View source for Mu Arae

{{Short description|Star in the constellation Ara}}
{{Use dmy dates|date=April 2021}}
{{Starbox begin
 | name=Mu Arae / Cervantes
}}
{{Starbox image
 | image = 
{{Location mark
 | image=Ara IAU.svg
 | alt= | float=center | width=240
 | label= | position=right
 | mark=Red circle.svg | mark_width=10 | mark_link=μ Arae
 | x%=44.5 | y%=38.6
}}
 | caption = The location of μ Arae (circled)
}}
{{Starbox observe
 | epoch       = J2000.0
 | constell    = [[Ara (constellation)|Ara]]
 | ra          = {{RA|17|44|08.70314}}<ref name=GaiaDR3/>
 | dec         = {{DEC|−51|50|02.5916}}<ref name=GaiaDR3/>
 | appmag_v    = 5.15<ref name="Benedict2022"/>
}}
{{Starbox character
 | class       = G3IV–V<ref name=aj132_1_161/>
 | appmag_1_passband = V
 | appmag_1    = {{val|5.15|0.01}}<ref name="Benedict2022"/>
 | appmag_2_passband = G
 | appmag_2    = {{val|4.943|0.003}}<ref name=GaiaDR3/>
 | appmag_3_passband = K
 | appmag_3    = {{val|3.68|0.25}}<ref name="Benedict2022"/>
 | b-v         = +0.70<ref name=ibsh8_30/>
 | u-b         = +0.24<ref name=ibsh8_30/>
 | r-i         = 
 | v-k         = {{val|1.47|0.25}}<ref name="Benedict2022"/>
 | variable    =
}}
{{Starbox astrometry
 | radial_v    = {{val|−9.54|0.13}}<ref name=GaiaDR3/>
 | prop_mo_ra  = {{val|−15.034}}
 | prop_mo_dec = {{val|−190.901}}
 | pm_footnote = <ref name=GaiaDR3/>
 | parallax    = 64.0853
 | p_error     = 0.0904
 | parallax_footnote = <ref name=GaiaDR3/>
 | absmag_v    = +4.17<ref name=Anderson2012/>
}}
{{Starbox detail
 | age_gyr     = {{val|6.34|0.40}}<ref name="soriano2009"/>
 | metal       = {{val|200|5|s=%}}<ref name="soriano2009" /><ref group="note">From [Fe/H] = 0.30 ± 0.01</ref>
 | metal_fe    = {{val|0.29|0.01}}<ref name="Soubiran2024"/>
 | mass        = {{val|1.10|0.01}}<ref name="soriano2009" />
 | radius      = {{val|1.280|0.025}}<ref name="Soubiran2024"/>
 | rotation    = 
 | rotational_velocity = {{val|3.1|0.5}}<ref name="Benedict2022"/>
 | gravity     = {{val|4.30|0.03}}<ref name="Soubiran2024"/>
 | luminosity  = {{val|1.879|0.019}}<ref name="Soubiran2024"/>
 | temperature = {{val|5974|61|fmt=commas}}<ref name="Soubiran2024"/>
}}
{{Starbox catalog
 | names = {{odlist | name=Cervantes | B=μ Arae | CD=−51°11094 | FK5=662 | GC=24024 | GJ=691 | HD=160691 | HIP=86796 | HR=6585 | SAO=244981 | PPM=346258 | LTT=7053 }}<ref name=SIMBAD/>
}}
{{Starbox reference
 | Simbad = *+mu+Ara
 | ARICNS = 01434
 | NSTED = HD-160691
}}
{{Starbox end}}

'''Mu Arae''' is a single [[star]] with a [[planetary system]] in the [[constellation]] of [[Ara (constellation)|Ara]]. Its name is a [[Bayer designation]] that is [[Romanization of Greek|Latinized]] from '''μ Arae''', and abbreviated '''Mu Ara''' or '''μ Ara'''. This star is officially named '''Cervantes''', pronounced  {{IPAc-en|s|ɜːr|'|v|æ|n|t|iː|z}} or {{respell|sur|VAN|teez}},<ref name="IAU-CSN"/> and is often designated '''HD&nbsp;160691'''. With an [[apparent visual magnitude]] of 5.15,<ref name="Benedict2022"/> it is faintly visible to the [[naked eye]]. Based on [[stellar parallax|parallax]] measurements it is located approximately {{convert|51|ly|pc|abbr=out|lk=on}} away from the [[Sun]].<ref name=GaiaDR3/> It is drifting closer with a [[radial velocity]] of −10&nbsp;km/s.<ref name=GaiaDR3/>

Cervantes is similar to the Sun, but is older, 10% more massive, and slightly [[stellar evolution|evolved]]. It has four known [[Exoplanet|extrasolar planets]] designated [[Mu Arae b]], [[Mu Arae c|c]], [[Mu Arae d|d]] and [[Mu Arae e|e]]; later named Quijote, Dulcinea, Rocinante and Sancho, respectively. Three of them have masses comparable with that of [[Jupiter]]. Mu Arae c, the innermost, was the first [[hot Neptune]] or [[super-Earth]] discovered.

== Nomenclature ==

''μ Arae'' ([[Latinisation of names|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 [[Latin alphabet|Roman letters]] starting from "b", in order of discovery.<ref name="planetnaming"/> This system was used by a team led by [[Krzysztof Goździewski]].<ref name="gozdziewski"/> 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.<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 [[International Astronomical Union]] has not defined an official system for designations of extrasolar planets,<ref name=IAU_2006/> 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]].<ref name=Short_et_al_2008/><ref name=exoplanet/>

In July 2014 the [[International Astronomical Union]] launched [[NameExoWorlds]], a process for giving proper names to certain exoplanets and their host stars.<ref>[http://www.iau.org/news/pressreleases/detail/iau1404/ NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars]. 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>[http://www.iau.org/news/pressreleases/detail/iau1514/ Final Results of NameExoWorlds Public Vote Released], 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=[[International Astronomical Union]] |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. [[Miguel de Cervantes]] Saavedra (1547–1616) was a famous Spanish writer and author of ''[[Don Quixote|El Ingenioso Hidalgo Don Quixote de la Mancha]]''. The planets are named after characters of that novel: Quijote was the lead character; [[Dulcinea del Toboso|Dulcinea]] his love interest; [[Rocinante]] his horse, and [[Sancho Panza|Sancho]] his [[squire]].<ref>[http://www.nameexoworlds.iau.org/approved-names#comp-jwdpj57w NameExoWorlds The Approved Names]</ref>

In 2016, the IAU organized a [[IAU Working Group on Star Names|Working Group on Star Names]] (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 ==

According to measurements made by the [[Gaia (spacecraft)|Gaia]] [[astrometry|astrometric]] [[satellite]], Mu Arae exhibits a [[parallax]] of 64.0853 [[Minute of arc|milliarcsecond]]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 [[apparent magnitude]] of +5.15 and is thus visible to the [[naked eye]].

[[Asteroseismology|Asteroseismic]] analysis of the star reveals it is approximately 10% more massive than the Sun and significantly older, at around 6.34&nbsp;billion years.<ref name="soriano2009" /> The radius of the star is 28% greater than that of the Sun and it is 90% more luminous.<ref name="Soubiran2024"/> 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]].<ref name="soriano2009" />

Mu Arae has a listed [[stellar classification|spectral type]] 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 [[subgiant]] stage of its evolution as it starts to run out of [[hydrogen]] in its core.{{dubious|reason=Sources for this star just call this a main sequence dwarf|Dwarf star?|date=April 2025}} This is reflected in its borderline [[luminosity class]], between IV (the subgiants) and V ([[main sequence]] [[dwarf star]]s like the Sun). This star has a low [[magnetic activity|chromospheric activity]] level and a low, non-variable [[Astrophysical X-ray source|X-ray luminosity]].<ref name="santos"/>

== Planetary system ==
[[File:Exoplanets of Cervantes.ogg|thumb|Emulation in [[Celestia]] of the exoplanets of Cervantes based in the [[Sudarsky's gas giant classification]]:  Dulcinea, Rocinante, Quijote y Sancho.]]
[[File:Mu Arae system.jpg|thumb|right|The Mu Arae star with distance relationships for its four planets]]
[[File:MuAraeOuterOrbits.svg|thumb|right|220px|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 [[eccentricity (orbit)|eccentric]] orbit of around 743 days.<ref name=Butler_2001/> The discovery was made by analysing variations in the star's [[radial velocity]] (measured by observing the [[Doppler shift]] of the star's [[spectral line]]s) 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.<ref name="McCarthy2004"/> 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 Neptune]]s" to be discovered. The discovery was made by making high-precision radial velocity measurements with the [[High Accuracy Radial Velocity Planet Searcher]] (HARPS) [[spectrograph]].<ref name="santos"/>

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.<ref name="gozdziewski"/><ref name="pepe"/> 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 [[planetary core|core]] of a gas giant which has had its outer layers stripped away by stellar radiation.<ref name=Baraffe_et_al_2006/> 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 [[orbital resonance]] which causes them to undergo strong interactions. The best-fit solution to the system is actually unstable:<ref name=Agnew_et_al_2019/><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 [[Gliese 876]] 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 [[orbital inclination|inclination]] of about 20°.<ref name="Goździewski2022"/>

[[Astrometry|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 {{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 [[circumstellar disc]]s 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.<ref name=Schütz_et_al_2004/>

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 [[natural satellite|moons]] of the gas giant could [[Habitable exomoon|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.<ref name=Canup_Ward_2006/> In addition, measurements of the star's [[ultraviolet]] [[flux]] suggest that any potentially [[planetary habitability|habitable]] planets or moons may not receive enough ultraviolet to trigger the formation of [[biomolecule]]s.<ref name="buccino"/> Planet "d" would receive a similar amount of ultraviolet to the Earth and thus lies in the [[Circumstellar_habitable_zone#Spectral_types_and_star-system_characteristics|ultraviolet habitable zone]]. However, it would be too hot for any moons to support surface liquid water.

{{OrbitboxPlanet begin
| table_ref = <ref name="Goździewski2022"/>
}}
{{OrbitboxPlanet
| exoplanet = [[Mu Arae c|c (Dulcinea)]]
| 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 = [[Mu Arae d|d (Rocinante)]]
| 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 = [[Mu Arae b|b (Quijote)]]
| 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 = [[Mu Arae e|e (Sancho)]]
| 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 ==
* [[55 Cancri]]
* [[Exoplanet]]
* [[Lists of exoplanets]]
* [[PSR B1257+12]]

== Notes ==
<references group="note" />

== References ==
{{Reflist|refs=

<ref name=SIMBAD>{{cite simbad | title=mu Ara | access-date=2025-04-29 }}</ref>

<ref name=GaiaDR3>{{Cite Gaia DR3|5945941905576552064}}</ref>

<ref name="Soubiran2024">{{Cite journal | display-authors=1 |last1=Soubiran |first1=C. |last2=Creevey |first2=O. L. |last3=Lagarde |first3=N. |last4=Brouillet |first4=N. |last5=Jofré |first5=P. |last6=Casamiquela |first6=L. |last7=Heiter |first7=U. |last8=Aguilera-Gómez |first8=C. |last9=Vitali |first9=S. |last10=Worley |first10=C. |last11=de Brito Silva |first11=D. |date=2024-02-01 |title=Gaia FGK benchmark stars: Fundamental Teff and log g of the third version |bibcode=2024A&A...682A.145S |journal=Astronomy and Astrophysics |volume=682 |pages=A145 |doi=10.1051/0004-6361/202347136 |arxiv=2310.11302 |issn=0004-6361}} [https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A%2BA/682/A145&HIP=HIP86796 Mu Arae's database entry] at [[VizieR]].</ref>

<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>

<ref name=Anderson2012>{{cite journal
 | 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| last=Feinstein | first=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>

<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>

<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=[[The Astronomical 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>

<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>

<ref name="soriano2009">{{cite journal|title=New seismic analysis of the exoplanet-host star Mu Arae|arxiv=0903.5475 | date=April 2010 |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>

<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>

<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 | display-authors=1 |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>

<ref name=Butler_2001>{{cite journal | display-authors=1 | 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>

<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=[[Astronomy and Astrophysics]]|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=1}}</ref>

<ref name=IAU_2006>{{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>

<ref name=Short_et_al_2008>{{cite journal|bibcode=2008MNRAS.386L..43S|title=New solutions for the planetary dynamics in HD160691 using a Newtonian model and latest data  | display-authors=1 | last1=Short | first1=D. | last2=Windmiller | first2=G. | last3=Orosz | first3=J. A. |journal=[[Monthly Notices of the Royal Astronomical Society|MNRAS]]|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 name=exoplanet>{{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=[[Extrasolar Planets Encyclopaedia]] |archive-date=22 December 2008 }}</ref>

<ref name="gozdziewski">{{Cite journal| last=Gozdziewski | first=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>

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}}

== External links ==
{{Commons category|Mu Arae}}
* [http://webviz.u-strasbg.fr/viz-bin/VizieR-S?GJ%20691 GJ 691]
* [http://webviz.u-strasbg.fr/viz-bin/VizieR-S?HR%206585 HR 6585]
* {{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=[[Space.com]] |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=[[European Southern Observatory]] |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 }}
* [http://aladin.u-strasbg.fr/AladinPreview?-c=17+44+08.7029-51+50+02.591&ident=LTT++7053&submit=Aladin+previewer Image Mu Arae]
* [http://www.lpl.arizona.edu/~rory/research/xsp/dynamics/ Extrasolar Planet Interactions] {{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}}
{{Stars of Ara}}
{{Sky|17|44|08.7|-|51|50|03|49.8}}

{{Good article}}
{{Authority control}}

{{DEFAULTSORT:Mu Arae}}
[[Category:Mu Arae| ]]
[[Category:G-type main-sequence stars]]
[[Category:G-type subgiants]]
[[Category:Planetary systems with four confirmed planets]]
[[Category:Ara (constellation)]]
[[Category:Bayer objects|Arae, Mu]]
[[Category:Bright Star Catalogue objects|6585]]
[[Category:Durchmusterung objects|CD-51 11094]]
[[Category:Gliese and GJ objects|0691]]
[[Category:Henry Draper Catalogue objects|160691]]
[[Category:Hipparcos objects|086796]]
[[Category:Stars with proper names|Cervantes]]