| 词条 | (84522) 2002 TC302 | ||
| 释义 |
| minorplanet=yes | background=#C2E0FF | name={{mp|(84522) 2002 TC|302}} | discovery_ref=[1] | discoverer=M. E. Brown, C. A. Trujillo, D. L. Rabinowitz(?) | discovered=9 October 2002 | mpc_name={{mp|(84522) 2002 TC|302}} | alt_names= | mp_category=SDO[2] 2:5 resonance[3][4] | orbit_ref=[5] | epoch=13 January 2016 (JD 2457400.5) | semimajor={{Convert|55.265|AU|Tm|abbr=on}} | perihelion={{Convert|38.979|AU|Tm|abbr=on}} | aphelion={{Convert|71.552|AU|Tm|abbr=on|lk=on}} | eccentricity=0.29469 | period=410.86 yr (150065 d) | inclination=35.107° | asc_node=23.902° | arg_peri=87.142° | mean_anomaly=322.056° | avg_speed=3.93 km/s | dimensions={{val|584.1|+105.6|-88.0}}[6] | mass= | density= | surface_grav= | escape_velocity= | rotation={{Convert|5.41|h|d|abbr=on|lk=on}}[7] | spectral_type=(red) B−V=1.03; V−R=0.67[6] | magnitude=20.5 (opposition)[9] | abs_magnitude=3.8[5] | albedo={{val|0.115|+0.047|-0.033}}[6] | single_temperature=< ≈38 K | mean_motion={{Deg2DMS|0.0023990|sup=ms}} / day | observation_arc=5574 days (15.26 yr) | uncertainty=3 | moid={{Convert|38.1784|AU|Tm|abbr=on}} | jupiter_moid={{Convert|34.8125|AU|Tm|abbr=on}} }}{{mp|(84522) 2002 TC|302}} is a red 2:5 resonant[3] trans-Neptunian object (TNO) discovered on October 9, 2002 by Mike Brown's team at the Palomar Observatory.[1] Physical characteristics{{mp|(84522) 2002 TC|302}} has an absolute magnitude (H) of 3.78.[5] It has an estimated diameter of {{val|584.1|+105.6|-88.0|u=km}}.[7] Using the Spitzer Space Telescope, it was previously estimated to have a diameter of {{val|1145|+337|-325|u=km}},[8] which would have made it one of the largest possible dwarf planets. This overestimation was due to insufficient motion to allow for a good sky subtraction and because it was very close to a brighter background object.[7] Brown noted that the Spitzer measurement involved a very large potential error and that the object would likely be smaller, making its chances of it being a dwarf planet "likely" rather than "near certainty", in his opinion.[9]It was predicted that on 30 November 2013, {{mp|(84522) 2002 TC|302}} might occult a star for slightly less than a minute.[10] However, the possibility to observe this occultation was judged as small. The precise duration that a Solar System object occults a star provides a precise way to determine its diameter, if observed from multiple locations. The red spectra suggests that {{mp|(84522) 2002 TC|302}} has very little fresh ice on its surface.[8] {{clear left}}Its rotational period is most likely 5.41 h, and it has a light-curve amplitude of {{val|0.04|0.01|u=mag}}.[11] Orbit{{mp|(84522) 2002 TC|302}} will come to perihelion in 2058.[5] Its perihelion (minimum distance from the Sun) of 39.1 AU[5] is about the same as Pluto's semi-major axis (average distance from the Sun). It is classified as a scattered disc object.[2][3]Given the long orbit that TNOs have around the Sun, {{mp|(84522) 2002 TC|302}} comes to opposition in late October of each year at an apparent magnitude of 20.5.[12] ResonanceBoth the Minor Planet Center (MPC) and the Deep Ecliptic Survey (DES) show this probable dwarf planet to be in a 2:5 resonance with Neptune.[3][4] Due to the resonance, it completes two orbits for every five orbits of Neptune. As of 2009, it is the largest likely dwarf planet that is known to be in a non-plutino resonance with Neptune. Plutinos are objects in 2:3 mean-motion resonance with Neptune. For every two orbits that a plutino makes, Neptune makes three.
PrecoveryIt has been observed 76 times back to August 5, 2000.[5] See also
References1. ^1 {{Cite web |date=2002-11-07 |title=MPEC 2002-V26 : 2002 TC302 |first=Brian G. |last=Marsden |work=IAU Minor Planet Center |publisher=Harvard-Smithsonian Center for Astrophysics |url=http://www.minorplanetcenter.org/mpec/K02/K02V26.html |accessdate=2010-01-06}} 2. ^1 {{Cite web |title=List Of Centaurs and Scattered-Disk Objects |publisher=Minor Planet Center |url=http://www.minorplanetcenter.org/iau/lists/Centaurs.html |accessdate=2008-09-19}} 3. ^1 2 3 {{Cite web |author=Marc W. Buie |author-link=Marc W. Buie |date=2007-09-16 |title=Orbit Fit and Astrometric record for 84522 |publisher=SwRI (Space Science Department) |url=http://www.boulder.swri.edu/~buie/kbo/astrom/84522.html |accessdate=2008-09-19}} 4. ^1 {{Cite web |title=MPEC 2009-C70 :Distant Minor Planets (2009 FEB. 28.0 TT) |date=2009-02-10 |publisher=Minor Planet Center |url=http://www.minorplanetcenter.org/mpec/K09/K09C70.html |accessdate=2009-03-05}} 5. ^1 2 3 4 5 {{Cite web |type=last observation:2009-10-25 |title=JPL Small-Body Database Browser: 84522 (2002 TC302) |url=http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=84522 |accessdate=7 April 2016}} 6. ^{{Cite web |url=http://www.physics.nau.edu/~tegler/research/survey.htm |title=Kuiper Belt Object Magnitudes and Surface Colors |accessdate=2006-11-05 |last=Tegler |first=Stephen C. |date=2006-01-26 |deadurl=yes |archiveurl=https://web.archive.org/web/20060901063349/http://www.physics.nau.edu/~tegler/research/survey.htm |archivedate=2006-09-01 |df= }} 7. ^1 2 3 {{cite journal |display-authors=4 |author=Fornasier, S. |author2=Lellouch, E. |author3=Müller, T. |author4=Santos-Sanz, P. |author5=Panuzzo, P. |author6=Kiss, C. |author7=Lim, T. |author8=Mommert, M. |author9=Bockelée-Morvan, D. |author10=Vilenius, E. |author11=Stansberry, J. |author12=Tozzi, G.P. |author13=Mottola, S. |author14=Delsanti, A. |author15=Crovisier, J. |author16=Duffard, R. |author17=Henry, F. |author18=Lacerda, P. |author19=Barucci, A. |author20=Gicquel, A. |date=July 2013 |url=https://arxiv.org/pdf/1305.0449v2.pdf |title=TNOs are Cool: A survey of the trans-Neptunian region. VIII. Combined Herschel PACS and SPIRE observations of 9 bright targets at 70–500 µm |journal=Astronomy & Astrophysics |volume=555 |id=A15 |doi=10.1051/0004-6361/201321329 }} 8. ^1 {{cite arXiv|title=Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope |display-authors=4 |author=John Stansberry |author2=Will Grundy |author3=Mike Brown |author4=Dale Cruikshank |author5=John Spencer |author6=David Trilling |author7=Jean-Luc Margot |eprint=astro-ph/0702538 |date=2007}} 9. ^{{cite web |title=How many dwarf planets are there in the outer solar system? (updates daily) |publisher=California Institute of Technology |author=Michael E. Brown |author-link=Michael E. Brown |url=http://web.gps.caltech.edu/~mbrown/dps.html |accessdate=31 August 2016}} 10. ^Stevge Preston's Asteroid Occultation Updates item {{webarchive|url=https://web.archive.org/web/20131030132644/http://www.asteroidoccultation.com/2013_11/1120_84522_30341.htm |date=2013-10-30 }}; accessed 22 February 2013 11. ^1 {{cite journal |url=https://arxiv.org/pdf/1207.2044.pdf |title=Short-term variability of 10 trans-Neptunian objects |display-authors=4 |author=Thirouin, A. |author2=Ortiz, J.L. |author3=Campo Bagatin, A. |author4=Pravec, P. |author5=Morales, N. |author6=Hainaut, O. |author7=Duffard, R. |journal=Monthly Notices of the Royal Astronomical Society |volume=424 |issue=4 |date=21 August 2012 |pages=3156–3177 |doi=10.1111/j.1365-2966.2012.21477.x }} 12. ^1 {{Cite web|title=(84522) 2002 TC302|date=2010-07-23|publisher=Minor Planet Center|url=http://scully.cfa.harvard.edu/~cgi/ReturnPrepEph?d=d&o=84522|accessdate=2010-10-24}} External links{{Commons category|(84522) 2002 TC302}}
5 : Scattered disc and detached objects|2:5 resonance|Discoveries by the Palomar Observatory|Possible dwarf planets|Astronomical objects discovered in 2002 |
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