20898 Fountainhills

Last updated

20898 Fountainhills
Discovery  [1]
Discovered by C. W. Juels
Discovery site Fountain Hills Obs.
Discovery date30 November 2000
Designations
(20898) Fountainhills
Named after
 Fountain Hills   [1]
(U.S. city in Arizona)
2000 WE147 ·1975 BE
1994 NA1
main-belt   [1] [2]  ·(outer)  [2] [3]
background   [4]  ·ACO  [5] : 872 
Orbital characteristics   [2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc 66.49 yr (24,285 d)
Aphelion 6.1881 AU
Perihelion 2.2572 AU
4.2226 AU
Eccentricity 0.4654
8.68 yr (3,169 d)
328.44°
0° 6m 48.96s / day
Inclination 45.523°
293.19°
234.78°
Jupiter  MOID 0.5295 AU
TJupiter 2.3490
Physical characteristics
37.08  km (derived) [3]
37.31±1.1 km [6]
41.53±0.85 km [7]
12.84±0.03  h [8]
0.0200 (derived) [3]
0.037±0.007 [7]
0.0505±0.003 [6]
D   [3] [5]
B–V = 0.767±0.008 [9]
V–R = 0.428±0.010 [9]
V–I = 0.826±0.008 [9]
11.0 [6]  ·11.10 [2] [7]
12.02 [3] [8]

    20898 Fountainhills (provisional designation 2000 WE147) is a dark asteroid in a cometary orbit (ACO) from the outermost regions of the asteroid belt, approximately 37 kilometers (23 miles) in diameter. It was discovered on 30 November 2000, by American amateur astronomer Charles W. Juels at the Fountain Hills Observatory in Arizona, United States. [1] The D-type asteroid has a rotation period of 12.84 hours. [3] It was named for the city of Fountain Hills, Arizona, in the United States. [1]

    Contents

    Orbit and classification

    Fountainhills is a non-family from the main belt's background population. [4] For an object in the asteroid belt, its orbit is extremely eccentric and highly inclined. With a Jupiter tisserand (TJupiter) of less than 3 and with no observable coma, it is an asteroid in cometary orbit (ACO) and a candidate for being a dormant or extinct comet. [5] It is however, not a damocloid based on current orbital criteria, which typically have a TJupiter of less than 2 (also see List of damocloids).

    The asteroid orbits the Sun in the outer main-belt at a distance of 2.3–6.2  AU once every 8 years and 8 months (3,169 days; semi-major axis of 4.22 AU). Its orbit has an eccentricity of 0.47 and an inclination of 46° with respect to the ecliptic. [2] The body's observation arc begins with a precovery taken at Palomar Observatory during the Digitized Sky Survey in July 1951, more than 49 years prior to its official discovery observation at Fountain Hills. [1]

    Fountainhills is the second most eccentric object as large as it is inside the orbit of Jupiter (after 1036 Ganymed), and the most highly inclined object of its size within the orbit of Jupiter. While its aphelion is outside that of Jupiter's orbit, it is so highly inclined that its furthest point from the Sun is far out of the ecliptic.[ citation needed ]

    Physical characteristics

    Fountainhills has been characterized as a dark D-type asteroid in a study of asteroids in cometary orbits using the Nordic Optical Telescope at Roque de los Muchachos Observatory on the Canary Island, Spain. [5]

    Rotation period

    In January 2001, a rotational lightcurve of Fountainhills was obtained from photometric observations by American amateur astronomer Bill Holliday at River Oaks Observatory ( 915 ) in Texas. Lightcurve analysis gave a well-defined rotation period of 12.84 hours with a brightness amplitude of 0.20 magnitude ( U=3 ). [8]

    Diameter and albedo

    According to the survey carried out by the Infrared Astronomical Satellite IRAS, and on data obtained by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Fountainhills measures between 37.31 and 41.53 kilometers in diameter and its surface has an albedo between 0.037 and 0.0505. [6] [7] The Collaborative Asteroid Lightcurve Link derives an albedo of 0.02 and a diameter of 37.08 kilometers based on an absolute magnitude of 12.02. [3]

    Naming

    This minor planet was named after the town of Fountain Hills, located near the Sonoran Desert on the foothills of the McDowell Mountains, home to one of the world's tallest water fountains. The official naming citation was published by the Minor Planet Center on 9 May 2001 ( M.P.C. 42678). [10]

    Related Research Articles

    <span class="mw-page-title-main">944 Hidalgo</span>

    944 Hidalgo is a centaur and unusual object on an eccentric, cometary-like orbit between the asteroid belt and the outer Solar System, approximately 52 kilometers in diameter. Discovered by German astronomer Walter Baade in 1920, it is the first member of the dynamical class of centaurs ever to be discovered. The dark D-type object has a rotation period of 10.1 hours and likely an elongated shape. It was named after Mexican revolutionary Miguel Hidalgo y Costilla.

    Damocloids are a class of minor planets such as 5335 Damocles and 1996 PW that have Halley-type or long-period highly eccentric orbits typical of periodic comets such as Halley's Comet, but without showing a cometary coma or tail. David Jewitt defines a damocloid as an object with a Jupiter Tisserand invariant (TJ) of 2 or less, while Akimasa Nakamura defines this group with the following orbital elements:

    1373 Cincinnati, provisional designation 1935 QN, is an asteroid in a comet-like orbit from the Cybele region, located at the outermost rim of the asteroid belt, approximately 20 kilometers in diameter. It was the only asteroid discovery made by famous American astronomer Edwin Hubble, while observing distant galaxies at Mount Wilson Observatory in California on 30 August 1935. The rather spherical X-type asteroid has a rotation period of 5.3 hours. It was named for the Cincinnati Observatory.

    20461 Dioretsa is a centaur and damocloid on a retrograde, cometary-like orbit from the outer Solar System. It was discovered on 8 June 1999, by members of the LINEAR team at the Lincoln Laboratory Experimental Test Site near Socorro, New Mexico, United States. The highly eccentric unusual object measures approximately 14 kilometers in diameter. It was named Dioretsa, the word "asteroid" spelled backwards.

    <span class="mw-page-title-main">748 Simeïsa</span> Hilda asteroid

    748 Simeïsa is a very large Hilda asteroid from the outermost regions of the asteroid belt, approximately 104 kilometers in diameter. It was discovered on 14 March 1913, by Russian astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The dark P-type asteroid has a rotation period of 11.9 hours and a shape that is reminiscent of a tetrahedron. It was the first asteroid discovery made in Russia and named after the discovering observatory and its nearby Crimean town, Simeiz.

    <span class="mw-page-title-main">909 Ulla</span> Outer main-belt asteroid

    909 Ulla is a large and dark asteroid from the outermost regions of the asteroid belt, that measures approximately 116 kilometers in diameter. It is the parent body and namesake of the Ulla family, which belongs to the larger group of Cybele asteroids. It was discovered on 7 February 1919, by German astronomer Karl Reinmuth at the Heidelberg Observatory in southwest Germany. The X-type asteroid has a rotation period of 8.7 hours and a notably low value for its Jupiter Tisserand's parameter. It was named after Ulla Ahrens, daughter of a friend of the discoverer.

    1952 Hesburgh, provisional designation 1951 JC, is a rare-type carbonaceous asteroid from the outer regions of the asteroid belt, approximately 37 kilometers in diameter.

    1213 Algeria is a carbonaceous asteroid from the outer region of the asteroid belt, approximately 32 kilometers in diameter. Discovered by Guy Reiss at Algiers Observatory in 1931, it was named after the North African country of Algeria.

    4946 Askalaphus ( ə-SKAL-ə-fəs; prov. designation: 1988 BW1) is a Jupiter trojan from the Greek camp, approximately 52 kilometers (32 miles) in diameter. It was discovered on 21 January 1988 by American astronomer couple Carolyn and Eugene Shoemaker at the Palomar Observatory in California. The dark D-type asteroid belongs to the 100 largest Jupiter trojans and has a rotation period of 22.7 hours. It was named after Ascalaphus from Greek mythology.

    1362 Griqua, provisional designation 1935 QG1 is a dark, Jupiter-resonant background asteroid on an eccentric, cometary-like orbit and the namesake of the Griqua group, located in the Hecuba gap in the outermost region of the asteroid belt. The carbonaceous asteroid measures approximately 28 kilometers (17 miles) in diameter and has a rotation period of 6.9 hours. It was discovered on 31 July 1935, by South-African astronomer Cyril Jackson at Union Observatory in Johannesburg. The asteroid was named after the Griqua people in South Africa and Namibia.

    <span class="mw-page-title-main">1693 Hertzsprung</span>

    1693 Hertzsprung is a dark and elongated background asteroid from the middle region of the asteroid belt, approximately 39 kilometers in diameter. It was discovered on 5 May 1935, by Dutch astronomer Hendrik van Gent at the Leiden Southern Station, annex to the Johannesburg Observatory in South Africa.

    3793 Leonteus is a large Jupiter trojan from the Greek camp, approximately 90 kilometers in diameter. It was discovered on 11 October 1985, by American astronomer couple Carolyn and Eugene Shoemaker at the Palomar Observatory in California, United States. The D-type Jovian asteroid belongs to the 30 largest Jupiter trojans and has a rotation period of 5.6 hours. It was named after the hero Leonteus from Greek mythology.

    4792 Lykaon is a dark Jupiter trojan from the Trojan camp, approximately 51 kilometers in diameter. It was discovered on 10 September 1988, by American astronomer Carolyn Shoemaker at the Palomar Observatory in California. The possibly elongated Jovian asteroid belongs to the 100 largest Jupiter trojans and has a long rotation period of 40.1 hours. It was named after the Trojan prince Lycaon from Greek mythology.

    3688 Navajo, provisional designation 1981 FD, is a Griqua asteroid and a 2:1 Jupiter librator on an eccentric, cometary-like orbit from the outermost regions of the asteroid belt, approximately 6 kilometers in diameter. It was discovered on 30 March 1981, by American astronomer Edward Bowell at the Anderson Mesa Station near Flagstaff, Arizona. The dark P-type asteroid was named for the Native American Navajo people.

    <span class="mw-page-title-main">1484 Postrema</span>

    1484 Postrema, provisional designation 1938 HC, is a carbonaceous Postremian asteroid and namesake of the Postrema family from the central regions of the asteroid belt, approximately 41 kilometers in diameter. It was discovered on 29 April 1938, by Soviet astronomer Grigory Neujmin at the Simeiz Observatory on the Crimean peninsula. The name "Postrema" celebrates the astronomer's last minor planet discovery.

    2223 Sarpedon is a dark Jupiter trojan from the Trojan camp, approximately 90 kilometers in diameter. It was discovered on 4 October 1977, by astronomers at the Purple Mountain Observatory near Nanking, China. The D-type asteroid belongs to the 30 largest Jupiter trojans and has a rotation period of 22.7 hours. It was named after the Lycian hero Sarpedon from Greek mythology.

    1922 Zulu, provisional designation 1949 HC, is a carbonaceous asteroid in a strongly unstable resonance with Jupiter, located in the outermost regions of the asteroid belt, and approximately 20 kilometers in diameter. It was discovered on 25 April 1949, by South African astronomer Ernest Johnson at Union Observatory in Johannesburg, and named for the South African Zulu people.

    (457175) 2008 GO98 (provisional designation 2008 GO98) with cometary number 362P, is a Jupiter family comet in a quasi-Hilda orbit within the outermost regions of the asteroid belt. It was discovered on 8 April 2008, by astronomers of the Spacewatch program at Kitt Peak National Observatory near Tucson, Arizona, in the United States. This presumably carbonaceous body has a diameter of approximately 15 kilometers (9 miles) and rotation period of 10.7 hours.

    (20729) 1999 XS143 (provisional designation 1999 XS143) is a Jupiter trojan from the Greek camp, approximately 51 kilometers (32 miles) in diameter. It was discovered on 15 December 1999, by American astronomer Charles Juels at the Fountain Hills Observatory in Arizona. The dark Jovian asteroid has a short rotation period of 5.72 hours and belongs to the 90 largest Jupiter trojans. It has not been named since its numbering in January 2001.

    (23958) 1998 VD30 (provisional designation 1998 VD30) is a Jupiter trojan from the Greek camp, approximately 47 kilometers (29 miles) in diameter. It was discovered on 10 November 1998, by astronomers with the LINEAR survey at the Lincoln Laboratory's Experimental Test Site near Socorro, New Mexico, in the United States. The dark Jovian asteroid belongs to the 110 largest Jupiter trojans and shows an exceptionally slow rotation of 562 hours. It has not been named since its numbering in April 2001.

    References

    1. 1 2 3 4 5 6 "20898 Fountainhills (2000 WE147)". Minor Planet Center. Retrieved 10 April 2018.
    2. 1 2 3 4 5 "JPL Small-Body Database Browser: 20898 Fountainhills (2000 WE147)" (2018-01-24 last obs.). Jet Propulsion Laboratory . Retrieved 10 April 2018.
    3. 1 2 3 4 5 6 7 "LCDB Data for (20898) Fountainhills". Asteroid Lightcurve Database (LCDB). Retrieved 8 December 2017.
    4. 1 2 "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Archived from the original on 2 August 2017. Retrieved 8 December 2017.
    5. 1 2 3 4 Licandro, J.; Alvarez-Candal, A.; de León, J.; Pinilla-Alonso, N.; Lazzaro, D.; Campins, H. (April 2008). "Spectral properties of asteroids in cometary orbits" (PDF). Astronomy and Astrophysics. 481 (3): 861–877. Bibcode:2008A&A...481..861L. doi: 10.1051/0004-6361:20078340 . Retrieved 8 December 2017.
    6. 1 2 3 4 Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T . Retrieved 22 October 2019.
    7. 1 2 3 4 Licandro, J.; Alí-Lagoa, V.; Tancredi, G.; Fernández, Y. (January 2016). "Size and albedo distributions of asteroids in cometary orbits using WISE data". Astronomy and Astrophysics. 585: 12. arXiv: 1510.02282 . Bibcode:2016A&A...585A...9L. doi:10.1051/0004-6361/201526866.
    8. 1 2 3 Holliday, B. (June 2001). "Photometry of Asteroid 251 Sophia, 393 Lampetia, and (20898) 2000 WE147, September 2000 through January 2001". The Minor Planet Bulletin. 28: 26–28. Bibcode:2001MPBu...28...26H.
    9. 1 2 3 Ye, Q.-z. (February 2011). "BVRI Photometry of 53 Unusual Asteroids". The Astronomical Journal. 141 (2): 8. arXiv: 1011.0133 . Bibcode:2011AJ....141...32Y. doi:10.1088/0004-6256/141/2/32.
    10. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 10 April 2018.
    This page is based on this Wikipedia article
    Text is available under the CC BY-SA 4.0 license; additional terms may apply.
    Images, videos and audio are available under their respective licenses.