Makemake

This article is about the dwarf planet. For the Rapa Nui god, see Makemake (deity). For other uses, see Makemake (disambiguation).
Makemake

Makemake as seen by the Hubble Space Telescope
Discovery
Discovered by
Discovery date March 31, 2005
Designations
MPC designation (136,472) Makemake
Pronunciation /ˌmækiˈmæki/, /ˌmɑːkiˈmɑːki/ or i/ˌmɑːkeɪˈmɑːkeɪ/[lower-alpha 1]
Named after
 Makemake
2005 FY9
Dwarf planet
cubewano[5]
scattered-near[lower-alpha 2]
Adjectives Makemakean
Orbital characteristics[6]
Epoch JD 2457000.5 (9 December 2014)
Aphelion 52.840 AU
Perihelion 38.590 AU
45.715 AU
Eccentricity 0.15586
309.09 yr (112,897 d)
4.419 km/s
156.353°
Inclination 29.00685°
79.3659°
297.240°
Physical characteristics
Dimensions
  • (1434 × 1422) ± 14 if viewed pole-on[7]
  • (1502±45) × (1430±9) km[8]
Mean radius
  • 715±7 km[7]
  • 739±17 km[8]
Flattening 0.05[lower-alpha 3]
17.0 (opposition)[11][12]
−0.3[6]

    Makemake (minor-planet designation 136472 Makemake) is a dwarf planet and perhaps the largest Kuiper belt object (KBO) in the classical population,[lower-alpha 2] with a diameter that is about 2/3 the size of Pluto.[17][18] Makemake has no known satellites, which makes it unique among the largest KBOs and means that its mass can only be estimated. Its extremely low average temperature, about 30 K (−243.2 °C), means its surface is covered with methane, ethane, and possibly nitrogen ices.[14]

    Makemake was discovered on March 31, 2005, by a team led by Michael E. Brown, and announced on July 29, 2005. Initially, it was known as 2005 FY9 and later given the minor-planet number 136472. Makemake was recognized as a dwarf planet by the International Astronomical Union (IAU) in July 2008.[18][19][20][21] Its name derives from Makemake in the mythology of the Rapa Nui people of Easter Island.[18]

    History

    Discovery

    Makemake was discovered on March 31, 2005, by a team at the Palomar Observatory, led by Michael E. Brown,[6] and was announced to the public on July 29, 2005. The team had planned to delay announcing their discoveries of the bright objects Makemake and Eris until further observations and calculations were complete, but announced them both on July 29 when the discovery of another large object they had been tracking, Haumea, was controversially announced on July 27 by a different team in Spain.[22]

    Despite its relative brightness (it is about a fifth as bright as Pluto),[lower-alpha 6] Makemake was not discovered until well after many much fainter Kuiper belt objects. Most searches for minor planets are conducted relatively close to the ecliptic (the region of the sky that the Sun, Moon and planets appear to lie in, as seen from Earth), due to the greater likelihood of finding objects there. It probably escaped detection during the earlier surveys due to its relatively high orbital inclination, and the fact that it was at its farthest distance from the ecliptic at the time of its discovery, in the northern constellation of Coma Berenices.[12]

    Besides Pluto, Makemake is the only other dwarf planet that was bright enough for Clyde Tombaugh to have possibly detected during his search for trans-Neptunian planets around 1930.[24] At the time of Tombaugh's survey, Makemake was only a few degrees from the ecliptic, near the border of Taurus and Auriga,[lower-alpha 7] at an apparent magnitude of 16.0.[12] This position, however, was also very near the Milky Way, and Makemake would have been almost impossible to find against the dense background of stars. Tombaugh continued searching for some years after the discovery of Pluto,[25] but he did not find Makemake or any other trans-Neptunian objects.

    Name

    The provisional designation 2005 FY9 was given to Makemake when the discovery was made public. Before that, the discovery team used the codename "Easterbunny" for the object, because of its discovery shortly after Easter.[1]

    In July 2008, in accordance with IAU rules for classical Kuiper belt objects, 2005 FY9 was given the name of a creator deity.[26] The name of Makemake, the creator of humanity and god of fertility in the mythos of the Rapa Nui, the native people of Easter Island,[20] was chosen in part to preserve the object's connection with Easter.[1]

    Orbit and classification

    Orbits of Makemake (blue), Haumea (green), contrasted with the orbit of Pluto (red) and the ecliptic (grey). The perihelia (q)[6] and the aphelia (Q) are marked with the dates of passage. The positions on April 2006 are marked with the spheres illustrating relative sizes and differences in albedo and colour.

    As of December 2015, Makemake is 52.4 AU (7.84×109 km) from the Sun,[11][12] almost as far from the Sun as it ever reaches on its orbit.[14] Makemake follows an orbit very similar to that of Haumea: highly inclined at 29° and a moderate eccentricity of about 0.16.[27] Nevertheless, Makemake's orbit is slightly farther from the Sun in terms of both the semi-major axis and perihelion. Its orbital period is nearly 310 years,[13] more than Pluto's 248 years and Haumea's 283 years. Both Makemake and Haumea are currently far from the ecliptic—the angular distance is almost 29°. Makemake is approaching its 2033 aphelion,[12] whereas Haumea passed its aphelion in early 1992.[28]

    Makemake is a classical Kuiper belt object,[5][lower-alpha 2] which means its orbit lies far enough from Neptune to remain stable over the age of the Solar System.[29][30] Unlike plutinos, which can cross Neptune's orbit due to their 2:3 resonance with the planet, the classical objects have perihelia further from the Sun, free from Neptune's perturbation.[29] Such objects have relatively low eccentricities (e below 0.2) and orbit the Sun in much the same way the planets do. Makemake, however, is a member of the "dynamically hot" class of classical KBOs, meaning that it has a high inclination compared to others in its population.[31] Makemake is, probably coincidentally, near the 11:6 resonance with Neptune.[32]

    Physical characteristics

    Brightness, size, and rotation

    Makemake (apmag 16.9)

    Makemake is currently visually the second-brightest Kuiper belt object after Pluto,[24] having a March opposition apparent magnitude of 17.0[11] in the constellation Coma Berenices.[12] This is bright enough to be visible using a high-end amateur telescope. Combining the detection in infrared by the Spitzer Space Telescope and Herschel Space Telescope with the similarities of spectrum with Pluto yielded an estimated diameter from 1,360 to 1,480 km.[17] From the 2011 stellar occultation by Makemake, its diameter has been measured to be (1502 ± 45) × (1430 ± 9) km. This is slightly larger than Haumea, making Makemake likely the third largest known trans-Neptunian object after Pluto and Eris.[27] Makemake was the fourth dwarf planet recognized, because it has a bright V-band absolute magnitude of −0.44.[6] Makemake has a high geometrical albedo of 0.81+0.01
    −0.02    .[7]

    Earth Moon Dysnomia Dysnomia Eris Eris Charon Charon Nix Nix Kerberos Kerberos Styx Styx Hydra Pluto Pluto Makemake Makemake Namaka Namaka Hi'iaka Hi'iaka Haumea Haumea Sedna Sedna 2007 OR10 2007 OR10 Weywot Weywot Quaoar Quaoar Vanth Vanth Orcus Orcus
    Artistic comparison of Pluto, Eris, Makemake, Haumea, Sedna, 2007 OR10, Quaoar, Orcus, and Earth along with the Moon.

    Spectra and surface

    In a letter written to the journal Astronomy and Astrophysics in 2006, Licandro and colleagues reported the measurements of the visible and near-infrared spectrum of Makemake. They used the William Herschel Telescope and Telescopio Nazionale Galileo and showed that the surface of Makemake resembles that of Pluto.[33] Like Pluto, Makemake appears red in the visible spectrum, and significantly redder than the surface of Eris (see colour comparison of TNOs).[33] The near-infrared spectrum is marked by the presence of the broad methane (CH4) absorption bands. Methane is observed also on Pluto and Eris, but its spectral signature is much weaker.[33]

    Spectral analysis of Makemake's surface revealed that methane must be present in the form of large grains at least one centimetre in size.[14] In addition, large amounts of ethane and tholins may be present as well, most likely created by photolysis of methane by solar radiation.[14] The tholins are probably responsible for the red color of the visible spectrum. Although evidence exists for the presence of nitrogen ice on its surface, at least mixed with other ices, there is nowhere near the same level of nitrogen as on Pluto and Triton, where it composes more than 98 percent of the crust. The relative lack of nitrogen ice suggests that its supply of nitrogen has somehow been depleted over the age of the Solar System.[14][34][35]

    The far-infrared (24–70 μm) and submillimeter (70–500 μm) photometry performed by Spitzer and Herschel telescopes revealed that the surface of Makemake is not homogeneous. Although the majority of it is covered by nitrogen and methane ices, where the albedo ranges from 78 to 90%, there are small patches of dark terrain whose albedo is only 2 to 12%, and that make up 3–7% of the surface.[17]

    Atmosphere

    Makemake was expected to have an atmosphere similar to that of Pluto but with a lower surface pressure. However, on 23 April 2011 Makemake passed in front of an 18th-magnitude star and abruptly blocked its light.[36] The results showed that Makemake presently lacks a substantial atmosphere and placed an upper limit of 4–12 nanobar on the pressure at its surface.[8]

    The presence of methane and possibly nitrogen suggests that Makemake could have a transient atmosphere similar to that of Pluto near its perihelion.[33] Nitrogen, if present, will be the dominant component of it.[14] The existence of an atmosphere also provides a natural explanation for the nitrogen depletion: because the gravity of Makemake is weaker than that of Pluto, Eris and Triton, a large amount of nitrogen was probably lost via atmospheric escape; methane is lighter than nitrogen, but has significantly lower vapor pressure at temperatures prevalent at the surface of Makemake (32–36 K),[8] which hinders its escape; the result of this process is a higher relative abundance of methane.[37]

    Lack of satellites

    No satellites have been detected around Makemake so far. A satellite having a brightness 1% of that of the primary would have been detected if it had been at the distance 0.4 arcseconds or further from Makemake.[24] This contrasts with other large trans-Neptunian objects, most of which have at least one satellite: Eris has one, Haumea has two and Pluto has five, though 2007 OR10 also has no known satellites. 10% to 20% of all trans-Neptunian objects are expected to have one or more satellites.[24] Because satellites offer a simple method to measure an object's mass, the lack of a satellite makes obtaining an accurate figure for Makemake's mass more difficult.[24]

    Exploration

    It was calculated that a flyby mission to Makemake could take just over 16 years using a Jupiter gravity assist, based on a launch date of 21 August 2024 and 24 August 2036. Makemake would be approximately 52 AU from the Sun when the spacecraft arrives.[38]

    See also

    Notes

    1. ↑ The Rapa Nui pronunciation is [ˈmakeˈmake], which is approximated in English as US /ˌmɑːkiˈmɑːki/ MAH-kee-MAH-kee,[1] UK /ˈmækiˈmæki/ MAK-ee-MAK-ee, or as /ˌmɑːkeɪˈmɑːkeɪ/ MAH-kay-MAH-kay.[2][3] The first is an anglicized pronunciation; the second is more Polynesian, and is used by Brown and his students.[4]
    2. 1 2 3 Astronomers Mike Brown, David Jewitt and Marc Buie classify Makemake as a near scattered object but the Minor Planet Center, from which Wikipedia draws most of its definitions for the trans-Neptunian population, places it among the main Kuiper belt population.[13][14][15][16]
    3. ↑ Calculated using (a−b)/a and the dimensions from [8]</ref> (6.9±0.3)×106 km2[lower-alpha 4]Albedo 0.81+0.01
      −0.02      [7]Temperature 32–36 K (single-terrain model)
      40–44 K (two-terrain model)[8]
      Spectral type
      B−V=0.83, V−R=0.5<ref name='Snodgrass2009'>Snodgrass, C.; Carry, B.; Dumas, C.; Hainaut, O. (February 2010). "Characterisation of candidate members of (136108) Haumea's family". Astronomy and Astrophysics 511: A72. arXiv:0912.3171. Bibcode:2010A&A...511A..72S. doi:10.1051/0004-6361/200913031.
    4. 1 2 Calculated using the dimensions from [8] assuming an oblate spheroid.</ref>[9]Volume (1.7±0.1)×109 km3[lower-alpha 4][10]Mass 2–5 × 1021 kg (estimated)[lower-alpha 5]
      Mean density
      1.4–3.2 g/cm3[7] 7.771±0.003 h<ref>A. N. Heinze and Daniel deLahunta, The rotation period and light-curve amplitude of Kuiper belt dwarf planet 136472 Makemake (2005 FY9), The Astronomical Journal 138 (2009), pp. 428–438. doi:10.1088/0004-6256/138/2/428
    5. ↑ The mass estimate is based on an density of 1.4–3.2 g/cm3 and a radius of 715 km. Makemake does not have a known satellite like Pluto, Eris, and Haumea have. A satellite offers a simple method to measure an object's mass.
    6. ↑ It has an apparent magnitude in opposition of 16.7 vs. 15 for Pluto.[23]
    7. ↑ Based on Minor Planet Center online Minor Planet Ephemeris Service: March 1, 1930: RA: 05h51m, Dec: +29.0.

    References

    1. 1 2 3 Brown, Mike (2008). "Mike Brown's Planets: What's in a name? (part 2)". California Institute of Technology. Retrieved 2008-07-14.
    2. ↑ Brown, Mike (2008). "Mike Brown's Planets: Make-make". California Institute of Technology. Retrieved 2008-07-14.
    3. ↑ Robert D. Craig (2004). Handbook of Polynesian Mythology. ABC-CLIO. p. 63. ISBN 978-1-57607-894-5.
    4. ↑ Podcast Dwarf Planet Haumea (Darin Ragozzine, at 3′11″)
    5. 1 2 "MPEC 2009-P26 :Distant Minor Planets (2009 AUG. 17.0 TT)". IAU Minor Planet Center. 2009-08-07. Retrieved 2009-08-28.
    6. 1 2 3 4 5 "JPL Small-Body Database Browser: 136472 Makemake (2005 FY9)". NASA Jet Propulsion Laboratory (2014-07-08 last obs). Retrieved 2015-08-27.
    7. 1 2 3 4 5 M.E. Brown, 2013, "On the size, shape, and density of dwarf planet Makemake"
    8. 1 2 3 4 5 6 7 Ortiz, J. L.; Sicardy, B.; Braga-Ribas, F.; Alvarez-Candal, A.; Lellouch, E.; Duffard, R.; Pinilla-Alonso, N.; Ivanov, V. D.; Littlefair, S. P.; Camargo, J. I. B.; Assafin, M.; Unda-Sanzana, E.; Jehin, E.; Morales, N.; Tancredi, G.; Gil-Hutton, R.; De La Cueva, I.; Colque, J. P.; Da Silva Neto, D. N.; Manfroid, J.; Thirouin, A.; Gutiérrez, P. J.; Lecacheux, J.; Gillon, M.; Maury, A.; Colas, F.; Licandro, J.; Mueller, T.; Jacques, C.; Weaver, D. (2012). "Albedo and atmospheric constraints of dwarf planet Makemake from a stellar occultation". Nature 491 (7425): 566–569. Bibcode:2012Natur.491..566O. doi:10.1038/nature11597. PMID 23172214. (ESO 21 November 2012 press release: Dwarf Planet Makemake Lacks Atmosphere)
    9. ↑ "surface ellipsoid 751x751x715 - Wolfram-Alpha".
    10. ↑ "volume ellipsoid 751x751x715 - Wolfram-Alpha".
    11. 1 2 3 "AstDys (136472) Makemake Ephemerides". Department of Mathematics, University of Pisa, Italy. Retrieved 2015-12-30.
    12. 1 2 3 4 5 6 "Asteroid 136472 Makemake (2005 FY9)". HORIZONS Web-Interface. JPL Solar System Dynamics. Retrieved 2015-12-30.
    13. 1 2 Marc W. Buie (2008-04-05). "Orbit Fit and Astrometric record for 136472". SwRI (Space Science Department). Retrieved 2008-07-13.
    14. 1 2 3 4 5 6 7 Mike Brown; K. M. Barksume; G. L. Blake; E. L. Schaller; et al. (2007). "Methane and Ethane on the Bright Kuiper Belt Object 2005 FY9". The Astronomical Journal 133 (1): 284–289. Bibcode:2007AJ....133..284B. doi:10.1086/509734.
    15. ↑ Audrey Delsanti; David Jewitt. "The Solar System Beyond The Planets" (PDF). University of Hawaii. Retrieved 2008-08-03.
    16. ↑ "List Of Transneptunian Objects". Minor Planet Center. Harvard-Smithsonian Center for Astrophysics. Retrieved 2008-08-03.
    17. 1 2 3 T.L. Lim; J. Stansberry; T.G. Müller (2010). ""TNOs are Cool": A survey of the trans-Neptunian region III. Thermophysical properties of 90482 Orcus and 136472 Makemake". Astronomy and Astrophysics 518: L148. Bibcode:2010A&A...518L.148L. doi:10.1051/0004-6361/201014701.
    18. 1 2 3 International Astronomical Union (2008-07-19). "Fourth dwarf planet named Makemake" (Press release). International Astronomical Union (News Release – IAU0806). Retrieved 2008-07-20.
    19. ↑ Michael E. Brown. "The Dwarf Planets". California Institute of Technology, Department of Geological Sciences. Retrieved 2008-01-26.
    20. 1 2 "Dwarf Planets and their Systems". Working Group for Planetary System Nomenclature (WGPSN). U.S. Geological Survey. 2008-11-07. Retrieved 2008-07-13.
    21. ↑ Gonzalo Tancredi; Sofia Favre (June 2008). "Which are the dwarfs in the Solar System?" (PDF). Icarus 195 (2): 851–862. Bibcode:2008Icar..195..851T. doi:10.1016/j.icarus.2007.12.020. Retrieved 2008-08-03.
    22. ↑ Thomas H. Maugh II & John Johnson Jr. (2005-10-16). "His Stellar Discovery Is Eclipsed". Los Angeles Times. Retrieved 2008-07-14.
    23. ↑ David L. Rabinowitz; Bradley E. Schaefer; Suzanne W. Tourtellotte (2007). "The Diverse Solar Phase Curves of Distant Icy Bodies. I. Photometric Observations of 18 Trans-Neptunian Objects, 7 Centaurs, and Nereid". The Astronomical Journal 133 (1): 26–43. arXiv:astro-ph/0605745. Bibcode:2007AJ....133...26R. doi:10.1086/508931.
    24. 1 2 3 4 5 Brown, M. E.; Van Dam, M. A.; Bouchez, A. H.; Le Mignant, D.; Campbell, R. D.; Chin, J. C. Y.; Conrad, A.; Hartman, S. K.; Johansson, E. M.; Lafon, R. E.; Rabinowitz, D. L. Rabinowitz; Stomski, P. J., Jr.; Summers, D. M.; Trujillo, C. A.; Wizinowich, P. L. (2006). "Satellites of the Largest Kuiper Belt Objects" (PDF). The Astrophysical Journal 639 (1): L43–L46. arXiv:astro-ph/0510029. Bibcode:2006ApJ...639L..43B. doi:10.1086/501524. Retrieved 2011-10-19.
    25. ↑ "Clyde W. Tombaugh". New Mexico Museum of Space History. Retrieved 2008-06-29.
    26. ↑ "Makemake Becomes the Newest Dwarf Planet". Slashdot. July 13, 2008. Retrieved November 23, 2012.
    27. 1 2 S. C. Tegler; W. M. Grundy; W. Romanishin; G. J. Consolmagno; et al. (2007-01-08). "Optical Spectroscopy of the Large Kuiper Belt Objects 136472 (2005 FY9) and 136108 (2003 EL61)". The Astronomical Journal 133 (2): 526–530. arXiv:astro-ph/0611135. Bibcode:2007AJ....133..526T. doi:10.1086/510134.
    28. ↑ "Asteroid 136108 (2003 EL61)". HORIZONS Web-Interface. JPL Solar System Dynamics. Retrieved 2008-08-04.
    29. 1 2 David Jewitt (February 2000). "Classical Kuiper Belt Objects (CKBOs)". University of Hawaii. Archived from the original on August 5, 2008. Retrieved 2008-08-04.
    30. ↑ Jane X. Luu & David C. Jewitt (2002). "Kuiper Belt Objects: Relics from the Accretion Disk of the Sun" (PDF). Ann. Rev. Astron. Astrophys. 40 (1): 63–101. Bibcode:2002ARA&A..40...63L. doi:10.1146/annurev.astro.40.060401.093818. Retrieved 2008-08-04.
    31. ↑ Levison, H. F.; Morbidelli, A. (2003-11-27). "The formation of the Kuiper belt by the outward transport of bodies during Neptune's migration". Nature 426 (6965): 419–421. Bibcode:2003Natur.426..419L. doi:10.1038/nature02120. PMID 14647375. Retrieved 2012-05-26.
    32. ↑ Preliminary simulation of Makemake (2005 FY9)'s orbit and the 2009-02-04 nominal (non-librating) rotating frame for Makemake. See (182294) 2001 KU76 for a proper 11:6 resonance libration.
    33. 1 2 3 4 J. Licandro; N. Pinilla-Alonso; M. Pedani; E. Oliva; et al. (2006). "The methane ice rich surface of large TNO 2005 FY9: a Pluto-twin in the trans-neptunian belt?". Astronomy and Astrophysics 445 (3): L35–L38. Bibcode:2006A&A...445L..35L. doi:10.1051/0004-6361:200500219.
    34. ↑ S.C. Tegler; W.M. Grundy; F. Vilas; W. Romanishin; et al. (June 2008). "Evidence of N2-ice on the surface of the icy dwarf Planet 136472 (2005 FY9)". Icarus 195 (2): 844–850. arXiv:0801.3115. Bibcode:2008Icar..195..844T. doi:10.1016/j.icarus.2007.12.015.
    35. ↑ Tobias C. Owen, Ted L. Roush, et al. (1993-08-06). "Surface Ices and the Atmospheric Composition of Pluto". Science 261 (5122): 745–748. Bibcode:1993Sci...261..745O. doi:10.1126/science.261.5122.745. PMID 17757212.
    36. ↑ "Dwarf Planet Makemake Lacks Atmosphere". ESO Press Release. Retrieved 23 November 2012.
    37. ↑ E.L. Schaller; M.E. Brown (2007-04-10). "Volatile Loss and Retention on Kuiper Belt Objects". The Astrophysical Journal 659 (1): L61–L64. Bibcode:2007ApJ...659L..61S. doi:10.1086/516709.
    38. ↑ McGranaghan, R.; Sagan, B.; Dove, G.; Tullos, A.; Lyne, J. E.; Emery, J. P. (2011). "A Survey of Mission Opportunities to Trans-Neptunian Objects". Journal of the British Interplanetary Society 64: 296–303. Bibcode:2011JBIS...64..296M.

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