(55636) 2002 TX300
{{Short description|Kuiper Belt object}}
{{DISPLAYTITLE:{{mp|(55636) 2002 TX|300}}}}
{{Use dmy dates|date=April 2020}}
{{Infobox planet
| minorplanet = yes
| background = #C2E0FF
| name = {{mp|(55636) 2002 TX|300}}
| image = 55636-2002tx300 hst.jpg
| image_size =
| caption = Hubble Space Telescope image of {{mp|2002 TX|300}} taken in 2005
| discovery_site = Palomar Mountain
| discovered = 15 October 2002
| mpc_name = {{mp|(55636) 2002 TX|300}}
| alt_names =
| mp_category = {{Hlist
| TNO
| Cubewano
}}
| epoch = 13 January 2016 (JD 2457400.5)
| semimajor = {{Convert|43.116|AU|Tm|abbr=on}}
| perihelion = {{Convert|37.8672|AU|Tm|abbr=on}}
| aphelion = {{Convert|48.365|AU|Tm|abbr=on|lk=on}}
| eccentricity = 0.12174
| period = 283.12 yr (103408 d)
| inclination = 25.87838°
| asc_node = 324.6984°
| arg_peri = 338.958°
| mean_anomaly = 73.7618°
| mean_radius = {{Ubl
| {{val|143|5|u=km}} (occultation)
| {{val|320.6|125.2|103.4|p=<|u=km}} (Spitzer two-band thermal model)
}}
| mass = {{Val|1.2e19|p=~|u=kg}} (assumed)
| sidereal_day = 0.504 d (12.101 h)
| spectral_type = {{Ubl
| (Neutral)
| B–V {{=}} 0.66
}}
| albedo = {{Ubl
| {{val|.173|0.203|0.083|p=> }} (Spitzer)
}}
| single_temperature = < 41 K
| mean_motion = {{Deg2DMS|0.00348134|sup=ms}} / day
| rotation = {{Convert|8.12|h|d|abbr=on|lk=on}}
| observation_arc = 22380 days (61.27 yr)
| uncertainty = 2
}}
{{mp|(55636) 2002 TX|300}} is a bright Kuiper belt object in the outer Solar System estimated to be about {{convert|286|km|mi}} in diameter. It is a large member of the Haumea family that was discovered on 15 October 2002 by the Near-Earth Asteroid Tracking (NEAT) program.
{{mp|2002 TX|300}} is a classical Kuiper belt object with an absolute magnitude between that of 50000 Quaoar and 20000 Varuna. {{mp|2002 TX|300}} has the most eccentric and inclined orbit of the three.
A variability of the visual brightness was also detected which could fit to 7.9 h or 15.8 h rotational period (the distinction between single or double-peaked curved could not be made with confidence). The changes in brightness are quite close to the error margin and could also be due to an irregular shape.
Orbit
File:TheKuiperBelt Orbits 2002TX300 2003EL61.svg (grey)]]
File:TheKuiperBelt Orbits 2002TX300 2003EL61 PolarView.svg
The adjacent diagrams show polar and ecliptic views of the orbits of the two cubewanos. The perihelia (q) and the aphelia (Q) are marked with the dates of passage. The present positions (as of April 2006) are marked with the spheres, illustrating relative sizes and differences in albedo (both objects appear neutral in the visible spectrum).
{{mp|2002 TX|300}} is classified as a classical Kuiper belt object and follows an orbit very similar to that of {{dp|Haumea}}: highly inclined (26°) and moderately eccentric (e ~0.12), far from Neptune's perturbations (perihelion at ~37 AU). Other mid-sized cubewanos follow similar orbits as well, notably {{mpl-|55637|2002 UX|25}} and {{mpl-|55565|2002 AW|197}}.
It has been observed 303 times, with precovery images back to 1954.
Size
File:Iau dozen.jpg suggested that {{mp|2002 TX|300}} could be as large as Quaoar]]
File:TX300-2009Nov16-04UT.jpg 19.4) as viewed with a 24" telescope]]
In 2004, the non-detection of IR thermal emissions put an upper limit of {{convert|709|km|mi}} on its diameter and a lower limit on the albedo of 0.19. In a 2006 International Astronomical Union press release discussing the IAU 2006 draft proposal, a diagram suggested that {{mp|2002 TX|300}} could be as large as 50000 Quaoar. The artist's diagram was largely based on the concept that {{mp|2002 TX|300}}, with an absolute magnitude (H) of 3.4, may have an albedo around 0.08, which resulted in an overly optimistic diameter estimate of around {{convert|1000|km|mi}}.
In 2007, measurements by the Spitzer Space Telescope showed that it may be less than {{convert|641|km|mi}} in diameter. In 2008, it was considered to be a dwarf planet candidate based on its small lightcurve amplitude (which would imply a spheroidal shape) and the assumption that it was larger than {{convert|450|km|mi}} in diameter. However, because {{mp|2002 TX|300}} is a member of the Haumea family, it is more likely to have a high albedo of around 0.7, which would result in a diameter of about {{convert|360|km|mi}}.
{{mp|2002 TX|300}} occulted a relatively bright apparent magnitude 13.1 star in the constellation of Andromeda on 9 October 2009. This event was visible from Australia, possibly New Zealand, and the southern United States and Mexico. The RA and declination for this event was about [http://skyview.gsfc.nasa.gov/cgi-bin/runquery.pl?Interface=quick&Position=00+37+13.64+%2B28+22+23.2&SURVEY=Digitized+Sky+Survey 00 37 13.64 +28 22 23.2.]: detailed information for observers was made available. The occultation produced a diameter of {{convert|286|km|mi}}, suggesting an albedo of about 0.88.
Surface
The spectrum in the visible and near-infrared rages is very similar to that of Charon, characterized by neutral to blue slope (1%/1000 Å) with deep (60%) water absorption bands at 1.5 and 2.0 μm. Mineralogical analysis indicates a substantial fraction of large ice (H2O) particles. The signal-to-noise ratio of the observations was insufficient to differentiate between amorphous or crystalline ice (crystalline ice was reported on Charon, Quaoar and Haumea). The proportion of highly processed organic materials (tholins), typically present on numerous trans-Neptunian objects, is very low. As suggested by Licandro et al. 2006, this lack of irradiated mantle suggest either a recent collision or comet activity.
Origin
{{Main|Haumea family}}
Common physical characteristics with the dwarf planet Haumea together with similar orbit elements led to suggestion that {{mp|2002 TX|300}} was a member of the Haumean collisional family. The object, together with other members of the family ({{mpl|(19308) 1996 TO|66}}, {{mpl|(24835) 1995 SM|55}}, {{mpl|(120178) 2003 OP|32}} and {{mpl|(145453) 2005 RR|43}}), would be created from ice mantle ejected from the proto-Haumea as result of a collision with another large (around {{convert|1660|km|mi}}) body.
{{clear|left}}
References
{{Reflist|30em|refs=
|type=last observation: 2015-12-05
|title=JPL Small-Body Database Browser: 55636 (2002 TX300)
|url=https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=55636
|accessdate=6 April 2016}}
|title=MPEC 2009-R09 :Distant Minor Planets (2009 SEPT. 16.0 TT)
|date=2009-09-04
|publisher=IAU Minor Planet Center
|url=http://www.cfa.harvard.edu/mpec/K09/K09R09.html
|accessdate=2009-10-04}}
|author=Marc W. Buie
|author-link=Marc W. Buie
|type=2013-12-04 using 341 observations over 59 years
|title=Orbit Fit and Astrometric record for 55636
|publisher=SwRI (Space Science Department)
|url=http://www.boulder.swri.edu/~buie/kbo/astrom/55636.html
|accessdate=2014-10-14}}
|last=Elliot|first=J. L.
|title=Size and albedo of Kuiper belt object 55636 from a stellar occultation
|date=2010
|journal=Nature|volume=465|pages=897–900
|doi=10.1038/nature09109|pmid=20559381|issue=7300
|bibcode= 2010Natur.465..897E
|author2=Person, M. J.
|last3=Zuluaga|first3=C. A.|display-authors=2
|last4=Bosh|first4=A. S.|last5=Adams|first5=E. R.
|last6=Brothers|first6=T. C.|last7=Gulbis|first7=A. A. S.
|last8=Levine|first8=S. E.|last9=Lockhart|first9=M.
|s2cid=4431420
|url=http://www.dtic.mil/cgi-bin/GetTRDoc?AD=ADA541934&Location=U2&doc=GetTRDoc.pdf|archive-url=https://web.archive.org/web/20140222100203/http://www.dtic.mil/cgi-bin/GetTRDoc?AD=ADA541934&Location=U2&doc=GetTRDoc.pdf|url-status=dead|archive-date=22 February 2014}}
|title=Physical Properties of Kuiper Belt and Centaur Objects: Constraints from Spitzer Space Telescope
|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
}}
Using a spherical radius of 143 km; volume of a sphere * an assumed density of {{Val|1.0|u=g/cm3}} yields a mass ({{Nowrap|m = d × v}}) of {{Val|1.224e19|u=kg}}
|author=Snodgrass, Carry
|author2=Dumas, Hainaut
|title=Characterisation of candidate members of (136108) Haumea's family
|journal=Astronomy and Astrophysics
|date=16 December 2009
|arxiv=0912.3171
|doi = 10.1051/0004-6361/200913031
|bibcode = 2010A&A...511A..72S
|volume=511
|pages=A72|s2cid=62880843
}}
{{cite journal
|title=The Youthful Appearance of the 2003 EL61 Collisional Family
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|author2=Bradley E. Schaefer
|author3=Martha W. Schaefer
|author4=Suzanne W. Tourtellotte
|date=2008
|doi=10.1088/0004-6256/136/4/1502
|journal=The Astronomical Journal
|volume=136
|issue=4
|pages=1502
|arxiv=0804.2864
|bibcode = 2008AJ....136.1502R|s2cid=117167835
}}
|title = (55636) 2002TX300 Ephemerides
|website = AstDys
|publisher = Department of Mathematics, University of Pisa, Italy
|url = https://newton.spacedys.com/astdys/index.php?pc=1.1.3.0&n=2002TX300
|accessdate = 2009-03-16
|archiveurl = https://web.archive.org/web/20110526232036/http://hamilton.dm.unipi.it/astdys/index.php?pc=1.1.3.0&n=2002TX300
|archivedate = 2011-05-26
|url-status = dead
}}
|author=Grundy, W. M
|title=Diverse albedos of small trans-neptunian objects
|journal=Icarus
|volume=176|issue=1|pages=184–191|date=2005
|doi=10.1016/j.icarus.2005.01.007
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|first2=K
|last3=Stephens
|first3=D
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|arxiv= astro-ph/0502229 |s2cid=118866288
}} ([https://arxiv.org/abs/astro-ph/0502229 Preprint on arXiv])
|title=The Path to Defining Planets
|first=Owen |last=Gingerich |author-link=Owen Gingerich
|work=Harvard-Smithsonian Center for Astrophysics and IAU EC Planet Definition Committee chair
|date=2006-08-16
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|accessdate=2007-03-13
|page=4 }}
|title=Conversion of Absolute Magnitude to Diameter for Minor Planets
|publisher=Department of Physics & Astronomy (Stephen F. Austin State University)
|author=Dan Bruton
|url=http://www.physics.sfasu.edu/astro/asteroids/sizemagnitude.html
|accessdate=2009-12-27 |archiveurl= https://web.archive.org/web/20100323180835/http://www.physics.sfasu.edu/astro/asteroids/sizemagnitude.html |archivedate=23 March 2010}}
|date=October 13, 2008
|title=Dwarf Planet & Plutoid Headquarters
|publisher=Portal Uruguayo de Astronomía
|author=Gonzalo Tancredi
|author2=Sofía Favre
|name-list-style=amp
|url=http://www.astronomia.edu.uy/dwarfplanet/list.html
|accessdate=2010-09-22}} [http://www.lpi.usra.edu/meetings/acm2008/pdf/8261.pdf (Which are the dwarfs in the Solar System?)]
|date=2009-12-29
|title=A ghost of Christmas past
|publisher=Mike Brown's Planets (blog)
|author=Mike Brown
|url=http://www.mikebrownsplanets.com/2009/12/ghost-of-christmas-past.html
|accessdate=2009-12-29
|authorlink=Michael E. Brown
|archiveurl=https://web.archive.org/web/20100102060222/http://www.mikebrownsplanets.com/2009/12/ghost-of-christmas-past.html
|archivedate=2 January 2010}}
|title = (55636) 2002 TX300 / UCAC2 41650964 event on 2009 Oct 09, 10:28 UT
|author = Steve Preston
|url = http://www.asteroidoccultation.com/2009_10/1009_55636_18018_Summary.txt
|accessdate = 2009-10-05
|archiveurl = https://archive.today/20091008145306/http://www.asteroidoccultation.com/2009_10/1009_55636_18018_Summary.txt
|archivedate = 2009-10-08
|url-status = dead
}}
{{Cite web |url=http://occult.mit.edu/research/occultations/kbo/55636/55636.20091009/index.html |title=55636.20091009 Occultation October 09, 2009 |author=Michael J. Person |date=2009-10-08 |publisher=Planetary Astronomy Lab. MIT |accessdate=2009-10-09}}
{{Cite journal
| title = The water ice rich surface of (145453) 2005 RR43: a case for a carbon-depleted population of TNOs?
| author = Pinilla-Alonso, N.
| author2 = Licandro, J.
| author3 = Gil-Hutton, R.
| author4 = Brunetto, R.
| journal=Astronomy and Astrophysics
| date=June 2007|volume=468|issue=1
| bibcode=2007A&A...468L..25P
| doi= 10.1051/0004-6361:20077294
| page=L25–L28 |arxiv= astro-ph/0703098| s2cid = 18546361
}}
}}
External links
{{Commons category}}
- [https://newton.spacedys.com/astdys/index.php?pc=1.1.0&n=2002TX300 AstDys] orbital elements
- {{JPL small body|id=55636}}
{{Minor planets navigator | |number=55636 |PageName={{mp|(55636) 2002 TX|300}} |(55637) 2002 UX25}}
{{Haumea}}
{{Solar System}}
{{Trans-Neptunian objects}}
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Category:Classical Kuiper belt objects