | epoch = J2000.0
}}
{{Starbox observe
| epoch = ]
| constell = ] | constell = ]
| ra = 17<sup>h</sup> 44<sup>m</sup> 08.7<sup>s</sup> | ra = {{RA|17|44|08.70314}}<ref name=GaiaDR3/>
| dec = −51° 50' 03" | dec = {{DEC|-51|50|02.5916}}<ref name=GaiaDR3/>
| appmag_v = +5.12 | appmag_v = 5.15<ref name="Benedict2022"/>
}} }}
{{Starbox character {{Starbox character
| class = G3IV&ndash;V | class = G3IV–V<ref name=aj132_1_161/>
| appmag_1_passband = V
| b-v = 0.694
| appmag_1 = {{val|5.15|0.01}}<ref name="Benedict2022"/>
| u-b = ?
| appmag_2_passband = G
| variable = none
| appmag_2 = {{val|4.943|0.003}}<ref name=GaiaDR3/>
}}
| appmag_3_passband = K
{{Starbox astrometry
| appmag_3 = {{val|3.68|0.25}}<ref name="Benedict2022"/>
| radial_v = −9.0
| b-v = +0.70<ref name=ibsh8_30/>
| prop_mo_ra = −15.06
| u-b = +0.24<ref name=ibsh8_30/>
| prop_mo_dec = −191.17
| parallax = 65.46 | r-i =
| v-k = {{val|1.47|0.25}}<ref name="Benedict2022"/>
| p_error = 0.80
| absmag_v = +4.28 | variable =
}} }}
{{Starbox detail {{Starbox astrometry
| radial_v = {{val|-9.54|0.13}}<ref name=GaiaDR3/>
| age = 6410 million
| prop_mo_ra = {{val|-15.034|0.084}}
| metal = 210 ± 20%
| prop_mo_dec = {{val|-190.901|0.065}}
| mass = 1.10 ± 0.05
| pm_footnote = <ref name=GaiaDR3/>
| radius = 1.3150 ± 0.0190
| rotation = 31 days | parallax = 64.0853
| luminosity = 1.75 ± 0.10 | p_error = 0.0904
| parallax_footnote = <ref name=GaiaDR3/>
| temperature = 5813 ± 40
| absmag_v = +4.17<ref name=Anderson2012/>
}}
}}
{{Starbox catalog
{{Starbox detail
| names = ] 6585, ] 160691, ] 691, ]-51°11094, ] 662, ] 86796, ] 244981, GC 24024
| age_gyr = {{val|6.34|0.40}}<ref name="soriano2009">{{cite journal|title=New seismic analysis of the exoplanet-host star Mu Arae|arxiv=0903.5475 |year=2009 |last1=Soriano | first1=M. |last2=Vauclair |first2=S. |doi=10.1051/0004-6361/200911862 |volume=513 |journal=Astronomy and Astrophysics |page=A49 |bibcode=2010A&A...513A..49S|s2cid=5688996 }}</ref>
}}
| metal = {{val|200|5|s=%}}<ref name="soriano2009" /><ref group="note">From = 0.30 ± 0.01</ref>
{{Starbox end}}
| metal_fe = {{val|0.30|0.01}}<ref name="soriano2009" />
| mass = {{val|1.10|0.01}}<ref name="soriano2009" />
| radius = {{val|1.36|0.01}}<ref name="soriano2009" />
| rotation =
| rotational_velocity = {{val|3.1|0.5}}<ref name="Benedict2022"/>
| gravity = {{val|4.2|0.1}}<ref name="Benedict2022"/>
| luminosity = {{val|1.90|0.10}}<ref name="soriano2009" />
| temperature = {{val|5820|40|fmt=commas}}<ref name="soriano2009" />
}}
{{Starbox catalog
| names = Cervantes, ]−51°11094, ]&nbsp;662, ]&nbsp;24024, ]&nbsp;691, ]&nbsp;160691, ]&nbsp;86796, ]&nbsp;6585, ]&nbsp;244981
}}
{{Starbox reference
| Simbad = LTT+7053
| ARICNS = 01434
| NSTED = Mu+Arae
| EPE = mu+Ara
}}
{{Starbox end}}
'''Mu Arae''' ('''μ Arae''', abbreviated '''Mu Ara''', '''μ Ara'''), often designated '''HD 160691''', officially named '''Cervantes''' {{IPAc-en|s|ɜːr|'|v|æ|n|t|iː|z}} {{respell|sur|VAN|teez}},<ref name="IAU-CSN">{{cite web | url=http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt | title=IAU Catalog of Star Names |access-date=28 July 2016}}</ref> is a ] ] ] approximately 50 ]s away from the ] in the ] of ]. The star has a ] with four known ] (designated ], ], ] and ]; later named Quijote, Dulcinea, Rocinante and Sancho, respectively), three of them with masses comparable with that of ]. Mu Arae c, the innermost, was the first ] or ] discovered.


== Nomenclature ==
'''Mu Arae''' (μ Ara / μ Arae) is a ]like yellow-orange ] located around 50 light years away in the ] ]. The star has a ] with four known planets. The system's innermost planet was the first "hot Neptune" to be discovered.


''μ Arae'' (] to ''Mu Arae'') is the star's ]. HD 160691 is the entry in the ].
== Distance and visibility ==

According to measurements made by the ] ] ], Mu Arae exhibits a ] of 65.46 ]s as the ] moves around the Sun. When combined with the known distance from the Earth to the Sun, this means the star is located at a distance of 49.8 ]s (15.3 ]s).<ref>{{cite web|url=http://vizier.u-strasbg.fr/viz-bin/VizieR-S?HIP%2086796|work=The Hipparcos and Tycho Catalogues|publisher=ESA|year=1997|title=HIP 86796|accessmonthday=10 September|accessyear=2006}}</ref> Seen from ] it has an ] of +5.12 and is visible to the ].
The established convention for extrasolar planets is that the planets receive designations consisting of the star's name followed by lower-case ] starting from "b", in order of discovery.<ref name="planetnaming">{{cite arXiv |title=On the naming convention used for multiple star systems and extrasolar planets |year=2010 |eprint=1012.0707 |class=astro-ph.SR |last1= Hessman |first1=F. V. |last2= Dhillon |first2=V. S. |last3= Winget |first3=D. E. |last4= Schreiber |first4=M. R. |last5= Horne |first5=K. |last6= Marsh |first6=T. R. |last7= Guenther |first7=E. |last8= Schwope |first8=A. |last9= Heber |first9=U.}}</ref> This system was used by a team led by ].<ref name="gozdziewski"/> On the other hand, a team led by ] proposed a modification of the designation system, where the planets are designated in order of characterization.<ref name="pepe"/> Since the parameters of the outermost planet were poorly constrained before the introduction of the 4-planet model of the system, this results in a different order of designations for the planets in the Mu Arae system. Both systems agree on the designation of the 640-day planet as "b". The old system designates the 9-day planet as "d", the 310-day planet as "e" and the outer planet as "c". Since the ] has not defined an official system for designations of extrasolar planets,<ref>{{cite web|url=http://www.iau.org/PLANETS_AROUND_OTHER_STARS.247.0.html|title=Planets Around Other Stars|publisher=IAU|access-date=16 September 2006|url-status=dead|archive-url=https://web.archive.org/web/20060928091032/http://www.iau.org/PLANETS_AROUND_OTHER_STARS.247.0.html|archive-date=28 September 2006}}</ref> the issue of which convention is 'correct' remains open, however most subsequent scientific publications about this system appear to have adopted the Pepe ''et al.'' system, as has the system's entry in the ].<ref>{{cite journal|bibcode=2008MNRAS.386L..43S|title=New solutions for the planetary dynamics in HD160691 using a Newtonian model and latest data|author=Short, D. |author2=Windmiller, G. |author3=Orosz, J. A.|journal=]|volume=386|issue=1|pages=L43–L46|doi=10.1111/j.1745-3933.2008.00457.x|year=2008|doi-access=free |arxiv = 0802.1781 |s2cid=15410895}}</ref><ref>{{cite encyclopedia |url=http://exoplanet.eu/star.php?st=HD+160691 |title=Notes for star HD 160691 |access-date=11 April 2009 |url-status=dead |archive-url=https://web.archive.org/web/20081222144505/http://exoplanet.eu/star.php?st=HD+160691 |encyclopedia=] |archive-date=22 December 2008 }}</ref>

In July 2014 the ] launched ], a process for giving proper names to certain exoplanets and their host stars.<ref>. IAU.org. 9 July 2014</ref> The process involved public nomination and voting for the new names.<ref>{{Cite web |url=http://nameexoworlds.iau.org/process |title=NameExoWorlds The Process |access-date=5 September 2015 |archive-date=15 August 2015 |archive-url=https://web.archive.org/web/20150815025117/http://www.nameexoworlds.iau.org/process |url-status=dead }}</ref> In December 2015, the IAU announced the winning names were Cervantes for this star and Quijote, Dulcinea, Rocinante and Sancho, for its planets (b, c, d, and e, respectively; the IAU used the Pepe ''et al'' system).<ref>, International Astronomical Union, 15 December 2015.</ref><ref>{{cite web |url=http://nameexoworlds.iau.org/systems/106 |title=The Proposals page for Mu Arae |date=3 January 2016 |publisher=] |archive-url=https://web.archive.org/web/20190417033628/http://nameexoworlds.iau.org:80/systems/106 |archive-date=17 April 2019}}</ref>

The winning names were those submitted by the Planetario de Pamplona, Spain. ] Saavedra (1547–1616) was a famous Spanish writer and author of '']''. The planets are named after characters of that novel: Quijote was the lead character; ] his love interest; ] his horse, and ] his ].<ref></ref>

In 2016, the IAU organized a ] (WGSN)<ref name="WGSN">{{cite web | url=https://www.iau.org/science/scientific_bodies/working_groups/280/ | title=IAU Working Group on Star Names (WGSN)|access-date=22 May 2016}}</ref> to catalog and standardize proper names for stars. In its first bulletin of July 2016,<ref name="WGSN1">{{cite web | url=http://www.pas.rochester.edu/~emamajek/WGSN/WGSN_bulletin1.pdf | title=Bulletin of the IAU Working Group on Star Names, No. 1 |access-date=28 July 2016}}</ref> the WGSN explicitly recognized the names of exoplanets and their host stars approved by the Executive Committee Working Group Public Naming of Planets and Planetary Satellites, including the names of stars adopted during the 2015 NameExoWorlds campaign. This star is now so entered in the IAU Catalog of Star Names.<ref name="IAU-CSN"/>


== Stellar characteristics == == Stellar characteristics ==
Mu Arae is estimated to be slightly more ]ive than our Sun at around 1.10 ]es. Based on the abundance of ], it is around twice as enriched in heavy elements as our Sun, and is therefore described as ]. Its surface ] of around 5800 ] is similar to our Sun.<ref name="santos">{{cite journal|url=http://adsabs.harvard.edu/cgi-bin/nph-bib_query?2004A%26A...426L..19S&db_key=AST|author=Santos ''et al.''|title=The HARPS survey for southern extra-solar planets II. A 14 Earth-masses exoplanet around μ Arae|journal=]|volume=426|year=2004|pages=L19 &ndash; L23}}</ref> The star has a ] estimated to be 31.5% greater than our Sun and is 75% more ].<ref name="valenti">{{cite web|url=http://data.bao.ac.cn/viz-bin/VizieR-5?-out.add=.&-source=J/ApJS/159/141/stars&recno=764|work=Spectroscopic properties of cool stars. I.|author=Valenti, J. ''et al.''|year=2005|title=SPOCS 763|accessmonthday=10 September|accessyear=2006}}</ref>


According to measurements made by the ] ] ], Mu Arae exhibits a ] of 64.0853 ]s as the Earth moves around the Sun. When combined with the known distance from the Earth to the Sun, this means the star is located at a distance of {{convert|50.89|ly|pc|lk=on|abbr=off}}.<ref name=GaiaDR3/><ref group="note">The formula for converting parallax to distance is <math>\scriptstyle\mathrm{Distance\ in\ parsecs}=\frac{1}{\mathrm{parallax\ in\ arcseconds}}</math></ref> Seen from Earth it has an ] of +5.15 and is thus visible to the ].
As a star ages, the level of activity in its ] is expected to decline. Based on observed activity levels, the age of Mu Arae is estimated to be around 6,410 ] or 1,450 million years, depending on the theoretical model used.<ref>{{cite journal|url=http://cdsads.u-strasbg.fr/cgi-bin/nph-bib_query?2005A%26A...443..609S&db_key=AST&nosetcookie=1|author=Saffe, C. ''et al.''|title=On the Ages of Exoplanet Host Stars|journal=]|volume=443|issue=2|pages=609 &ndash; 626|year=2005}}</ref> Another way to estimate the star's age is to match its properties with models of ]. This method suggests an age of around 4,400 million years.<ref name="valenti" />


] analysis of the star reveals it is approximately 10% more massive than the Sun and significantly older, at around 6.34&nbsp;billion years. The radius of the star is 36% greater than that of the Sun and it is 90% more luminous. The star contains twice the abundance of iron relative to ] of the Sun and is therefore described as ]. Mu Arae is also more enriched than the Sun in the element ].<ref name="soriano2009" />
Mu Arae has a listed ] of G3IV&ndash;V. The G3 part means the star is classified as yellow in colour, similar to our Sun (a G2V star). The star may be entering the ] stage of its evolution as it starts to run out of ] in its core. This is reflected in its uncertain ], between IV (the subgiants) and V (] dwarf stars like the Sun).

Mu Arae has a listed ] of G3IV–V.<ref name=aj132_1_161/> The G3 part means the star is similar to the Sun (a G2V star). The star may be entering the ] stage of its evolution as it starts to run out of ] in its core. This is reflected in its uncertain ], between IV (the subgiants) and V (] ] stars like the Sun).


== Planetary system == == Planetary system ==
] of the exoplanets of Cervantes based in the ]: Dulcinea, Rocinante, Quijote y Sancho.]]
]
]
As of August 2006, four ]s have been detected in orbit around Mu Arae. Three have high masses and are likely to be ]s. The innermost planet has a mass comparable to that of ] and may either be a small gas giant or a large ].
]. Central star is not to scale. At the scale of this picture, the innermost planet would be located at the edge of the disc representing the central star.]]


=== Discovery === === Discovery ===
In ], an extrasolar planet was announced by the ] team, together with the planet orbiting ]. The planet, designated ], was thought to be in a highly ] orbit of around 743 days.<ref>{{cite journal|url=http://www.journals.uchicago.edu/ApJ/journal/issues/ApJ/v555n1/53257/brief/53257.abstract.html|author=Butler, R. ''et al.''|title=Two New Planets from the Anglo-Australian Planet Search|journal=]|volume=555|issue=1|year=2001|pages=410 &ndash; 417}}</ref> The discovery was made by analysing variations in the star's ] (measured by observing the ] of the star's ]s) as a result of being pulled around by the planet's ]. In 2001, an extrasolar planet was announced by the ] team, together with the planet orbiting ]. The planet, designated ], was thought to be in a highly ] orbit of around 743 days.<ref>{{cite journal | author=Butler | title=Two New Planets from the Anglo-Australian Planet Search | journal=The Astrophysical Journal | volume=555 | issue=1 |year=2001 | pages=410–417 | doi=10.1086/321467 | last2=Tinney | first2=C. G. | last3=Marcy | first3=Geoffrey W. | last4=Jones | first4=Hugh R. A. | last5=Penny | first5=Alan J. | last6=Apps | first6=Kevin | bibcode=2001ApJ...555..410B| hdl=2299/137 | s2cid=122572834 | hdl-access=free }}</ref> The discovery was made by analysing variations in the star's ] (measured by observing the ] of the star's ]s) as a result of being pulled around by the planet's ]. Further observations revealed the presence of a second object in the system (now designated as ]), which was published in 2004. At the time, the parameters of this planet were poorly constrained and it was thought to be in an orbit of around 8.2 years with a high eccentricity.<ref name="McCarthy2004"/> Later in 2004, a small inner planet designated ] was announced with a mass comparable with that of ] in a 9-day orbit. This was the first of the class of planets known as "]s" to be discovered. The discovery was made by making high-precision radial velocity measurements with the ] (HARPS) ].<ref name="santos">{{cite journal|bibcode=2004A&A...426L..19S |last1=Santos |first1=N. C. |title=The HARPS survey for southern extra-solar planets II. A 14 Earth-masses exoplanet around μ Arae|journal=]|volume=426 |issue=1|year=2004|pages=L19 – L23|doi=10.1051/0004-6361:200400076 |last2=Bouchy|first2=F. |last3=Mayor|first3=M. |last4=Pepe|first4=F. |last5=Queloz|first5=D. |last6=Udry|first6=S. |last7=Lovis|first7=C. |last8=Bazot|first8=M. |last9=Benz|first9=W. |last10=Bertaux|first10=J.-L. |last11=Lo Curto|first11=G. |last12=Delfosse|first12=X. |last13=Mordasini|first13=C. |last14=Naef|first14=D. |last15=Sivan|first15=J.-P. |last16=Vauclair|first16=S. |arxiv = astro-ph/0408471 |s2cid=14938593 |display-authors=8}}</ref>


In 2006, two teams, one led by ] and the other by ] independently announced four-planet models for the radial velocity measurements of the star, with a new planet (]) in a near-circular orbit lasting approximately 311 days.<ref name="gozdziewski">{{Cite journal|author=Gozdziewski, K.|title=On the extrasolar multi-planet system around HD160691|journal=The Astrophysical Journal|volume=657|issue=1|pages=546–558|year=2007|arxiv=astro-ph/0608279|last2= Maciejewski|first2=Andrzej J.|last3=Migaszewski|first3=Cezary|doi=10.1086/510554|bibcode = 2007ApJ...657..546G |s2cid=16620036}}</ref><ref name="pepe">{{Cite journal|author=Pepe, F.|title=The HARPS search for southern extra-solar planets. IX. μ Ara, a system with four planets|journal=Astronomy and Astrophysics|volume=462|issue=2|pages=769–776|year=2006|arxiv=astro-ph/0608396|last2= Correia|first2=A. C. M.|last3= Mayor|first3=M.|last4= Tamuz|first4=O.|last5= Benz|first5=W.|last6= Bertaux|first6=J. -L.|last7= Bouchy|first7=F.|last8= Couetdic|first8=J.|last9= Laskar|first9=J.|last10= Lovis|first10=C.|last11= Naef|first11=D.|last12= Queloz|first12=D.|last13= Santos|first13=N. C.|last14= Sivan|first14=J. -P.|last15= Sosnowska|first15=D.|last16= Udry|first16=S.|doi=10.1051/0004-6361:20066194|bibcode = 2007A&A...462..769P |s2cid=119071803}}</ref> The new model gives revised parameters for the previously known planets, with lower eccentricity orbits than in the previous model and including a more robust characterization of the orbit of Mu Arae e. The discovery of the fourth planet made Mu Arae the second known four-planet extrasolar system, after ].
Further observations revealed the presence of a second object in the system (]), which was published in ]. At the time, the parameters of this planet were poorly constrained and it was thought to be in an orbit of around 8.2 ]s with a high eccentricity.<ref>{{cite journal|url=http://adsabs.harvard.edu/cgi-bin/nph-bib_query?2004ApJ...617..575M&db_key=AST|author=McCarthy ''et al.''|title=Multiple Companions to HD 154857 and HD 160691|journal=]|volume=617|issue=1|year=2004|pages=575-579}}</ref>


=== System architecture and habitability ===
Later in ], a small inner planet designated ] was announced with a mass comparable to that of ] in a 9-day orbit. This was the first of the class of planets known as "hot Neptunes" to be discovered. The discovery was made by making high-precision radial velocity measurements with the ] (HARPS) ].<ref name="santos" />
The Mu Arae system consists of an inner Uranus-mass planet in a tight 9-day orbit and three massive planets, probably gas giants, on wide, near-circular orbits, which contrasts with the high-eccentricity orbits typically observed for long-period extrasolar planets. The Uranus-mass planet may be a ], the ] of a gas giant which has had its outer layers stripped away by stellar radiation.<ref>{{cite journal|bibcode=2006A&A...450.1221B |author=Baraffe, I.|title=Birth and fate of hot-Neptune planets|journal=]|volume=450|issue=3|year=2006|pages=1221–1229|doi=10.1051/0004-6361:20054040|arxiv = astro-ph/0512091 |last2=Alibert|first2=Y.|last3=Chabrier|first3=G.|last4=Benz|first4=W.|s2cid=15574680}}</ref> Alternatively it may have formed in the inner regions of the Mu Arae system as a rocky "super-Earth".<ref name="santos"/>


The inner gas giants "d" and "b" are located close to the 2:1 ] which causes them to undergo strong interactions. The best-fit solution to the system is actually unstable:<ref>{{cite journal |last1=Agnew |first1=Matthew T |last2=Maddison |first2=Sarah T |last3=Horner |first3=Jonathan |last4=Kane |first4=Stephen R |title=Predicting multiple planet stability and habitable zone companions in the TESS era |journal=Monthly Notices of the Royal Astronomical Society |date=June 2019 |volume=485 |issue=4 |pages=4703–4725 |doi=10.1093/mnras/stz345|arxiv=1901.11297 |doi-access=free }}</ref><ref name="Benedict2022"/> simulations suggest the system is destroyed after 78 million years, which is significantly shorter than the estimated age of the star system. More stable solutions, including ones in which the two planets are actually in the resonance (similar to the situation in the ] system) can be found which give only a slightly worse fit to the data.<ref name="pepe"/> A 2022 study finds a stable orbital fit to the system, and estimates a lower limit on the system ] of about 20°.<ref name="Goździewski2022"/>
In 2006, two teams, one led by ] and the other by ] independently announced four-planet models for the radial velocity measurements of the star, with a new planet (]) in a near-circular orbit lasting approximately 311 days.<ref name="gozdziewski">{{cite arXiv|author=Gozdziewski, K. ''et al.''|title=About the extrasolar multi-planet system around HD160691|year=2006|version=August 14, 2006|eprint=astro-ph/0608279}}</ref><ref name="pepe">{{cite arXiv|author=Pepe, F. ''et al.''|title=The HARPS search for southern extra-solar planets. IX. μ Ara, a system with four planets|year=2006|version=August 18, 2006|eprint=astro-ph/0608396}}</ref> The new model gives revised parameters for the previously known planets, with lower eccentricity orbits than in the previous model. The discovery of the fourth planet made Mu Arae the second known four-planet extrasolar system, after ].


] observations using the ] have not detected any of the known planets, but have set upper limits on the masses of the outer three planets: planet b is {{Jupiter mass|<4.3|link=y}}, planet d is {{Jupiter mass|<7.0}}, and planet e is {{Jupiter mass|<4.4}}.<ref name="Benedict2022"/> Searches for ]s show no evidence for a debris disc similar to the ] around Mu Arae. If Mu Arae does have a Kuiper belt, it is too faint to be detected with current instruments.<ref>{{cite journal|bibcode=2004A&A...424..613S |author=Schütz, O.|title=A search for circumstellar dust disks with ADONIS|journal=]|volume=424 |issue=2|year=2004|pages=613–618|doi=10.1051/0004-6361:20034215|arxiv = astro-ph/0408530 |last2=Bönhardt|first2=H.|last3=Pantin|first3=E.|last4=Sterzik|first4=M.|last5=Els|first5=S.|last6=Hahn|first6=J.|last7=Henning|first7=Th.|s2cid=25921357}}</ref>
=== System structure ===
]
The Mu Arae system consists of an inner Uranus-mass planet in a tight 9-day orbit and three massive planets, probably gas giants, on wide, near-circular orbits, which contrasts with the high-eccentricity orbits typically observed for long-period extrasolar planets. The Uranus-mass planet may be a ], the ] of a gas giant which has had its outer layers stripped away by stellar radiation.<ref>{{cite journal|url=http://adsabs.harvard.edu/cgi-bin/nph-bib_query?2006A%26A...450.1221B&db_key=AST|author=Baraffe, I. ''et al.''|title=Birth and fate of hot-Neptune planets|journal=]|volume=450|issue=3|year=2006|pages=1221 &ndash; 1229}}</ref> Alternatively it may have formed in the inner regions of the Mu Arae system as a rocky "super-Earth".<ref name="santos" />


The gas giant planet "b" is located in the liquid water habitable zone of Mu Arae. This would prevent an Earth-like planet from forming in the habitable zone, however large ] of the gas giant could ] On the other hand, it is unclear whether moons sufficiently massive to retain an atmosphere and liquid water could actually form around a gas giant planet, due to a theorized scaling law between the mass of a planet and its satellite system.<ref>{{cite journal|doi= 10.1038/nature04860|author=Canup, R. |author1-link=Robin Canup |author2=Ward, W.|title=A common mass scaling for satellite systems of gaseous planets|journal=]|volume=441|year=2006|pages=834–839|pmid= 16778883|issue= 7095|bibcode = 2006Natur.441..834C |s2cid=4327454 }}</ref> In addition, measurements of the star's ] ] suggest that any potentially ] planets or moons may not receive enough ultraviolet to trigger the formation of ]s.<ref name="buccino">{{cite journal|bibcode=2006Icar..183..491B|author=Buccino, A.|title=Ultraviolet Radiation Constraints around the Circumstellar Habitable Zones|journal=]|volume=183|issue=2|pages=491–503|year=2006|doi=10.1016/j.icarus.2006.03.007|arxiv = astro-ph/0512291 |last2=Lemarchand|first2=Guillermo A.|last3=Mauas|first3=Pablo J.D.|s2cid=2241081}}</ref> Planet "d" would receive a similar amount of ultraviolet to the Earth and thus lies in the ]. However, it would be too hot for any moons to support surface liquid water.
The inner gas giants "e" and "b" are located close to the 2:1 ] which causes them to undergo strong interactions. The best-fit solution to the system is actually unstable: simulations suggest the system is destroyed after 78 million years, which is significantly shorter than the estimated age of the star system. More stable solutions, including ones in which the two planets are actually in the resonance (similar to the situation in the ] system) can be found which give only a slightly worse fit to the data.<ref name="pepe" />


{{OrbitboxPlanet begin
Searches for ]s show no evidence for a debris disc similar to the ] around Mu Arae. If Mu Arae does have a Kuiper belt, it is too faint to be detected with current instruments.<ref>{{cite journal|url=http://adsabs.harvard.edu/cgi-bin/nph-bib_query?2004A%26A...424..613S&db_key=AST|author=Schütz, O. ''et al.''|title=A search for circumstellar dust disks with ADONIS|journal=]|volume=424|year=2004|pages=613 &ndash; 618}}</ref>
| table_ref = <ref name="Goździewski2022"/>
}}
{{OrbitboxPlanet
| exoplanet = ]
| mass = {{val|0.032|0.002|p=≥}}
| period = {{val|9.638|0.001}}
| semimajor = {{val|0.092319|0.000005}}
| eccentricity = {{val|0.090|0.042}}
}}
{{OrbitboxPlanet
| exoplanet = ]
| mass = {{val|0.448|0.011|p=≥}}
| period = {{val|308.36|0.29}}
| semimajor = {{val|0.9347|0.0015}}
| eccentricity = {{val|0.055|0.014}}
}}
{{OrbitboxPlanet
| exoplanet = ]
| mass = {{val|1.65|0.009|p=≥}}
| period = {{val|644.92|0.29}}
| semimajor = {{val|1.522|0.001}}
| eccentricity = {{val|0.041|0.009}}
}}
{{OrbitboxPlanet
| exoplanet = ]
| mass = {{val|1.932|0.022|p=≥}}
| period = {{val|4019|24|fmt=commas}}
| semimajor = {{val|5.204|0.021}}
| eccentricity = {{val|0.049|0.011}}
}}
{{Orbitbox end}}


== See also ==
{{Planetbox-4p
| ] * ]
* ]
| &gt;0.03321
* ]
| 9.6386 ± 0.0015
* ]
| 0.09094
| 0.172 ± 0.04
|-
| ]
| &gt;0.5219
| 310.55 ± 0.83
| 0.921
| 0.0666 ± 0.0122
|-
| ]
| &gt;1.676
| 643.25 ± 0.90
| 1.497
| 0.128 ± 0.017
|-
| ]
| &gt;1.814
| 4205.8 ± 758.9
| 5.235
| 0.0985 ± 0.0627}}


=== Habitability === == Notes ==
<references group="note" />
The gas giant planet "b" is located in the liquid water habitable zone of Mu Arae. This would prevent an Earthlike planet from forming in the habitable zone, however large ] of the gas giant could potentially support liquid water. On the other hand it is unclear whether such massive moons could actually form around a gas giant planet, thanks to an apparent scaling law between the mass of the planet and its satellite system.<ref>{{cite journal|url=http://www.nature.com/nature/journal/v441/n7095/abs/nature04860.html|author=Canup, R., Ward, W.|title=A common mass scaling for satellite systems of gaseous planets|journal=]|volume=441|year=2006|pages=834 &ndash; 839}}</ref> In addition, measurements of the star's ] ] suggest that any potentially ] planets or moons may not receive enough ultraviolet to trigger the formation of ]s.<ref name="buccino">{{cite journal|url=http://adsabs.harvard.edu/abs/2005astro.ph.12291B|author=Buccino, A. ''et al.''|title=Ultraviolet Radiation Constraints around the Circumstellar Habitable Zones|journal=]|volume=183|issue=2|pages=491 &ndash; 503|year=2006}}</ref>


== References ==
Planet "e" would receive a similar amount of ultraviolet to the Earth and thus lies in the ultraviolet habitable zone, however, it would be too hot for any moons to support surface liquid water.
{{Reflist|refs=


<ref name=GaiaDR3>{{Cite Gaia DR3|5945941905576552064}}</ref>
===Planet naming conventions===
The established convention for extrasolar planets is that the planets receive lower-case ] starting from "b", in order of discovery. This system is used by the team led by Goździewski,<ref name="gozdziewski" /> and has been adopted in this article for compatibility with the designations used previously for the 3-planet model.


<ref name=aj132_1_161>{{Cite journal| display-authors=1 | last1=Gray | first1=R. O. | first2=C. J. | last2=Corbally | first3=R. F. | last3=Garrison | first4=M. T. | last4=McFadden | last5=Bubar | first5=E. J. | last6=McGahee | first6=C. E. | last7=O'Donoghue | first7=A. A. | last8=Knox | first8=E. R. | title=Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I | journal=The Astronomical Journal | volume=132 | issue=1 | pages=161–170 |date=July 2006 | doi=10.1086/504637 | bibcode=2006AJ....132..161G |arxiv = astro-ph/0603770 | s2cid=119476992 }}</ref>
On the other hand, the team led by Pepe have proposed a modification of the designation system, where the planets are designated in order of characterisation.<ref name="pepe" /> Since the parameters of the outermost planet were poorly constrained before the introduction of the 4-planet model of the system, this results in a different order of designations for the planets in the Mu Arae system. Both systems agree on the designation of the 670-day planet as "b". The Pepe system designates the 9-day planet as "c", the 310-day planet as "d" and the outer planet as "e".


<ref name=Anderson2012>{{cite journal
Since the ] has not defined an official system for designations of extrasolar planets,<ref>{{cite web|url=http://www.iau.org/PLANETS_AROUND_OTHER_STARS.247.0.html|title=Planets Around Other Stars|publisher=IAU|accessmonthday=16 September|accessyear=2006}}</ref> the issue of which convention is "correct" remains open.
| title=XHIP: An extended hipparcos compilation
| last1=Anderson | first1=E. | last2=Francis | first2=Ch.
| journal=Astronomy Letters
| volume=38 | issue=5 | pages=331 | year=2012
| bibcode=2012AstL...38..331A | doi=10.1134/S1063773712050015
| arxiv=1108.4971 | s2cid=119257644 }}</ref>


<ref name=ibsh8_30>{{Cite journal| last1=Feinstein | first1=A. | title=Photoelectric observations of Southern late-type stars | journal=The Information Bulletin for the Southern Hemisphere | volume=8 | page=30 |year=1966 | bibcode=1966IBSH....8...30F }}</ref>
==References==
<div class="references-small"><references /></div>


<ref name="McCarthy2004">{{cite journal | title=Multiple Companions to HD 154857 and HD 160691 | last1=McCarthy | first1=Chris | last2=Butler | first2=R. Paul | last3=Tinney | first3=C. G. | last4=Jones | first4=Hugh R. A. | last5=Marcy | first5=Geoffrey W. | last6=Carter | first6=Brad | last7=Penny | first7=Alan J. | last8=Fischer | first8=Debra A. | display-authors=1 | journal=The Astrophysical Journal | volume=617 | issue=1 | pages=575–579 |year=2004 | arxiv=astro-ph/0409335 | bibcode=2004ApJ...617..575M | doi=10.1086/425214 | s2cid=119446133 }}</ref>
==See also==
* ]
* ]
* ]


<ref name="Benedict2022">{{cite journal |last1=Benedict |first1=G. F. |last2=McArthur |first2=B. E. |date=June 2022 |title=The μ Arae Planetary System: Radial Velocities and Astrometry |journal=] |volume=163 |issue=6 |pages=295 |doi=10.3847/1538-3881/ac6ac8 |arxiv=2204.13706 |bibcode=2022AJ....163..295B|s2cid=248476290 |doi-access=free }}</ref>
==External links==
*
*
*
*
*
*
*


<ref name="Goździewski2022">{{cite journal |last=Goździewski |first=Krzysztof |arxiv=2209.04542 |title=The orbital architecture and stability of the μ Arae planetary system |journal=Monthly Notices of the Royal Astronomical Society |date=September 2022|volume=516 |issue=4 |pages=6096–6115 |doi=10.1093/mnras/stac2584 |doi-access=free }}</ref>


}}
{{Mu Arae}}


== External links ==
]
{{Commons category|Mu Arae}}
]
*
]
*
]
* {{cite web |url=http://www.space.com/scienceastronomy/super_earth_040825.html |title='Super Earth' Discovered at Nearby Star |access-date=17 July 2008 |work=] |date=25 August 2004 |first=Robert Roy |last=Britt }}
]
* {{cite web |url=http://www.eso.org/public/outreach/press-rel/pr-2004/pr-22-04.html |title=Fourteen Times the Earth |access-date=17 July 2008 |work=] |date=25 August 2004 |url-status=dead |archive-url=https://web.archive.org/web/20070607190706/http://www.eso.org/public/outreach/press-rel/pr-2004/pr-22-04.html |archive-date=7 June 2007 }}
* {{cite web |url=http://obswww.unige.ch/Exoplanets/hd160691.html |title=Mu Ara: a system with 4 planets |access-date=17 July 2008 |work=Geneva Observatory |archive-date=9 June 2008 |archive-url=https://web.archive.org/web/20080609091537/http://obswww.unige.ch/Exoplanets/hd160691.html |url-status=dead }}
* {{cite web |url=http://www.solstation.com/stars2/mu-arae.htm |title=Mu Arae |access-date=17 July 2008 |work=SolStation }}
*
* {{Webarchive|url=https://web.archive.org/web/20160505160348/http://www.lpl.arizona.edu/~rory/research/xsp/dynamics/ |date=5 May 2016 }} by Rory Barnes & Richard Greenberg, Lunar and Planetary Lab, University of Arizona


{{Mu Arae|state=collapsed}}
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{{Stars of Ara}}
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Latest revision as of 15:39, 19 August 2024

Star in the constellation Ara

Mu Arae / Cervantes
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ara
Right ascension 17 44 08.70314
Declination −51° 50′ 02.5916″
Apparent magnitude (V) 5.15
Characteristics
Spectral type G3IV–V
Apparent magnitude (V) 5.15±0.01
Apparent magnitude (G) 4.943±0.003
Apparent magnitude (K) 3.68±0.25
U−B color index +0.24
B−V color index +0.70
Astrometry
Radial velocity (Rv)−9.54±0.13 km/s
Proper motion (μ) RA: −15.034±0.084 mas/yr
Dec.: −190.901±0.065 mas/yr
Parallax (π)64.0853 ± 0.0904 mas
Distance50.89 ± 0.07 ly
(15.60 ± 0.02 pc)
Absolute magnitude (MV)+4.17
Details
Mass1.10±0.01 M☉
Radius1.36±0.01 R☉
Luminosity1.90±0.10 L☉
Surface gravity (log g)4.2±0.1 cgs
Temperature5,820±40 K
Metallicity200±5%
Metallicity 0.30±0.01 dex
Rotational velocity (v sin i)3.1±0.5 km/s
Age6.34±0.40 Gyr
Other designations
Cervantes, CD−51°11094, FK5 662, GC 24024, GJ 691, HD 160691, HIP 86796, HR 6585, SAO 244981
Database references
SIMBADdata
Exoplanet Archivedata
ARICNSdata

Mu Arae (μ Arae, abbreviated Mu Ara, μ Ara), often designated HD 160691, officially named Cervantes /sɜːrˈvæntiːz/ sur-VAN-teez, is a main sequence G-type star approximately 50 light-years away from the Sun in the constellation of Ara. The star has a planetary system with four known extrasolar planets (designated Mu Arae b, c, d and e; later named Quijote, Dulcinea, Rocinante and Sancho, respectively), three of them with masses comparable with that of Jupiter. Mu Arae c, the innermost, was the first hot Neptune or super-Earth discovered.

Nomenclature

μ Arae (Latinised to Mu Arae) is the star's Bayer designation. HD 160691 is the entry in the Henry Draper Catalogue.

The established convention for extrasolar planets is that the planets receive designations consisting of the star's name followed by lower-case Roman letters starting from "b", in order of discovery. This system was used by a team led by Krzysztof Goździewski. On the other hand, a team led by Francesco Pepe proposed a modification of the designation system, where the planets are designated in order of characterization. Since the parameters of the outermost planet were poorly constrained before the introduction of the 4-planet model of the system, this results in a different order of designations for the planets in the Mu Arae system. Both systems agree on the designation of the 640-day planet as "b". The old system designates the 9-day planet as "d", the 310-day planet as "e" and the outer planet as "c". Since the International Astronomical Union has not defined an official system for designations of extrasolar planets, the issue of which convention is 'correct' remains open, however most subsequent scientific publications about this system appear to have adopted the Pepe et al. system, as has the system's entry in the Extrasolar Planets Encyclopaedia.

In July 2014 the International Astronomical Union launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars. The process involved public nomination and voting for the new names. In December 2015, the IAU announced the winning names were Cervantes for this star and Quijote, Dulcinea, Rocinante and Sancho, for its planets (b, c, d, and e, respectively; the IAU used the Pepe et al system).

The winning names were those submitted by the Planetario de Pamplona, Spain. Miguel de Cervantes Saavedra (1547–1616) was a famous Spanish writer and author of El Ingenioso Hidalgo Don Quixote de la Mancha. The planets are named after characters of that novel: Quijote was the lead character; Dulcinea his love interest; Rocinante his horse, and Sancho his squire.

In 2016, the IAU organized a Working Group on Star Names (WGSN) to catalog and standardize proper names for stars. In its first bulletin of July 2016, the WGSN explicitly recognized the names of exoplanets and their host stars approved by the Executive Committee Working Group Public Naming of Planets and Planetary Satellites, including the names of stars adopted during the 2015 NameExoWorlds campaign. This star is now so entered in the IAU Catalog of Star Names.

Stellar characteristics

According to measurements made by the Gaia astrometric satellite, Mu Arae exhibits a parallax of 64.0853 milliarcseconds as the Earth moves around the Sun. When combined with the known distance from the Earth to the Sun, this means the star is located at a distance of 50.89 light-years (15.60 parsecs). Seen from Earth it has an apparent magnitude of +5.15 and is thus visible to the naked eye.

Asteroseismic analysis of the star reveals it is approximately 10% more massive than the Sun and significantly older, at around 6.34 billion years. The radius of the star is 36% greater than that of the Sun and it is 90% more luminous. The star contains twice the abundance of iron relative to hydrogen of the Sun and is therefore described as metal-rich. Mu Arae is also more enriched than the Sun in the element helium.

Mu Arae has a listed spectral type of G3IV–V. The G3 part means the star is similar to the Sun (a G2V star). The star may be entering the subgiant stage of its evolution as it starts to run out of hydrogen in its core. This is reflected in its uncertain luminosity class, between IV (the subgiants) and V (main sequence dwarf star stars like the Sun).

Planetary system

Emulation in Celestia of the exoplanets of Cervantes based in the Sudarsky's gas giant classification: Dulcinea, Rocinante, Quijote y Sancho.
The Mu Arae star with distance relationships for its four planets
The orbits of the outer three planets in the Mu Arae system compared with those in the Solar System. Central star is not to scale. At the scale of this picture, the innermost planet would be located at the edge of the disc representing the central star.

Discovery

In 2001, an extrasolar planet was announced by the Anglo-Australian Planet Search team, together with the planet orbiting Epsilon Reticuli. The planet, designated Mu Arae b, was thought to be in a highly eccentric orbit of around 743 days. The discovery was made by analysing variations in the star's radial velocity (measured by observing the Doppler shift of the star's spectral lines) as a result of being pulled around by the planet's gravity. Further observations revealed the presence of a second object in the system (now designated as Mu Arae e), which was published in 2004. At the time, the parameters of this planet were poorly constrained and it was thought to be in an orbit of around 8.2 years with a high eccentricity. Later in 2004, a small inner planet designated Mu Arae c was announced with a mass comparable with that of Uranus in a 9-day orbit. This was the first of the class of planets known as "hot Neptunes" to be discovered. The discovery was made by making high-precision radial velocity measurements with the High Accuracy Radial Velocity Planet Searcher (HARPS) spectrograph.

In 2006, two teams, one led by Krzysztof Goździewski and the other by Francesco Pepe independently announced four-planet models for the radial velocity measurements of the star, with a new planet (Mu Arae d) in a near-circular orbit lasting approximately 311 days. The new model gives revised parameters for the previously known planets, with lower eccentricity orbits than in the previous model and including a more robust characterization of the orbit of Mu Arae e. The discovery of the fourth planet made Mu Arae the second known four-planet extrasolar system, after 55 Cancri.

System architecture and habitability

The Mu Arae system consists of an inner Uranus-mass planet in a tight 9-day orbit and three massive planets, probably gas giants, on wide, near-circular orbits, which contrasts with the high-eccentricity orbits typically observed for long-period extrasolar planets. The Uranus-mass planet may be a chthonian planet, the core of a gas giant which has had its outer layers stripped away by stellar radiation. Alternatively it may have formed in the inner regions of the Mu Arae system as a rocky "super-Earth".

The inner gas giants "d" and "b" are located close to the 2:1 orbital resonance which causes them to undergo strong interactions. The best-fit solution to the system is actually unstable: simulations suggest the system is destroyed after 78 million years, which is significantly shorter than the estimated age of the star system. More stable solutions, including ones in which the two planets are actually in the resonance (similar to the situation in the Gliese 876 system) can be found which give only a slightly worse fit to the data. A 2022 study finds a stable orbital fit to the system, and estimates a lower limit on the system inclination of about 20°.

Astrometric observations using the Hubble Space Telescope have not detected any of the known planets, but have set upper limits on the masses of the outer three planets: planet b is <4.3 MJ, planet d is <7.0 MJ, and planet e is <4.4 MJ. Searches for circumstellar discs show no evidence for a debris disc similar to the Kuiper belt around Mu Arae. If Mu Arae does have a Kuiper belt, it is too faint to be detected with current instruments.

The gas giant planet "b" is located in the liquid water habitable zone of Mu Arae. This would prevent an Earth-like planet from forming in the habitable zone, however large moons of the gas giant could potentially support liquid water. On the other hand, it is unclear whether moons sufficiently massive to retain an atmosphere and liquid water could actually form around a gas giant planet, due to a theorized scaling law between the mass of a planet and its satellite system. In addition, measurements of the star's ultraviolet flux suggest that any potentially habitable planets or moons may not receive enough ultraviolet to trigger the formation of biomolecules. Planet "d" would receive a similar amount of ultraviolet to the Earth and thus lies in the ultraviolet habitable zone. However, it would be too hot for any moons to support surface liquid water.

The Mu Arae planetary system
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
c (Dulcinea) ≥0.032±0.002 MJ 0.092319±0.000005 9.638±0.001 0.090±0.042 — —
d (Rocinante) ≥0.448±0.011 MJ 0.9347±0.0015 308.36±0.29 0.055±0.014 — —
b (Quijote) ≥1.65±0.009 MJ 1.522±0.001 644.92±0.29 0.041±0.009 — —
e (Sancho) ≥1.932±0.022 MJ 5.204±0.021 4,019±24 0.049±0.011 — —

See also

Notes

  1. From = 0.30 ± 0.01
  2. The formula for converting parallax to distance is D i s t a n c e   i n   p a r s e c s = 1 p a r a l l a x   i n   a r c s e c o n d s {\displaystyle \scriptstyle \mathrm {Distance\ in\ parsecs} ={\frac {1}{\mathrm {parallax\ in\ arcseconds} }}}

References

  1. ^ 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. ^ Benedict, G. F.; McArthur, B. E. (June 2022). "The μ Arae Planetary System: Radial Velocities and Astrometry". The Astronomical Journal. 163 (6): 295. arXiv:2204.13706. Bibcode:2022AJ....163..295B. doi:10.3847/1538-3881/ac6ac8. S2CID 248476290.
  3. ^ Gray, R. O.; et al. (July 2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 parsecs: The Northern Sample I". The Astronomical Journal. 132 (1): 161–170. arXiv:astro-ph/0603770. Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID 119476992.
  4. ^ Feinstein, A. (1966). "Photoelectric observations of Southern late-type stars". The Information Bulletin for the Southern Hemisphere. 8: 30. Bibcode:1966IBSH....8...30F.
  5. Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  6. ^ Soriano, M.; Vauclair, S. (2009). "New seismic analysis of the exoplanet-host star Mu Arae". Astronomy and Astrophysics. 513: A49. arXiv:0903.5475. Bibcode:2010A&A...513A..49S. doi:10.1051/0004-6361/200911862. S2CID 5688996.
  7. ^ "IAU Catalog of Star Names". Retrieved 28 July 2016.
  8. Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707 .
  9. ^ Gozdziewski, K.; Maciejewski, Andrzej J.; Migaszewski, Cezary (2007). "On the extrasolar multi-planet system around HD160691". The Astrophysical Journal. 657 (1): 546–558. arXiv:astro-ph/0608279. Bibcode:2007ApJ...657..546G. doi:10.1086/510554. S2CID 16620036.
  10. ^ Pepe, F.; Correia, A. C. M.; Mayor, M.; Tamuz, O.; Benz, W.; Bertaux, J. -L.; Bouchy, F.; Couetdic, J.; Laskar, J.; Lovis, C.; Naef, D.; Queloz, D.; Santos, N. C.; Sivan, J. -P.; Sosnowska, D.; Udry, S. (2006). "The HARPS search for southern extra-solar planets. IX. μ Ara, a system with four planets". Astronomy and Astrophysics. 462 (2): 769–776. arXiv:astro-ph/0608396. Bibcode:2007A&A...462..769P. doi:10.1051/0004-6361:20066194. S2CID 119071803.
  11. "Planets Around Other Stars". IAU. Archived from the original on 28 September 2006. Retrieved 16 September 2006.
  12. Short, D.; Windmiller, G.; Orosz, J. A. (2008). "New solutions for the planetary dynamics in HD160691 using a Newtonian model and latest data". MNRAS. 386 (1): L43 – L46. arXiv:0802.1781. Bibcode:2008MNRAS.386L..43S. doi:10.1111/j.1745-3933.2008.00457.x. S2CID 15410895.
  13. "Notes for star HD 160691". Extrasolar Planets Encyclopaedia. Archived from the original on 22 December 2008. Retrieved 11 April 2009.
  14. NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars. IAU.org. 9 July 2014
  15. "NameExoWorlds The Process". Archived from the original on 15 August 2015. Retrieved 5 September 2015.
  16. Final Results of NameExoWorlds Public Vote Released, International Astronomical Union, 15 December 2015.
  17. "The Proposals page for Mu Arae". International Astronomical Union. 3 January 2016. Archived from the original on 17 April 2019.
  18. NameExoWorlds The Approved Names
  19. "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  20. "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
  21. Butler; Tinney, C. G.; Marcy, Geoffrey W.; Jones, Hugh R. A.; Penny, Alan J.; Apps, Kevin (2001). "Two New Planets from the Anglo-Australian Planet Search". The Astrophysical Journal. 555 (1): 410–417. Bibcode:2001ApJ...555..410B. doi:10.1086/321467. hdl:2299/137. S2CID 122572834.
  22. McCarthy, Chris; et al. (2004). "Multiple Companions to HD 154857 and HD 160691". The Astrophysical Journal. 617 (1): 575–579. arXiv:astro-ph/0409335. Bibcode:2004ApJ...617..575M. doi:10.1086/425214. S2CID 119446133.
  23. ^ Santos, N. C.; Bouchy, F.; Mayor, M.; Pepe, F.; Queloz, D.; Udry, S.; Lovis, C.; Bazot, M.; et al. (2004). "The HARPS survey for southern extra-solar planets II. A 14 Earth-masses exoplanet around μ Arae". Astronomy and Astrophysics. 426 (1): L19 – L23. arXiv:astro-ph/0408471. Bibcode:2004A&A...426L..19S. doi:10.1051/0004-6361:200400076. S2CID 14938593.
  24. Baraffe, I.; Alibert, Y.; Chabrier, G.; Benz, W. (2006). "Birth and fate of hot-Neptune planets". Astronomy and Astrophysics. 450 (3): 1221–1229. arXiv:astro-ph/0512091. Bibcode:2006A&A...450.1221B. doi:10.1051/0004-6361:20054040. S2CID 15574680.
  25. Agnew, Matthew T; Maddison, Sarah T; Horner, Jonathan; Kane, Stephen R (June 2019). "Predicting multiple planet stability and habitable zone companions in the TESS era". Monthly Notices of the Royal Astronomical Society. 485 (4): 4703–4725. arXiv:1901.11297. doi:10.1093/mnras/stz345.
  26. ^ Goździewski, Krzysztof (September 2022). "The orbital architecture and stability of the μ Arae planetary system". Monthly Notices of the Royal Astronomical Society. 516 (4): 6096–6115. arXiv:2209.04542. doi:10.1093/mnras/stac2584.
  27. Schütz, O.; Bönhardt, H.; Pantin, E.; Sterzik, M.; Els, S.; Hahn, J.; Henning, Th. (2004). "A search for circumstellar dust disks with ADONIS". Astronomy and Astrophysics. 424 (2): 613–618. arXiv:astro-ph/0408530. Bibcode:2004A&A...424..613S. doi:10.1051/0004-6361:20034215. S2CID 25921357.
  28. Canup, R.; Ward, W. (2006). "A common mass scaling for satellite systems of gaseous planets". Nature. 441 (7095): 834–839. Bibcode:2006Natur.441..834C. doi:10.1038/nature04860. PMID 16778883. S2CID 4327454.
  29. Buccino, A.; Lemarchand, Guillermo A.; Mauas, Pablo J.D. (2006). "Ultraviolet Radiation Constraints around the Circumstellar Habitable Zones". Icarus. 183 (2): 491–503. arXiv:astro-ph/0512291. Bibcode:2006Icar..183..491B. doi:10.1016/j.icarus.2006.03.007. S2CID 2241081.

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