(55637) 2002 UX25
Wikipedia on Answers.com:
Top
(55637) 2002 UX25
|
|
|
Discovery[1]
|
|
|---|---|
| Discovered by | Spacewatch (291) |
| Discovery date | October 30, 2002 |
|
Designations
|
|
| MPC designation | (55637) 2002 UX25 |
| Alternate name(s) | none |
| Minor planet category |
Cubewano (MPC)[2] Extended (DES)[3] |
| Epoch July 23, 2010 (JD 2455400.5 ) | |
| Aphelion | 7 318.7 Gm (48.923 AU) |
| Perihelion | 5 507.4 Gm (36.815 AU) |
| Semi-major axis | 6 413.1 Gm (42.869 AU) |
| Eccentricity | 0.14121 |
| Orbital period | 102522 d (280.69 yr) |
| Average orbital speed | 4.54 km/s |
| Mean anomaly | 289.85° |
| Inclination | 19.398° |
| Longitude of ascending node | 204.60° |
| Argument of perihelion | 275.49° |
| Satellites | One roughly 205 ± 55 km in diameter[5][6] |
|
Physical characteristics
|
|
| Dimensions | 681 +116 −114 km[7] |
| Mass | ≈3.3×1020? kg[8] |
| Mean density | 2.0? g/cm3 |
| Equatorial surface gravity | 0.2543? m/s2 |
| Escape velocity | 0.4811? km/s |
| Sidereal rotation period |
14.382 h[4] |
| Albedo | 0.115 +0.05 −0.03[7] |
| Temperature | ~43 K |
| Spectral type | (pushing red) B-V=1.12, V-R=0.61[9] B-V=0.95, V-R=0.56[10][11] |
| Apparent magnitude | 19.8[12] |
| Absolute magnitude (H) | 3.6[4] |
(55637) 2002 UX25 is a Spitzer dwarf-planet candidate that orbits the Sun in the Kuiper belt beyond Neptune. It takes roughly 280 years to orbit the Sun, and it has one known moon.
It is a trans-Neptunian object with an absolute magnitude of 3.6,[4] making it a dwarf planet candidate. The Spitzer Space Telescope estimates it to be about 681 km in diameter.[7] It was discovered on October 30, 2002, by the Spacewatch program.[1] It is a mid-sized cubewano similar to (20000) Varuna.
|
Contents
|
Brightness and color
A variability of the visual brightness was detected which could be fit to a period of 14.38 or 16.78 h (depending on a single-peaked or double peaked curve).[13]
The Spitzer Space Telescope has estimated it to have a size of 681 +116
−114 km.[7] It is redder than Varuna, unlike its neutral-colored "twin" 2002 TX300, in spite of similar brightness and orbit elements.
Satellite
The discovery of a satellite of 2002 UX25 was reported in IAUC 8812 on 22 February 2007.[5] The satellite was detected using the Hubble Space Telescope in August 2005.[5] The orbit of this satellite has yet to be determined. The satellite was found at 0.16 arcsec from the primary with an apparent magnitude difference of 2.5.[14] Assuming a similar albedo the magnitude suggests the satellite has a diameter of 205 ± 55 km.[6]
Classification
2002 UX25 has a perihelion (closest approach to the Sun) of 36.7 AU,[4] which it will next reach in 2065.[4] As of 2010, 2002 UX25 is 41 AU from the Sun.[12]
The Minor Planet Center (MPC) classifies 2002 UX25 as a cubewano[2] while the Deep Ecliptic Survey (DES) classifies it as scattered-extended.[3] The DES using a 10My integration (last observation: 2009-10-22) shows it with a minimum perihelion (qmin) distance of 36.3 AU.[3]
2002 UX25 has been observed 60 times with precovery images back to 1991.[4]
Dwarf planet?
The Spitzer Space Telescope has estimated 2002 UX25 to have a diameter of 681 +116
−114 km,[7] and most icy objects around 400 km in diameter are believed to be spherical.[15] Mike Brown's website lists it as a highly likely dwarf planet,[16] and Mike Brown calls it a probable dwarf planet.[17] Light curve analysis has questioned whether it would truly qualify as a dwarf planet.[18][19]
References
- ^ a b Marsden, Brian G. (2002-11-01). "MPEC 2002-V08 : 2002 UX25". IAU Minor Planet Center. Harvard-Smithsonian Center for Astrophysics. http://www.minorplanetcenter.net/mpec/K02/K02V08.html. Retrieved 2011-07-05.
- ^ a b "MPEC 2009-C70 :Distant Minor Planets (2009 FEB. 28.0 TT)". Minor Planet Center. 2009-02-10. http://www.minorplanetcenter.net/mpec/K09/K09C70.html. Retrieved 2011-07-05.
- ^ a b c Marc W. Buie (2009-10-22 using 60 observations). "Orbit Fit and Astrometric record for 55637". SwRI (Space Science Department). http://www.boulder.swri.edu/~buie/kbo/astrom/55637.html. Retrieved 2009-03-12.
- ^ a b c d e f g "JPL Small-Body Database Browser: 55637 (2002 UX25)". 2009-10-22 last obs. http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=55637. Retrieved 2008-12-09.
- ^ a b c Daniel W. E. Green (2007-02-22). "IAUC 8812: Sats OF 2003 AZ_84, (50000), (55637), (90482)". International Astronomical Union Circular. Archived from the original on 19 July 2011. http://web.archive.org/web/20110719205520/http://cbat.eps.harvard.edu/iauc/08800/08812.html. Retrieved 2011-07-05.
- ^ a b Wm. Robert Johnston (2007-03-04). "(55637) 2002 UX25". Johnston's Archive. http://www.johnstonsarchive.net/astro/astmoons/am-55637.html. Retrieved 2009-10-06.
- ^ a b c d e John Stansberry, Will Grundy, Mike Brown, Dale Cruikshank, John Spencer, David Trilling, Jean-Luc Margot (2007). "Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope". arXiv:astro-ph/0702538 [astro-ph].
- ^ Using the 2007 Spitzer radius of 340.5 km; volume of a sphere * an assumed density of 2 g/cm3 yields a mass (m=d*v) of 3.307E+20 kg
- ^ TNO Colors
- ^ Tegler, Stephen C. (2007-02-01). "Kuiper Belt Object Magnitudes and Surface Colors". http://www.physics.nau.edu/~tegler/research/survey.htm. Retrieved 2009-12-30.
- ^ Doressoundiram (2004). "The Meudon Multicolor Survey (2MS) of Centraurs and Trans-Neptunian objects". http://www.iop.org/EJ/article/1538-3881/134/6/2186/205733.web.pdf. Retrieved 2006-11-06.
- ^ a b "AstDys (55637) 2002UX25 Ephemerides". Department of Mathematics, University of Pisa, Italy. http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=2002UX25. Retrieved 2009-11-19.
- ^ Rousselot, P.; Petit, J.-M.; Poulet, F.; Sergeev, A. Photometric study of Centaur (60558) 2000 EC98 and trans-neptunian object (55637) 2002 UX25 at different phase angles, Icarus, 176, (2005) pp. 478–491.Abstract.
- ^ Distant EKO The Kuiper Belt Electronic newsletter, March 2007
- ^ Mike Brown. "The Dwarf Planets". Archived from the original on 29 January 2008. http://web.archive.org/web/20080129195021/http://web.gps.caltech.edu/~mbrown/dwarfplanets/. Retrieved 2008-01-20.
- ^ Michael E. Brown. "How many dwarf planets are there in the outer solar system? (updates daily)". California Institute of Technology. http://www.gps.caltech.edu/~mbrown/dps.html. Retrieved 2011-08-25.
- ^ Plutokiller (2012-Jan-13). "Probable". Twitter. https://twitter.com/#!/plutokiller/status/158054628418793472. Retrieved 2012-01-14.
- ^ Gonzalo Tancredi and Sofía Favre (13-Oct-2008?). "Dwarf Planet & Plutoid Headquarters". Portal Uruguayo de Astronomía. http://www.astronomia.edu.uy/dwarfplanet/list.html. Retrieved 2010-09-22. (Which are the dwarfs in the Solar System?)
- ^ Tancredi, Gonzalo (2009). "Physical and dynamical characteristics of icy “dwarf planets” (plutoids)". Proceedings of the International Astronomical Union Symposium S263 5: 173–185. Bibcode 2010IAUS..263..173T. DOI:10.1017/S1743921310001717.
External links
- Orbital simulation from JPL (Java) / Ephemeris
- MPEC 2002-V08
- AstDys orbital elements
|
|||||
|
||||||||||||||||||||
|
||||||||||||||||||||||
|
||||||||||||||||||||
|
||||||||
This entry is from Wikipedia, the leading user-contributed encyclopedia. It may not have been reviewed by professional editors (see full disclaimer)
Post a question - any question - to the WikiAnswers community:
Copyrights:
Wikipedia on Answers.com
This article is licensed under the Creative Commons Attribution/Share-Alike License. It uses material from the Wikipedia article (55637) 2002 UX25.
Read more