| 词条 | (55638) 2002 VE95 |
| 释义 |
| minorplanet = yes | background = #C2E0FF | name = {{mp|(55638) 2003 VE|95}} | symbol = | image = | caption = | discovery_ref = [1] | discoverer = NEAT | discovered = 14 November 2002 | earliest_precovery_date = 12 October 1990 | mpc_name = {{mp|2002 VE|95}} | mp_category = Plutino[2] | orbit_ref = [3] | epoch = 27 April 2019 (JD 2458600.5) | aphelion = {{Convert|50.167|AU|Tm|abbr=on|lk=on}} (Q) | perihelion = {{Convert|27.943|AU|Tm|abbr=on}} (q) | semimajor = {{Convert|39.055|AU|Tm|abbr=on}} (a) | eccentricity = 0.28452 (e) | period = 244.07 yr (89148.1 d) | avg_speed = | inclination = 16.337° (i) | asc_node = 199.87° (Ω) | mean_anomaly = 26.267° (M) | arg_peri = 206.37° (ω) | satellites = | dimensions = {{val|249.8|+13.5|-13.1}}[4] | mass = | density = | surface_grav = | escape_velocity = | sidereal_day = | axial_tilt = | pole_ecliptic_lat = | pole_ecliptic_lon = | albedo = {{val|0.149|+0.019|-0.016}}[4] | spectral_type = B−V={{val|1.07|0.14}} V−R={{val|0.72|0.05}} B−R={{val|1.79|0.04}} R−I={{val|0.76|0.12}} V−I={{val|1.38|0.15}} B−I={{val|2.47|0.13}}[4] | magnitude = 20.5[4] | abs_magnitude = {{val|5.70|0.06}},[4] 5.3[3] | mean_motion = {{Deg2DMS|0.0040382|sup=ms}} / day (n) | rotation = {{Convert|6.76|h|d|abbr=on|lk=on}} {{Convert|9.97|h|d|abbr=on}} (ambiguous)[5] 6–9 h[11] | observation_arc = 9246 days (25.31 yr) | uncertainty = 2 | moid = {{Convert|26.9598|AU|Tm|abbr=on}} | jupiter_moid = {{Convert|22.9846|AU|Tm|abbr=on}} }}{{mp|(55638) 2002 VE|95}}, also written as 2002 VE95, is a trans-Neptunian object (TNO) with an absolute magnitude of 5.7.[4] A 2:3 orbital resonance with Neptune makes it a plutino.[2] Orbit and rotationAs a plutino {{mp|2002 VE|95}} is locked in 2:3 resonance with Neptune. This means that the ratio of their orbital periods is equal to 3/2.[2] It has been observed 291 times over 19 oppositions with precovery images back to 1990.[3] The rotation period of {{mp|2002 VE|95}} is unknown but it probably lies between 6 and 9 hours.[6] Physical characteristicsThe size of {{mp|2002 VE|95}} is estimated at {{val|249.8|+13.5|-13.1|u=km}}, based on the Herschel Space Telescope measurements of the thermal radiation coming from it.[7] In the visible light this object is from moderately red to very red in color (different observations produced different results) and has a featureless reflectance spectrum.[8] The near-infrared spectrum of {{mp|2002 VE|95}} is flat with two distinct absorption bands of water ice at 1.5 and 2.0 μm. There is the third feature near 2.3 μm of unclear origin.[9] The spectral behavior of this object is similar to 5145 Pholus, a centaur.[9] The surface of {{mp|2002 VE|95}} is heterogeneous—the amount of different ices and non-ice components depends on the observed area. Among the probable surface materials are water ice, methanol ice and various titan/triton tholins. The methanol ice is generally associated with redder areas. The surface of {{mp|2002 VE|95}} appears to be primordial in origin.[10] References1. ^{{cite web|url=http://www.minorplanetcenter.org/iau/lists/TNOs.html |title=List Of Transneptunian Objects |accessdate=2011-01-08 |publisher=IAU Minor Planet Center |archiveurl=https://archive.is/20101027133511/http://www.minorplanetcenter.org/iau/lists/TNOs.html |archivedate=27 October 2010 |deadurl=no |df= }} 2. ^1 2 {{cite web |date=2008-07-17 |title=MPEC 2008-O05 : Distant Minor Planets |publisher=Minor Planet Center & Tamkin Foundation Computer Network |url=http://www.minorplanetcenter.org/mpec/K08/K08O05.html |accessdate=2008-07-23}} 3. ^1 2 {{cite web |type=2017-03-16 last obs |title=JPL Small-Body Database Browser: (55638) 2003 VE95 |url=http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=55638 |accessdate=6 January 2019}} 4. ^{{cite web |title=AstDys 2002VE95 Ephemerides |publisher=Department of Mathematics, University of Pisa, Italy |url=http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.0&n=55638 |accessdate=2010-08-05|deadurl=no}} 5. ^{{Cite journal|url=https://www.aanda.org/articles/aa/pdf/2010/14/aa12340-09.pdf|title=Short-term variability of a sample of 29 trans-Neptunian objects and Centaurs|author1=Thirouin, A.|author2=Ortiz, J. L.|author3=Duffard, R.|author4=Santos-Sanz, P.|author5=Aceituno, F. J.|author6=Morales, N.|date=October 2010|doi=10.1051/0004-6361/200912340|journal=Astronomy and Astrophysics|volume=522}} 6. ^1 {{cite book | last1 = Sheppard | first1 = Scott S. | last2 = Lacerda | first2 = Pedro | last3 = Ortiz | first3 = Jose L. | chapter = Photometric Lightcurves of Transneptunian Objects and Centaurs: Rotations, Shapes, and Densities | title = The Solar System Beyond Neptune | editor1-first = M. Antonietta | editor1-last = Barucci | editor2-last = Boehnhardt | editor2-first = H. | editor3-last = Cruikshank | editor3-first = D.P. | editor4-last = Morbidelli | editor4-first = A. | year = 2008 | publisher = University of Arizona Press | pages = 129–142 | isbn = 978-0-8165-2755-7 | url = http://www.dtm.ciw.edu/users/sheppard/pub/SheppardKBOBook2008.pdf | format = pdf }} 7. ^1 2 3 4 5 {{Cite journal | last1 = Mommert | first1 = Michael| last2 = Harris | first2 = A. W. | last3 = Kiss | first3 = C. | last4 = Pál | first4 = A. | last5 = Santos-Sanz | first5 = P. | last6 = Stansberry | first6 = J. | last7 = Delsanti | first7 = A. | last8 = Vilenius | first8 = E. | last9 = Müller | first9 = T. G. | first10 = N. | last10 = Peixinho| first11 = E. | last11 = Lellouch| first12 = N. | last12 = Szalai| first13 = F. | last13 = Henry| first14 = R. | last14 = Duffard| first15 = S. | last15 = Fornasier| first16 = P. | last16 = Hartogh| first17 = M. | last17 = Mueller| first18 = J. L. | last18 = Ortiz| first19 = S. | last19 = Protopapa| first20 = M. | last20 = Rengel| first21 = A. | last21 = Thirouin| title = TNOs are cool: A survey of the trans-Neptunian region—V. Physical characterization of 18 Plutinos using Herschel-PACS observations| doi = 10.1051/0004-6361/201118562 | journal = Astronomy & Astrophysics | volume = 541 | pages = A93 | date = May 2012| pmid = | pmc = | bibcode = 2012A&A...541A..93M | arxiv = 1202.3657 }} 8. ^{{cite journal|last1=Fornasier|first1=S.|last2=Barucci | first2= M.A. | last3 = De Bergh | first3 = C. | last4 = Alvarez-Candal | first4 = A. | last5 = Demeo | first5 = F. | last6 = Merlin | first6 = F. | last7 = Perna | first7 = D. | last8 = Guilbert | first8 = A. | last9 = Delsanti | first9 = A. | last10 = Dotto | first10 = E. | last11 = Doressoundiram | first11 = A. | title=Visible spectroscopy of the new ESO large programme on trans-Neptunian objects and Centaurs: final results|year=2009|journal=Astronomy and Astrophysics|volume=508|issue=1|pages=457–465|doi=10.1051/0004-6361/200912582 |bibcode=2009A&A...508..457F|arxiv = 0910.0450 }} 9. ^1 {{cite journal | last1 = Barucci | first1 = M. A. | last2 = Merlin | first2 = F. | last3 = Dotto | first3 = E. | last4 = Doressoundiram | first4 = A. | last5 = De Bergh | first5 = C. | title = TNO surface ices Observations of the TNO 55638 (2002 VE95) and analysis of the population's spectral properties | year = 2006 | journal = Astronomy and Astrophysics | volume = 455 | issue = 2 | pages = 725–730 | doi = 10.1051/0004-6361:20064951 | bibcode = 2006A&A...455..725B }} 10. ^{{Cite journal | last1 = Barucci | first1 = M. A. | last2 = Merlin | first2 = F. | last3 = Perna | first3 = D. | last4 = Alvarez-Candal | first4 = A. | last5 = Müller | first5 = T. | last6 = Mommert | first6 = M. | last7 = Kiss | first7 = C. | last8 = Fornasier | first8 = S. | last9 = Santos-Sanz | first9 = P. | last10 = Dotto | first10 = E. | title = The extra red plutino (55638) 2002 VE95 | doi = 10.1051/0004-6361/201118505 | journal = Astronomy & Astrophysics | volume = 539 | pages = A152 | year = 2012 |bibcode = 2012A&A...539A.152B }} External links
3 : Plutinos|Discoveries by NEAT|Astronomical objects discovered in 2002 |
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