| 词条 | 1998 WW31 |
| 释义 |
| minorplanet = yes | name = {{mp|1998 WW|31}} | background = #C2E0FF | image = 2000 (1998 WW31) 1.jpg | image_size = 250 | caption = Hubble Space Telescope image of {{mp|1998 WW|31}} and its satellite in orbit | discovery_ref = [1] | discoverer = M. W. Buie [2] R. Millis [3] | discovery_site = Kitt Peak Obs. | discovered = 18 November 1998 {{small|(first observed only)}} | mpc_name = {{mp|1998 WW|31}} | alt_names = | pronounced = | named_after = | mp_category = TNO [2]{{·}}KBO (hot)[7] {{nowrap|p-DP [8]{{·}}distant [1]{{·}}BIN [10]}} | orbit_ref = | epoch = 27 April 2019 (JD 2458600.5) | uncertainty = 4 | observation_arc = 13.10 yr (4,784 d) | aphelion = 48.476 AU | perihelion = 40.387 AU | semimajor = 44.432 AU | eccentricity = 0.0910 | period = 296.17 yr (108,178 d) | mean_anomaly = 141.84° | mean_motion = {{Deg2DMS|0.0033|sup=ms}} / day | inclination = 6.8240° | asc_node = 237.16° | arg_peri = 50.059° | satellites = 1 {{small|(D: {{val|123|ul=km}}; P: 587 d)}}[10][13] | mean_diameter = {{val|148|ul=km}} {{small|(est. primary)}}[7][10] {{val|192.10|u=km}} {{small|(cal. system)}}[16] {{val|267|u=km}} {{small|(est. system)}}[8] | rotation = | albedo = 0.04 {{small|(est.)}}[8] {{val|0.10}} {{small|(assumed)}}[16] | spectral_type = blue[8] C {{small|(assumed)}}[16] V–I {{=}} {{val|0.910|0.020}}[22] | abs_magnitude = 6.7[16] 6.9[8] }}{{mp|1998 WW|31}}, is a non-resonant trans-Neptunian object and binary system from the Kuiper belt located in the outermost region of the Solar System, approximately {{convert|148|km|mi|abbr=off|sigfig=2|sp=us}} in diameter. It was first observed on 18 November 1998, by American astronomer Marc Buie and Robert Millis at the Kitt Peak National Observatory in Arizona, United States.[2][3][1] According to astronomer Michael Brown, the bluish object is "possibly" a dwarf planet.[8] In December 2000, a minor-planet moon, designated S/2000 ({{mp|1998 WW|31}}) 1 with a diameter of {{convert|123|km|mi|abbr=off|sigfig=2|sp=us}}, was discovered in its orbit.[13] After Charon in 1978, it was the first of nearly 100 satellites since discovered in the outer Solar System.[3][13] Orbit and classificationLocated beyond the orbit of Neptune, {{mp|1998 WW|31}} is a non-resonant classical Kuiper belt object (cubewano) of the so-called hot population, which have higher inclinations than those of the cold population.[7][34] It orbits the Sun at a distance of 40.4–48.5 AU once every 296 years and 2 months (108,178 days; semi-major axis of 44.43 AU). Its orbit has an eccentricity of 0.09 and an inclination of 7° with respect to the ecliptic. The body's observation arc begins at Kitt Peak with its first observation on 18 November 1998.[1] Numbering and namingAs of 2018, this minor planet has not been numbered nor named by the Minor Planet Center.[1] Physical characteristics{{mp|1998 WW|31}} is expected to have a low albedo due to its blue (neutral) color.[8] Other sources assume a higher albedo of 0.10 and 0.16, respectively (see below).[10][16] It has a V–I color index of 0.91,[22] notably lower than the mean-color index for cubewanos, and in between that of comets and Jupiter trojans.[42]{{rp|35}} Satellite{{mp|1998 WW|31}} is a binary minor planet with a minor-planet moon in its orbit. On 22 December 2000, French astronomers Christian Veillet and Alain Doressoundiram in collaboration with J. Shapiro discovered the satellite using the Canada–France–Hawaii Telescope at Mauna Kea on the Big Island of Hawaii, United States. The discovery was announced on 16 April 2001 and received the provisional designation {{nowrap|S/2000 ({{mp|1998 WW|31}}) 1}}.[13]It was the first trans-Neptunian binary discovered after Charon in 1978, the largest satellite in the Pluto–Charon system.[3] Since then nearly 100 trans-Neptunian binaries have been discovered. {{mp|1998 WW|31}} is also one of the most symmetrical binaries known in the Solar System. The satellite has a highly eccentric orbit of approximately 0.8 with an exceptionally long orbital period of 587 days and a semi-major axis of 22,620 kilometers.[3][10] Diameter and albedoWhile the primary measures 148 kilometer, the satellite has a diameter of 123 kilometers (a ratio of 0.883) with a combined system diameter of 192 kilometers.[10][34] The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.10 and calculates a system diameter of 192 kilometers based on an absolute magnitude of 6.7,[16] while Mike Brown finds a diameter of 267 kilometers with a lower albedo of 0.04.[8] Rotation periodAs of 2018, no rotational lightcurve of {{mp|1998 WW|31}} has been obtained from photometric observations. The body's rotation period, pole and shape remain unknown.[16][34] References1. ^1 2 3 4 5 6 {{cite web |title = 1998 WW31 |work = Minor Planet Center |url = https://www.minorplanetcenter.net/db_search/show_object?object_id=1998+WW31 |accessdate = 10 October 2018}} [1][2][3][4][5][6][7][8][9][10][11]2. ^1 2 3 {{cite web |title = List Of Transneptunian Objects |work = Minor Planet Center |url = https://minorplanetcenter.net/iau/lists/TNOs.html |accessdate = 10 October 2018}} 3. ^1 2 3 {{cite web |title = List of Known Trans-Neptunian Objects |work = Johnston's Archive |date = 30 December 2017 |last = Johnston |first= Wm. Robert |url = http://www.johnstonsarchive.net/astro/tnoslist.html |accessdate = 10 October 2018}} 4. ^1 2 3 4 5 6 7 8 {{cite web |title = How many dwarf planets are there in the outer solar system? |publisher = California Institute of Technology |last = Brown |first= Michael E. |url = http://web.gps.caltech.edu/~mbrown/dps.html |accessdate = 10 October 2018}} 5. ^1 2 3 {{cite web |title = Asteroid 1998 WW31 |work = Small Bodies Data Ferret |url = https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=1998+WW31 |accessdate = 10 October 2018}} 6. ^1 2 3 4 5 6 {{cite web |title = Asteroids with Satellites Database – 1998 WW31 and S/2000 (1998 WW31) 1 |work = Johnston's Archive |date = 31 January 2015 |author = Johnston, Wm. Robert |url = http://www.johnstonsarchive.net/astro/astmoons/am1998ww31.html |accessdate = 10 October 2018}} 7. ^1 2 3 4 {{Cite journal |first1 = C. |last1 = Veillet |first2 = A. |last2 = Doressoundiram |first3 = J. |last3 = Shapiro |first4 = J. J. |last4 = Kavelaars |first5 = A. |last5 = Morbidelli |date = April 2001 |title = S/2000 (1998 WW_31) 1 |url = http://www.cbat.eps.harvard.edu/iauc/07600/07610.html#Item1 |journal = IAU Circ. |issue = 7610 |bibcode = 2001IAUC.7610....1V |access-date= 10 October 2018}} 8. ^1 2 3 4 5 {{cite web |title = The binary Kuiper-belt object 1998 WW31 |publisher = Nature |date = 18 April 2002 |url = http://www.cfht.hawaii.edu/~veillet/Nature_final.pdf |format = PDF |accessdate = 10 October 2018}} 9. ^1 2 3 4 5 6 7 {{cite web |title = LCDB Data for (1998 WW31) |publisher = Asteroid Lightcurve Database (LCDB) |url = http://www.minorplanet.info/PHP/GenerateALCDEFPage_Local.php?AstInfo=0%7C1998+WW31 |accessdate = 10 October 2018}} 10. ^1 2 {{cite journal |first1 = O. R. |last1 = Hainaut |first2 = H. |last2 = Boehnhardt |first3 = S. |last3 = Protopapa |date = October 2012 |title = Colours of minor bodies in the outer solar system. II. A statistical analysis revisited |url = https://arxiv.org/pdf/1209.1896.pdf |journal = Astronomy and Astrophysics |volume = 546 |page = 20 |bibcode = 2012A&A...546A.115H |doi = 10.1051/0004-6361/201219566 |arxiv = 1209.1896 |access-date= 10 October 2018}} 11. ^1 {{Cite journal |display-authors = 6 |first1 = S. |last1 = Fornasier |first2 = E. |last2 = Dotto |first3 = O. |last3 = Hainaut |first4 = F. |last4 = Marzari |first5 = H. |last5 = Boehnhardt |first6 = F. |last6 = De Luise |first7 = M. A. |last7 = Barucci |date = October 2007 |title = Visible spectroscopic and photometric survey of Jupiter Trojans: Final results on dynamical families |journal = Icarus |volume = 190 |issue = 2 |pages = 622–642 |bibcode = 2007Icar..190..622F |doi = 10.1016/j.icarus.2007.03.033 |arxiv = 0704.0350}} }} External links{{Commons category}}
4 : Classical Kuiper belt objects|Minor planet object articles (unnumbered)|Binary trans-Neptunian objects|Astronomical objects discovered in 1998 |
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