Mu Arae

Mu Arae (μ Arae, abbreviated Mu Ara, μ Ara), often designated HD 160691, officially named Cervantes /sɜːrˈvæntiːz/ sur-VAN-teez,[8] 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 to that of Jupiter. Mu Arae c, the innermost, was the first hot Neptune discovered.

Mu Arae

Mu Arae
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Ara
Right ascension  17h 44m 08.70114s[1]
Declination −51° 50′ 02.5853″[1]
Apparent magnitude (V) +5.12
Characteristics
Spectral type G3IV–V[2]
U−B color index +0.24[3]
B−V color index +0.70[3]
R−I color index 0.2
Astrometry
Radial velocity (Rv)−9.0[4] km/s
Proper motion (μ) RA: −16.85[1] mas/yr
Dec.: −190.60[1] mas/yr
Parallax (π)64.47 ± 0.31[1] mas
Distance50.6 ± 0.2 ly
(15.51 ± 0.07 pc)
Absolute magnitude (MV)+4.17[5]
Details
Mass1.10 ± 0.01[6] M☉
Radius1.36 ± 0.01[6] R☉
Luminosity1.90 ± 0.10[6] L☉
Surface gravity (log g)4.19[2] cgs
Temperature5820 ± 40[6] K
Metallicity200 ± 5%[6][note 1]
Metallicity [Fe/H]0.30 ± 0.01[6] dex
Rotation31 days
Rotational velocity (v sin i)1.4[7] km/s
Age6.34 ± 0.40[6] 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
Extrasolar Planets
Encyclopaedia		data

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.[9] This system was used by a team led by Krzysztof Goździewski.[10] 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.[11] 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,[12] the issue of which convention is 'correct' remains open, however 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.[13][14]

In July 2014 the International Astronomical Union launched a process for giving proper names to certain exoplanets and their host stars.[15] The process involved public nomination and voting for the new names.[16] 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).[17][18]

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.[19]

In 2016, the IAU organized a Working Group on Star Names (WGSN)[20] to catalog and standardize proper names for stars. In its first bulletin of July 2016,[21] 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.[8]

Stellar characteristics

According to measurements made by the Hipparcos astrometric satellite, Mu Arae exhibits a parallax of 64.47 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 50.6 light years (15.51 parsecs).[1][note 2] Seen from Earth it has an apparent magnitude of +5.12 and is 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.[6]

Mu Arae has a listed spectral type of G3IV–V.[2] 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
The Mu Arae star with distance relationships for its four planets
The orbits of the outer three planets in the Mu Arae system compared to 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.[22] 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.[23] Later in 2004, a small inner planet designated Mu Arae c was announced with a mass comparable to 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.[24]

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.[10][11] 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.[25] Alternatively it may have formed in the inner regions of the Mu Arae system as a rocky "super-Earth".[24] 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:[26] 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.[11] 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.[27]

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 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.[28] 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.[29] 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[11]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
c (Dulcinea) >0.03321 MJ 0.09094 9.6386 ± 0.0015 0.172 ± 0.04 — —
d (Rocinante) >0.5219 MJ 0.921 310.55 ± 0.83 0.0666 ± 0.0122 — —
b (Quijote) >1.676 MJ 1.497 643.25 ± 0.90 0.128 ± 0.017 — —
e (Sancho) >1.814 MJ 5.235 4205.8 ± 758.9 0.0985 ± 0.0627 — —
gollark: I wonder if anyone already made a C minifier.
gollark: If you write this and it's in a production system, you literally cannot be fired.
gollark: Also job security.
gollark: Suffering maximization, naturally.
gollark: C makes it quite easy to make particularly annoying and bad mistakes. With higher-level languages I can focus on cool™ higher-level mistakes.

See also
  • 55 Cancri
  • Extrasolar planet
  • List of extrasolar planets
  • PSR 1257+12

Notes
  1. From [Fe/H] = 0.30 ± 0.01
  2. The formula for converting parallax to distance is

References
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  2. 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.
  3. Feinstein, A. (1966). "Photoelectric observations of Southern late-type stars". The Information Bulletin for the Southern Hemisphere. 8: 30. Bibcode:1966IBSH....8...30F.
  4. Wielen, R.; et al. (1999). "Sixth Catalogue of Fundamental Stars (FK6). Part I. Basic fundamental stars with direct solutions". Veröff. Astron. Rechen-Inst. Heidelb. Astronomisches Rechen-Institut Heidelberg. 35 (35): 1. Bibcode:1999VeARI..35....1W.
  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.
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  7. Bruntt, H.; et al. (July 2010). "Accurate fundamental parameters for 23 bright solar-type stars". Monthly Notices of the Royal Astronomical Society. 405 (3): 1907–1923. arXiv:1002.4268. Bibcode:2010MNRAS.405.1907B. doi:10.1111/j.1365-2966.2010.16575.x.
  8. "IAU Catalog of Star Names". Retrieved 28 July 2016.
  9. 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 [astro-ph.SR].
  10. 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.
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  12. "Planets Around Other Stars". IAU. Archived from the original on 28 September 2006. Retrieved 16 September 2006.
  13. 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.
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  15. NameExoWorlds: An IAU Worldwide Contest to Name Exoplanets and their Host Stars. IAU.org. 9 July 2014
  16. NameExoWorlds The Process
  17. Final Results of NameExoWorlds Public Vote Released, International Astronomical Union, 15 December 2015.
  18. The Proposals page for Mu Arae, International Astronomical Union, 3 January 2016.
  19. NameExoWorlds The Approved Names
  20. "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  21. "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
  22. 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.
  23. 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.
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  25. 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.
  26. 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. doi:10.1093/mnras/stz345. Retrieved 28 April 2020.
  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.
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