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Coordinates: Sky map 17h 44m 08.7s, −51° 50′ 03″
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{{Short description|Extrasolar planet orbiting Mu Arae in the constellation of Ara}}

{{Infobox planet
{{Planetbox begin
| name = Mu Arae c
| name = Mu Arae c / Dulcinea
⚫
<!-- DISCOVERY -->| discoverer = [[Nuño Santos|Santos]], [[François Bouchy|Bouchy]]<br/> [[Michel Mayor|Mayor]], [[Francesco Pepe|Pepe]]
}}
⚫
| discovery_site = [[La Silla Observatory]], [[Chile]]
{{Planetbox star
⚫
| discovered = August 25, 2004<ref name="eso0427"/>
⚫
| discovery_method = [[HARPS]]
<!-- DESIGNATIONS -->
<!-- ORBITAL -->| apsis = astron
| aphelion = {{convert|0.10659|AU|e6km|abbr=unit}}
| perihelion = {{convert|0.07529|AU|e6km|abbr=unit}}
⚫
| semimajor = {{convert|0.09094|AU|e6km|abbr=unit}}<ref name="pepe07">{{cite journal|bibcode=2007A&A...462..769P|title=The HARPS search for southern extra-solar planets. VIII. μ Arae, a system with four planets|author=Pepe, F. |display-authors=4 |author2=Correia, A. C. M. |author3=Mayor, M. |author4=Tamuz, O. |author5=Couetdic, J. |author6=Benz, W. |author7=Bertaux, J.-L. |author8=Bouchy, F. |author9=Laskar, J. |author10=Lovis, C. |author11=Naef, D. |author12=Queloz, D. |author13=Santos, N. C. |author14=Sivan, J.-P. |author15=Sosnowska, D. |author16=Udry, S.|journal=[[Astronomy and Astrophysics]]|volume=462|issue=2|date=2007|pages=769–776|doi=10.1051/0004-6361:20066194|arxiv = astro-ph/0608396 |s2cid=59157984 }}</ref>
⚫
| eccentricity = 0.172 ± 0.040<ref name="pepe07"/>
⚫
| period = 9.6386 ± 0.0015<ref name="pepe07"/> [[day|d]]<br>0.02639 [[year|y]]
⚫
| time_periastron = 2,452,991.1 ± 0.4<ref name="pepe07"/>
⚫
| arg_peri = 212.7 ± 13.3<ref name="pepe07"/>
⚫
| semi-amplitude = 3.06 ± 0.13<ref name="pepe07"/>
| star = [[Mu Arae]]
| star = [[Mu Arae]]
<!-- PHYS CHARS -->
| constell = [[Ara (constellation)|Ara]]
<!-- ATMOSPHERE -->
| RA = {{RA|17|44|08.7}}
<!-- NOTES -->}}
| DEC = {{DEC|−51|50|03}}
⚫
'''Mu Arae c''', also known as '''HD 160691 c''', formally named '''Dulcinea''' (pronounced {{IPAc-en|d|V|l|'|s|I|n|i|@}} or {{IPAc-en|d|V|l|s|I|'|n|iː|@}}),<ref>{{OED|Dulcinea}}</ref> is an [[extrasolar planet]] orbiting the [[star]] [[Mu Arae]] of the [[constellation]] [[Ara (constellation)|Ara]]. It was the first '[[hot Neptune]]' to be discovered.
| app_mag = 5.15
| dist_ly=50.6 ± 0.2
| dist_pc=15.51 ± 0.07
| class = G3IV–V
| mass = 1.10 ± 0.01
| radius = 1.36 ± 0.01
| temperature = 5820 ± 40
| metallicity = 0.30 ± 0.01
| age = 6.34 ± 0.40
}}
{{Planetbox orbit
⚫
| semimajor = 0.09094<ref name="pepe07">{{cite journal|bibcode=2007A&A...462..769P|title=The HARPS search for southern extra-solar planets. VIII. μ Arae, a system with four planets|author=Pepe, F. |display-authors=4 |author2=Correia, A. C. M. |author3=Mayor, M. |author4=Tamuz, O. |author5=Couetdic, J. |author6=Benz, W. |author7=Bertaux, J.-L. |author8=Bouchy, F. |author9=Laskar, J. |author10=Lovis, C. |author11=Naef, D. |author12=Queloz, D. |author13=Santos, N. C. |author14=Sivan, J.-P. |author15=Sosnowska, D. |author16=Udry, S.|journal=[[Astronomy and Astrophysics]]|volume=462|issue=2|date=2007|pages=769–776|doi=10.1051/0004-6361:20066194|arxiv = astro-ph/0608396 }}</ref>
| semimajor_gm = 13.605
| periastron = 0.07529
| periastron_gm = 11.264
| apastron = 0.10659
| apastron_gm = 15.946
⚫
| eccentricity = 0.172 ± 0.040<ref name="pepe07" />
⚫
| period = 9.6386 ± 0.0015<ref name="pepe07" />
| period_year = 0.02639
⚫
| arg_peri = 212.7 ± 13.3<ref name="pepe07" />
⚫
| t_peri = 2452991.1 ± 0.4<ref name="pepe07" />
⚫
| semi-amp = 3.06 ± 0.13<ref name="pepe07" />
}}
{{Planetbox character
| minimum_mass = 0.03321<ref name="pepe07" />
| minimum_mass_earth = 10.55
}}
{{Planetbox discovery
⚫
| discovery_date = August 25, 2004<ref name="eso0427"/>
⚫
| discovery_site=[[La Silla Observatory]], [[Chile]]
⚫
| discovery_method = [[HARPS]]
⚫
| discoverers = [[Nuño Santos|Santos]], [[François Bouchy|Bouchy]]<br /> [[Michel Mayor|Mayor]], [[Francesco Pepe|Pepe]]
| discovery_status=Published
}}
{{Planetbox catalog
| names = Dulcinea, HD 160691 c
}}
{{Planetbox reference
| star = HD+160691
}}
{{Planetbox end}}


⚫
None of the four planets orbiting Mu Arae are directly visible from Earth using currently available tools. All four were found using the [[radial velocity]] method of extrasolar planet detection.
⚫
'''Mu Arae c''', also known as '''HD 160691 c''', later named '''Dulcinea''', is an [[extrasolar planet]] orbiting the [[star]] [[Mu Arae]] of the constellation [[Ara (constellation)|Ara]]. It was the first '[[hot Neptune]]' or '[[mega-Earth]]' to be discovered.


==Discovery==
⚫
In July 2014 the [[International Astronomical Union]] launched 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>[http://nameexoworlds.iau.org/process NameExoWorlds The Process]</ref> In December 2015, the IAU announced the winning name was Dulcinea for this planet.<ref>[http://www.iau.org/news/pressreleases/detail/iau1514/ Final Results of NameExoWorlds Public Vote Released], International Astronomical Union, 15 December 2015.</ref> The winning name was submitted by the Planetario de Pamplona, [[Spain]]. [[Dulcinea del Toboso|Dulcinea]] was the love-interest of the lead character of the novel ''[[Don Quixote|El Ingenioso Hidalgo Don Quixote de la Mancha]]''.<ref>[http://nameexoworlds.iau.org/names NameExoWorlds The Approved Names]</ref>
⚫
The planet's discovery was announced on August 25, 2004.<ref name="eso0427"/> At the time, its minimum mass was reported at just 14 times that of [[Earth (planet)|Earth]],<ref name=harps>{{cite journal | title=A 14 Earth-masses exoplanet around μ Arae | author=N.C. Santos |author2=F. Bouchy |author3=M. Mayor |author3-link=Michel Mayor |author4=F. Pepe |author5=D. Queloz |author5-link=Didier Queloz |author6=S. Udry |author6-link=Stéphane Udry |author7=C. Lovis |author8=M. Bazot |author9=W. Benz |author10=J.-L. Bertaux |author11=G. Lo Curto |author12=X. Delfosse |author13=C. Mordasini |author14=D. Naef |author15=J.-P. Sivan |author16=S. Vauclair |name-list-style=amp | doi=10.1051/0004-6361:200400076 | date=2004 | journal=Astronomy and Astrophysics | volume=426 | pages=L19–L23 | arxiv=astro-ph/0408471|bibcode = 2004A&A...426L..19S | s2cid=14938593 }}</ref> although later work established a value of 10.5 Earth masses.<ref name=harps2>{{cite journal | title=μ Ara, a system with four planets | author=F. Pepe |author2=A.C.M. Correia |author3=M. Mayor |author3-link=Michel Mayor |author4=O. Tamuz |author5=W. Benz |author6=J.-L. Bertaux |author7=F. Bouchy |author8=J. Couetdic |author9=J. Laskar |author10=C. Lovis |author11=D. Naef |author12=D. Queloz |author12-link=Didier Queloz |author13=N. C. Santos |author14=J.-P. Sivan |author15=D. Sosnowska |author16=S. Udry |author16-link=Stéphane Udry |name-list-style=amp | doi=10.1051/0004-6361:20066194 | date=2007 | journal=Astronomy and Astrophysics | volume=462 | issue=2 | pages=769–776 | arxiv=astro-ph/0608396|bibcode = 2007A&A...462..769P | s2cid=59157984 }}</ref> It orbits very close to [[Mu Arae]], completing one revolution every 9.6 days. The discovery was made with the aid of the [[High Accuracy Radial Velocity Planet Searcher]] (HARPS) [[spectrograph]], at the [[European Southern Observatory]]'s [[La Silla Observatory]] in [[Chile]]. The data that revealed the presence of this planet was gathered on 8 nights of observations in June 2004.


==Name==
⚫
The planet's discovery was announced on August 25, 2004.<ref name="eso0427"/> At the time, its minimum mass was reported at just 14 times that of [[Earth (planet)|Earth]],<ref name=harps>{{cite journal | title=A 14 Earth-masses exoplanet around μ Arae | author=N.C. Santos |author2=F. Bouchy |author3=[[Michel Mayor|M. Mayor]], F. Pepe, [[Didier Queloz|D. Queloz]], [[Stéphane Udry|S. Udry]], C. Lovis, M. Bazot, W. Benz, J.-L. Bertaux, G. Lo Curto, X. Delfosse, C. Mordasini, D. Naef, J.-P. Sivan, and S. Vauclair | doi=10.1051/0004-6361:200400076 | date=2004 | journal=Astronomy and Astrophysics | volume=426 | pages=L19–L23 | arxiv=astro-ph/0408471|bibcode = 2004A&A...426L..19S }}</ref> although later work established a value of 10.5 Earth masses.<ref name=harps2>{{cite journal | title=μ Ara, a system with four planets | author=F. Pepe |author2=A.C.M. Correia |author3=[[Michel Mayor|M. Mayor]], O. Tamuz, W. Benz, J.-L. Bertaux, F. Bouchy, J. Couetdic, J. Laskar, C. Lovis, D. Naef, [[Didier Queloz|D. Queloz]], N. C. Santos, J.-P. Sivan, D. Sosnowska, and [[Stéphane Udry|S. Udry]] | doi=10.1051/0004-6361:20066194 | date=2007 | journal=Astronomy and Astrophysics | volume=462 | issue=2 | pages=769–776 | arxiv=astro-ph/0608396|bibcode = 2007A&A...462..769P }}</ref> It orbits very close to [[Mu Arae]], completing one revolution every 9.6 days. The discovery was made with the aid of the [[High Accuracy Radial Velocity Planet Searcher]] (HARPS) [[spectrograph]], at the [[European Southern Observatory]]'s [[La Silla Observatory]] in [[Chile]]. The data that revealed the presence of this planet was gathered on 8 nights of observations in June 2004.
⚫
In July 2014 the [[International Astronomical Union]] (IAU) 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=2015-09-05 |archive-date=2015-08-15 |archive-url=https://web.archive.org/web/20150815025117/http://nameexoworlds.iau.org/process |url-status=dead }}</ref> In December 2015, the IAU announced the winning name was Dulcinea for this planet.<ref>[http://www.iau.org/news/pressreleases/detail/iau1514/ Final Results of NameExoWorlds Public Vote Released], International Astronomical Union, 15 December 2015.</ref> The winning name was submitted by the Planetario de Pamplona, [[Spain]]. [[Dulcinea del Toboso|Dulcinea]] was the love interest of the lead character of the novel ''[[Don Quixote]]''.<ref>{{Cite web |url=http://nameexoworlds.iau.org/names |title=NameExoWorlds The Approved Names |access-date=2016-01-03 |archive-date=2018-02-01 |archive-url=https://web.archive.org/web/20180201043609/http://nameexoworlds.iau.org/names |url-status=dead }}</ref>


==Characteristics==
Assuming its true mass is comparable to those of [[Neptune]] and [[Gliese 436 b]], 14 Earth masses is theoretically the maximum size for a terrestrial planet. A rocky planet this size could certainly have formed, since Mu Arae has a higher [[metallicity]] than our Sun. Also, it is thought to have formed well inside the system's "snow line" at 3.2 AU.<ref name=harps /> However, various models of the system's formation have since converged that the planet attracted large amounts of volatiles before its star had cleared out the ice, and that it now has a core of only 6 Earth masses.<ref name=baraffe>{{cite journal | title=Birth and fate of hot-Neptune planets| author=I. Baraffe |author2=Y. Alibert |author3=G. Chabrier |author4= W. Benz | date=2005 | doi=10.1051/0004-6361:20054040 | journal=Astronomy and Astrophysics | volume=450 | issue=3 | pages=1221–1229 |arxiv=astro-ph/0512091|bibcode = 2006A&A...450.1221B }}</ref> Its core is likely enveloped in so much hot-ice and gas that the planet would behave more like Neptune.
Assuming its true mass is comparable to those of [[Neptune]] and [[Gliese 436 b]], the authors of the discovery paper speculated that Mu Arae c could be a [[terrestrial planet]], though they expect a gaseous envelope to compose 5-10% of its mass. A rocky planet this size could possibly have formed, since Mu Arae has a higher [[metallicity]] than the Sun. Also, it is thought to have formed well inside the system's "snow line" at 3.2 AU.<ref name=harps/> However, various models of the system's formation have since converged that the planet attracted large amounts of volatiles before its star had cleared out the ice, and that it now has a core of only six Earth masses.<ref name=baraffe>{{cite journal | title=Birth and fate of hot-Neptune planets| author=I. Baraffe |author2=Y. Alibert |author3=G. Chabrier |author4= W. Benz | date=2005 | doi=10.1051/0004-6361:20054040 | journal=Astronomy and Astrophysics | volume=450 | issue=3 | pages=1221–1229 |arxiv=astro-ph/0512091|bibcode = 2006A&A...450.1221B | s2cid=15574680 }}</ref> Its core is likely enveloped in so much [[hot ice]] and gas that the planet would behave more like Neptune. Indeed, it is now understood that planets this massive are rarely rocky.<ref name="ChenKipping2017">{{cite journal |arxiv=1603.08614|doi=10.3847/1538-4357/834/1/17 |title=Probabilistic Forecasting of the Masses and Radii of Other Worlds |year=2017 |last1=Chen |first1=Jingjing |last2=Kipping |first2=David |journal=The Astrophysical Journal |volume=834 |issue=1 |page=17 |s2cid=119114880 |bibcode=2017ApJ...834...17C |doi-access=free }}</ref>


Mu Arae c is too far from its sun to be subject to [[coronal mass ejections]]. There is disagreement as to whether it is and has always been a [[hot Neptune]] in mass (Lammer),<ref>{{cite journal | journal=Geophysical Research Abstracts | volume=9| issue=07850 |date=2007 | url=http://www.cosis.net/abstracts/EGU2007/07850/EGU2007-J-07850.pdf?PHPSESSID=1eb3a7a98603083dda25d18001ea2a33 | title=The impact of nonthermal loss processes on planet masses from Neptunes to Jupiters |author=H. Lammer|display-authors=etal}} The 0.09 AU sub-Jup is there called "HD160691d",</ref> or if it could have developed from a gas giant, losing most of its mass on the way (Baraffe).
Mu Arae c is too far from its star to be subject to [[coronal mass ejections]]. There is disagreement as to whether it is and has always been a [[hot Neptune]] in mass (Lammer),<ref>{{cite journal | journal=Geophysical Research Abstracts | volume=9| issue=7850 |date=2007 | url=http://www.cosis.net/abstracts/EGU2007/07850/EGU2007-J-07850.pdf?PHPSESSID=1eb3a7a98603083dda25d18001ea2a33 | title=The impact of nonthermal loss processes on planet masses from Neptunes to Jupiters |author=H. Lammer|display-authors=etal}} The 0.09 AU sub-Jup is there called "HD160691d",</ref> or if it could have developed from a gas giant, losing most of its mass on the way (Baraffe).


If an eroded gas giant, the sun would have boiled the planet from a larger protoplanet, of 20 Earth masses up to half Jupiter's mass. If the latter, its current radius could be as high as 0.6 Jupiter.<ref name=baraffe />
If an eroded gas giant, the star would have boiled the planet from a larger protoplanet, of 20 Earth masses up to half [[Jupiter mass|Jupiter's mass]]. If the latter, its current radius could be as high as 0.6 Jupiter.<ref name=baraffe/>


The planet must be hot because of its proximity to its star. The discoverers chose for it an albedo of 0.35, lighter than albedos chosen to calculate the temperatures of [[hot Jupiter]]s such as [[tau Boötis b]]. This was perhaps due to the discoverers' assumption that the planet would be a silicate super-terrestrial with neither clouds nor a deep Rayleigh-scattering atmosphere. If so the surface temperature would be about 900 [[Kelvin|K]].<ref name=harps />
The planet must be hot because of its proximity to its star. The discoverers chose for it an [[albedo]] of 0.35, lighter than albedos chosen to calculate the temperatures of [[hot Jupiter]]s such as [[Tau Boötis b]]. This was perhaps due to the discoverers' assumption that the planet would be a silicate super-terrestrial with neither clouds nor a deep [[Rayleigh scattering]] atmosphere. If so the surface temperature would be about {{Val|900|ul=K}}.<ref name=harps/>

⚫
None of the four planets orbiting Mu Arae are directly visible from Earth using currently available tools. All four were found using the [[radial velocity]] method of extrasolar planet detection.


== See also ==
== See also ==
Line 72: Line 44:


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


<ref name="eso0427">{{cite press release | title=Fourteen Times the Earth | date=August 25, 2004 | publisher=[[European Southern Observatory]] | location=Garching, Germany | url=http://www.eso.org/public/news/eso0427/ | accessdate=December 31, 2012 }}</ref>
<ref name="eso0427">{{cite press release | title=Fourteen Times the Earth | date=August 25, 2004 | publisher=[[European Southern Observatory]] | location=Garching, Germany | url=http://www.eso.org/public/news/eso0427/ | accessdate=December 31, 2012 }}</ref>

}}
}}


{{Mu Arae}}
{{Mu Arae}}
{{Stars of Ara}}


{{Sky|17|44|08.7|-|51|50|03|49.8}}
{{Sky|17|44|08.7|-|51|50|03|49.8}}
{{Nearest bright star systems|5.}}


{{DEFAULTSORT:Mu Arae c}}
[[Category:Ara (constellation)]]
[[Category:Ara (constellation)]]
⚫
[[Category:Exoplanets]]
[[Category:Super-Earths]]
[[Category:Terrestrial planets]]
[[Category:Exoplanets discovered in 2004]]
[[Category:Exoplanets discovered in 2004]]
[[Category:Exoplanets detected by radial velocity]]
[[Category:Exoplanets detected by radial velocity]]
[[Category:Hot Neptunes]]
[[Category:Hot Neptunes]]
[[Category:Exoplanets with proper names]]
⚫
[[Category:Mu Arae]]

Latest revision as of 13:26, 26 November 2023

Mu Arae c / Dulcinea
Discovery
Discovered bySantos, Bouchy
Mayor, Pepe
Discovery siteLa Silla Observatory, Chile
Discovery dateAugust 25, 2004[1]
HARPS
Orbital characteristics
Apastron0.10659 AU (15.946 million km)
Periastron0.07529 AU (11.263 million km)
0.09094 AU (13.604 million km)[2]
Eccentricity0.172 ± 0.040[2]
9.6386 ± 0.0015[2] d
0.02639 y
2,452,991.1 ± 0.4[2]
212.7 ± 13.3[2]
Semi-amplitude3.06 ± 0.13[2]
StarMu Arae

Mu Arae c, also known as HD 160691 c, formally named Dulcinea (pronounced /dʌlˈsɪniə/ or /dʌlsɪˈniːə/),[3] is an extrasolar planet orbiting the star Mu Arae of the constellation Ara. It was the first 'hot Neptune' to be discovered.

None of the four planets orbiting Mu Arae are directly visible from Earth using currently available tools. All four were found using the radial velocity method of extrasolar planet detection.

Discovery

[edit]

The planet's discovery was announced on August 25, 2004.[1] At the time, its minimum mass was reported at just 14 times that of Earth,[4] although later work established a value of 10.5 Earth masses.[5] It orbits very close to Mu Arae, completing one revolution every 9.6 days. The discovery was made with the aid of the High Accuracy Radial Velocity Planet Searcher (HARPS) spectrograph, at the European Southern Observatory's La Silla Observatory in Chile. The data that revealed the presence of this planet was gathered on 8 nights of observations in June 2004.

Name

[edit]

In July 2014 the International Astronomical Union (IAU) launched NameExoWorlds, a process for giving proper names to certain exoplanets and their host stars.[6] The process involved public nomination and voting for the new names.[7] In December 2015, the IAU announced the winning name was Dulcinea for this planet.[8] The winning name was submitted by the Planetario de Pamplona, Spain. Dulcinea was the love interest of the lead character of the novel Don Quixote.[9]

Characteristics

[edit]

Assuming its true mass is comparable to those of Neptune and Gliese 436 b, the authors of the discovery paper speculated that Mu Arae c could be a terrestrial planet, though they expect a gaseous envelope to compose 5-10% of its mass. A rocky planet this size could possibly have formed, since Mu Arae has a higher metallicity than the Sun. Also, it is thought to have formed well inside the system's "snow line" at 3.2 AU.[4] However, various models of the system's formation have since converged that the planet attracted large amounts of volatiles before its star had cleared out the ice, and that it now has a core of only six Earth masses.[10] Its core is likely enveloped in so much hot ice and gas that the planet would behave more like Neptune. Indeed, it is now understood that planets this massive are rarely rocky.[11]

Mu Arae c is too far from its star to be subject to coronal mass ejections. There is disagreement as to whether it is and has always been a hot Neptune in mass (Lammer),[12] or if it could have developed from a gas giant, losing most of its mass on the way (Baraffe).

If an eroded gas giant, the star would have boiled the planet from a larger protoplanet, of 20 Earth masses up to half Jupiter's mass. If the latter, its current radius could be as high as 0.6 Jupiter.[10]

The planet must be hot because of its proximity to its star. The discoverers chose for it an albedo of 0.35, lighter than albedos chosen to calculate the temperatures of hot Jupiters such as Tau Boötis b. This was perhaps due to the discoverers' assumption that the planet would be a silicate super-terrestrial with neither clouds nor a deep Rayleigh scattering atmosphere. If so the surface temperature would be about 900 K.[4]

See also

[edit]

References

[edit]
  1. ^ a b "Fourteen Times the Earth" (Press release). Garching, Germany: European Southern Observatory. August 25, 2004. Retrieved December 31, 2012.
  2. ^ a b c d e f Pepe, F.; Correia, A. C. M.; Mayor, M.; Tamuz, O.; et al. (2007). "The HARPS search for southern extra-solar planets. VIII. μ Arae, 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 59157984.
  3. ^ "Dulcinea". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
  4. ^ a b c N.C. Santos; F. Bouchy; M. Mayor; F. Pepe; D. Queloz; S. Udry; C. Lovis; M. Bazot; W. Benz; J.-L. Bertaux; G. Lo Curto; X. Delfosse; C. Mordasini; D. Naef; J.-P. Sivan & S. Vauclair (2004). "A 14 Earth-masses exoplanet around μ Arae". Astronomy and Astrophysics. 426: L19–L23. arXiv:astro-ph/0408471. Bibcode:2004A&A...426L..19S. doi:10.1051/0004-6361:200400076. S2CID 14938593.
  5. ^ F. Pepe; A.C.M. Correia; M. Mayor; O. Tamuz; W. Benz; J.-L. Bertaux; F. Bouchy; J. Couetdic; J. Laskar; C. Lovis; D. Naef; D. Queloz; N. C. Santos; J.-P. Sivan; D. Sosnowska & S. Udry (2007). "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 59157984.
  6. ^ NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars. IAU.org. 9 July 2014
  7. ^ "NameExoWorlds The Process". Archived from the original on 2015-08-15. Retrieved 2015-09-05.
  8. ^ Final Results of NameExoWorlds Public Vote Released, International Astronomical Union, 15 December 2015.
  9. ^ "NameExoWorlds The Approved Names". Archived from the original on 2018-02-01. Retrieved 2016-01-03.
  10. ^ a b I. Baraffe; Y. Alibert; G. Chabrier; W. Benz (2005). "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.
  11. ^ Chen, Jingjing; Kipping, David (2017). "Probabilistic Forecasting of the Masses and Radii of Other Worlds". The Astrophysical Journal. 834 (1): 17. arXiv:1603.08614. Bibcode:2017ApJ...834...17C. doi:10.3847/1538-4357/834/1/17. S2CID 119114880.
  12. ^ H. Lammer; et al. (2007). "The impact of nonthermal loss processes on planet masses from Neptunes to Jupiters" (PDF). Geophysical Research Abstracts. 9 (7850). The 0.09 AU sub-Jup is there called "HD160691d",


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