(120216) 2004 EW95

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(120216) 2004 EW95
120216-2004ew95 hst.jpg
Hubble Space Telescope image of 2004 EW95 taken in 2010
Discovery [1]
Discovered by Kitt Peak Obs.
Discovery date14 March 2004
Designations
(120216) 2004 EW95
Orbital characteristics [1]
Epoch 23 March 2018 (JD  2458200.5)
Uncertainty parameter 2
Observation arc 4847 days (13.27 yr)
Aphelion 52.590  AU (7.8674  Tm)
Perihelion 26.975 AU (4.0354 Tm)
39.783 AU (5.9515 Tm)
Eccentricity 0.32193
250.93  yr (91652  d)
359.95°
0° 0m 14.219s / day (n)
Inclination 29.234°
25.704°
204.67°
Earth  MOID 25.99 AU (3.888 Tm)
Jupiter  MOID 21.69 AU (3.245 Tm)
Uranus  MOID 9 AU (1.3 Tm) [4]
Physical characteristics
Dimensions291 km [5]
0.04 (dark) [5]
~21.0 [6]
6.3 [1]

    (120216) 2004 EW95, provisionally known as 2004 EW95, is a resonant trans-Neptunian object in the Kuiper belt located in the outermost regions of the Solar System. It measures approximately 291 kilometers in diameter. [7] It has more carbon than typical of KBOs, and the first to be confirmed as having this composition in this region of space. [8] It is thought to have originated closer to the Sun, perhaps even in the main asteroid belt. [8]

    Contents

    Orbit

    2004 EW95 is currently well inside the orbit of Neptune. 2004EW95-orbit.png
    2004 EW95 is currently well inside the orbit of Neptune.

    Like Pluto, 2004 EW95 is classified as a plutino. It stays in a 2:3 resonance with Neptune. [2] [3] For every 2 orbits that a plutino makes, Neptune orbits 3 times.

    2004 EW95 is currently 27.0  AU from the Sun, [6] and came to perihelion (q=26.98 AU) in April 2018. [1] This means that this object is currently inside the orbit of the planet Neptune. Like Pluto, this plutino spends part of its orbit closer to the Sun than Neptune is even though their orbits are controlled by Neptune. (Plutinos Huya and (15875) 1996 TP66 are even currently inside the orbit of Neptune.) Simulations by the Deep Ecliptic Survey (DES) show that over the next 10 million years 2004 EW95 can acquire a perihelion distance (qmin) as small as 24.6 AU. [3]

    It comes within 9  AU (1.3  billion   km ) of Uranus and stays more than 21 AU from Neptune over a 14,000 year period. [4] 2004 EW95 has been observed 158 times with an observation arc of 13 years and has an orbit quality of 2. [1]

    Physical characteristics

    Artist's impression of plutino and possible former C-type asteroid 2004 EW95 Artist's impression of exiled asteroid 2004 EW95.jpg
    Artist's impression of plutino and possible former C-type asteroid 2004 EW95

    2004 EW95 has a dark albedo of 0.04, giving it a diameter of about 291 km. [5] Its reflectance spectrum bears striking resemblance to those of some hydrated C-type asteroids, indicating that this object possibly formed in the same environment as the C-type asteroids found today in the outer asteroid belt. [10]

    Unlike the majority of small objects in the Kuiper belt observed so far, the visible spectrum of 2004 EW95 has two features, each respectively associated with ferric oxides and phyllosilicates. [10] The presence of a phyllosilicate feature in the spectrum of a minor planet indicates that the rocky component of its composition has been altered by the presence of liquid water at some point since its formation. [11] For this to have occurred on 2004 EW95 in its current orbit and at temperatures of ~35K, [12] significant quantities of thermal energy would have been required. While this energy could have been delivered by a very large chance collision, [13] the strong overall similarity between the modern C-type asteroids in the outer asteroid belt and 2004 EW95 suggests that these objects formed in the same region of the early Sun's protoplanetary disk, much closer to the Sun and at higher temperatures.

    The Grand tack hypothesis [14] predicts that the primitive C-type asteroids were dispersed from their formation location by the migrations of Jupiter and Saturn and many were injected into the outer asteroid belt where we find them today. By the same mechanism (and others that result from planetary formation), [15] simulations show that C-types can also be thrown outward to the trans-Neptunian region, where later they may become captured into the mean-motion resonances of Neptune. [14] [15]

    See also

    Related Research Articles

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    A classical Kuiper belt object, also called a cubewano ( "QB1-o"), is a low-eccentricity Kuiper belt object (KBO) that orbits beyond Neptune and is not controlled by an orbital resonance with Neptune. Cubewanos have orbits with semi-major axes in the 40–50 AU range and, unlike Pluto, do not cross Neptune's orbit. That is, they have low-eccentricity and sometimes low-inclination orbits like the classical planets.

    <span class="mw-page-title-main">Kuiper belt</span> Area of the Solar System beyond the planets, comprising small bodies

    The Kuiper belt is a circumstellar disc in the outer Solar System, extending from the orbit of Neptune at 30 astronomical units (AU) to approximately 50 AU from the Sun. It is similar to the asteroid belt, but is far larger—20 times as wide and 20–200 times as massive. Like the asteroid belt, it consists mainly of small bodies or remnants from when the Solar System formed. While many asteroids are composed primarily of rock and metal, most Kuiper belt objects are composed largely of frozen volatiles, such as methane, ammonia, and water. The Kuiper belt is home to most of the objects that astronomers generally accept as dwarf planets: Orcus, Pluto, Haumea, Quaoar, and Makemake. Some of the Solar System's moons, such as Neptune's Triton and Saturn's Phoebe, may have originated in the region.

    In astronomy, the plutinos are a dynamical group of trans-Neptunian objects that orbit in 2:3 mean-motion resonance with Neptune. This means that for every two orbits a plutino makes, Neptune orbits three times. The dwarf planet Pluto is the largest member as well as the namesake of this group. The next largest members are Orcus, (208996) 2003 AZ84, and Ixion. Plutinos are named after mythological creatures associated with the underworld.

    <span class="mw-page-title-main">Trans-Neptunian object</span> Solar system objects beyond Neptune

    A trans-Neptunian object (TNO), also written transneptunian object, is any minor planet in the Solar System that orbits the Sun at a greater average distance than Neptune, which has an orbital semi-major axis of 30.1 astronomical units (au).

    <span class="nowrap">(55565) 2002 AW<sub>197</sub></span> Classical Kuiper belt object

    (55565) 2002 AW197 is a classical, non-resonant trans-Neptunian object from the Kuiper belt in the outermost region of the Solar System, also known as a cubewano. With a likely diameter of at least 700 kilometers (430 miles), it is approximately tied with 2002 MS4 and 2013 FY27 (to within measurement uncertainties) as the largest unnamed object in the Solar System. It was discovered at Palomar Observatory in 2002.

    In astronomy, a resonant trans-Neptunian object is a trans-Neptunian object (TNO) in mean-motion orbital resonance with Neptune. The orbital periods of the resonant objects are in a simple integer relations with the period of Neptune, e.g. 1:2, 2:3, etc. Resonant TNOs can be either part of the main Kuiper belt population, or the more distant scattered disc population.

    <span class="mw-page-title-main">Scattered disc</span> Collection of bodies in the extreme Solar System

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    <span class="mw-page-title-main">10370 Hylonome</span>

    10370 Hylonome (; prov. designation: 1995 DW2) is a minor planet orbiting in the outer Solar System. The dark and icy body belongs to the class of centaurs and measures approximately 72 kilometers (45 miles) in diameter. It was discovered on 27 February 1995, by English astronomer David C. Jewitt and Vietnamese American astronomer Jane Luu at the U.S. Mauna Kea Observatory in Hawaii, and later named after the mythological creature Hylonome.

    <span class="nowrap">(208996) 2003 AZ<sub>84</sub></span> Plutino

    (208996) 2003 AZ84 is a trans-Neptunian object with a possible moon located in the outer regions of the Solar System. It is approximately 940 kilometers across its longest axis, as it has an elongated shape. It belongs to the plutinos – a group of minor planets named after its largest member Pluto – as it orbits in a 2:3 resonance with Neptune in the Kuiper belt. It is the third-largest known plutino, after Pluto and Orcus. It was discovered on 13 January 2003, by American astronomers Chad Trujillo and Michael Brown during the NEAT survey using the Samuel Oschin telescope at Palomar Observatory.

    <span class="nowrap">(15875) 1996 TP<sub>66</sub></span>

    (15875) 1996 TP66, provisional designation 1996 TP66, is a resonant trans-Neptunian object of the plutino population, located in the outermost region of the Solar System, approximately 154 kilometers (96 miles) in diameter. It was discovered on 11 October 1996, by astronomers Jane Luu, David C. Jewitt and Chad Trujillo at the Mauna Kea Observatories, Hawaii, in the United States. The very reddish RR-type with a highly eccentric orbit has been near its perihelion around the time of its discovery. This minor planet was numbered in 2000 and has since not been named. It is probably not a dwarf planet candidate.

    (118228) 1996 TQ66, prov. designation:1996 TQ66, is a resonant trans-Neptunian object of the plutino population in the Kuiper belt, located in the outermost region of the Solar System. It was discovered on 8 October 1996, by American astronomers Jun Chen, David Jewitt, Chad Trujillo and Jane Luu, using the UH88 telescope at the Mauna Kea Observatories, Hawaii. The very red object measures approximately 185 kilometers (110 miles) in diameter. As of 2021, it has not been named.

    (35671) 1998 SN165, prov. designation: 1998 SN165, is a trans-Neptunian object from the Kuiper belt located in the outermost region of the Solar System. It was discovered on 23 September 1998, by American astronomer Arianna Gleason at the Kitt Peak National Observatory near Tucson, Arizona. The cold classical Kuiper belt object is a dwarf planet candidate, as it measures approximately 400 kilometers (250 miles) in diameter. It has a grey-blue color (BB) and a rotation period of 8.8 hours. As of 2021, it has not been named.

    <span class="mw-page-title-main">Detached object</span> Dynamical class of minor planets

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    <span class="nowrap">(455502) 2003 UZ<sub>413</sub></span>

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    References

    1. 1 2 3 4 5 6 "JPL Small-Body Database Browser: 120216 (2004 EW95)" (last observation: 2015-06-19). Retrieved 7 April 2016.
    2. 1 2 "MPEC 2009-E53 :Distant Minor Planets (2009 MAR. 30.0 TT)". Minor Planet Center. 11 March 2009. Retrieved 24 March 2009.
    3. 1 2 3 Marc W. Buie. "Orbit Fit and Astrometric record for 120216" (last observation: 2009-05-26 using 44 observations). SwRI (Space Science Department). Archived from the original on 1 February 2018. Retrieved 18 September 2009.
    4. 1 2 "MPEC 2004-H77 : 2004 EW95". Minor Planet Center. 26 April 2004. Retrieved 24 March 2009.
    5. 1 2 3 Wm. Robert Johnston (22 August 2008). "List of Known Trans-Neptunian Objects". Johnston's Archive. Archived from the original on 15 April 2009. Retrieved 24 March 2009.
    6. 1 2 "AstDys (120216) 2004EW95 Ephemerides". Department of Mathematics, University of Pisa, Italy. Archived from the original on 27 February 2012. Retrieved 24 March 2009.
    7. ↑ St. Fleur, Nicholas (10 May 2018). "This Asteroid Shouldn't Be Where Astronomers Found It". The New York Times . Retrieved 11 May 2018.
    8. 1 2 "Exiled asteroid discovered in outer reaches of solar system: ESO telescopes find first confirmed carbon-rich asteroid in Kuiper Belt". ScienceDaily. Retrieved 1 November 2018.
    9. ↑ "Exiled Asteroid Discovered in Outer Reaches of Solar System – ESO telescopes find first confirmed carbon-rich asteroid in Kuiper Belt". www.eso.org. Retrieved 12 May 2018.
    10. 1 2 Seccull, Tom; Fraser, Wesley C.; Puzia, Thomas H.; Brown, Michael E.; Schönebeck, Frederik (2018). "2004 EW95: A phyllosilicate bearing carbonaceous asteroid in the Kuiper Belt". The Astrophysical Journal . 855 (2): L26. arXiv: 1801.10163 . Bibcode:2018ApJ...855L..26S. doi: 10.3847/2041-8213/aab3dc . S2CID   51688469.
    11. ↑ Fornasier, S.; Lantz, C.; Barucci, M. A.; Lazzarin, M. (2014). "Aqueous alteration on main belt primitive asteroids: Results from visible spectroscopy". Icarus . 233: 163–178. arXiv: 1402.0175 . Bibcode:2014Icar..233..163F. doi:10.1016/j.icarus.2014.01.040. S2CID   119234996.
    12. ↑ Mommert, M.; Harris, A. W.; Kiss, C.; Pál, A.; Santos-Sanz, P.; Stansberry, J.; Delsanti, A.; Vilenius, E.; Müller, T. G.; Peixinho, N.; Lellouch, E.; Szalai, N.; Henry, F.; Duffard, R.; Fornasier, S.; Hartogh, P.; Mueller, M.; Ortiz, J. L.; Protopapa, S.; Rengel, M.; Thirouin, A. (2012). "TNOs are cool: A survey of the trans-Neptunian region V. Physical characterization of 18 Plutinos using Herschel-PACS observations". Astronomy and Astrophysics . 541 (A93): A93. arXiv: 1202.3657 . Bibcode:2012A&A...541A..93M. doi:10.1051/0004-6361/201118562.
    13. ↑ Rubin, Alan E. (1995). "Petrologic evidence for collisional heating of chondritic asteroids". Icarus . 113 (1): 156–167. Bibcode:1995Icar..113..156R. doi:10.1006/icar.1995.1013.
    14. 1 2 Walsh, Kevin J.; Morbidelli, Alessandro; Raymond, Sean N.; O'Brien, David P.; Mandell, Avi M. (2011). "A low mass for Mars from Jupiter's early gas-driven migration". Nature . 475 (206): 206–209. arXiv: 1201.5177 . Bibcode:2011Natur.475..206W. doi:10.1038/nature10201. PMID   21642961. S2CID   4431823.
    15. 1 2 Raymond, Sean N.; Izidoro, Andre (2017). "Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion". Icarus . 297: 134–148. arXiv: 1707.01234 . Bibcode:2017Icar..297..134R. doi:10.1016/j.icarus.2017.06.030. S2CID   119031134.
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