(55636) 2002 TX300

Infobox Planet
bgcolour=#FFFFC0
name=mp|(55636) 2002 TX|300
discovery=yes
discoverer=NEAT
discovered=October 15, 2002
mp_name=mp|(55636) 2002 TX|300
alt_names="none"
mp_category=TNO
(cubewano)cite web|date=2008-07-17 |title=MPEC 2008-O05 : Distant Minor Planets (2008 Aug. 2.0 TT) |author=Brian G. Marsden |work=IAU Minor Planet Center |publisher=Harvard-Smithsonian Center for Astrophysics |url=http://cfa-www.harvard.edu/iau/mpec/K08/K08O05.html |accessdate=2008-10-01]
epoch=December 31, 2006 (JD 2454100.5)
semimajor=6453.572 Gm (43.139 AU)
perihelion=5654.528 Gm (37.798 AU)
aphelion=7252.615 Gm (48.481 AU)
eccentricity=0.124
period=103492.895 d (283.35 a)
inclination=25.856°
asc_node=324.575°
arg_peri=338.907°
mean_anomaly=62.175°
avg_speed=4.52 km/s
physical_characteristics=yes
dimensions=470?cite web
title=Conversion of Absolute Magnitude to Diameter
publisher=IAU: Minor Planet Center
url=http://www.cfa.harvard.edu/iau/lists/Sizes.html
accessdate=2008-06-12] -709 km
radius=265?-354.5 km
mass=1.6–3.7e|20? kg
density=2.0? g/cm³
surface_grav=0.15–0.20? m/s²
escape_velocity=0.28–0.37? km/s
sidereal_day=0.33 or 0.66 d (7.9 or 15.8 h)
spectral_type=(neutral) B-V=0.63; V-R=0.36 [cite web
date=2004
title=The Meudon Multicolor Survey (2MS) of Centraurs and Trans-Neptunian objects
url=http://calys.obspm.fr/~pcorps/TNO/publi/doressoundiram2004_final_2MS.pdf
last=Doressoundiram
accessdate=2006-11-06]
abs_magnitude=3.09cite web
date=2006-10-30 last obs
title=JPL Small-Body Database Browser: 55636 (2002 TX300)
url=http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=55636
accessdate=2008-06-12]
albedo=>0.19
single_temperature=<41 K

mp|(55636) 2002 TX|300 is a large Trans-Neptunian object (TNO) discovered in October 15, 2002 by the NEAT program.

A Classical Kuiper Belt object with the 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 irregular shapeJ. L. Ortiz, A. Sota, R. Moreno, E. Lellouch, N. Biver, A. Doressoundiram, P. Rousselot, P. J. Gutiérrez, I. Márquez, R. M. González Delgado and V. Casanova "A study of Trans-Neptunian object (55636) mp|2002 TX|300", Astronomy & Astrophysics, 420 (2004), Issue 1, pp. 383-388. [http://www.edpsciences.org/articles/aa/pdf/2004/22/aa0507.pdf Abstract.] ] .

ize

The non-detection of IR thermal emissions puts an upper limit of 709 km on its diameter and a lower limit on the albedo of 0.19.cite journal
author=Grundy, W. M
coauthors=Noll, K. S.; Stephens, D. C.
title=Diverse albedos of small trans-neptunian objects
journal=Icarus
volume=176 |issue=1 |pages=184–191 |year=2005
doi=10.1016/j.icarus.2005.01.007
accessdate=2006-10-22 ( [http://arxiv.org/abs/astro-ph/0502229 Preprint on arXiv.] )]

Orbit

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-sizes cubewanos follow similar orbits as well, notably mpl|2002 UX|25 and mpl|2002 AW|197.

The 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).

urface

The spectrum in visible and infrared is very similar to that of Charon characterised by neutral to blue slope (1%/1000 Å) with deep (60%) water absorption bands at 1.5 and 2.0 μm)J.Licandro, L. di Fabrizio, N. Pinilla-Alonso, J. de León, and E. Oliva "Trans-Neptunian object (55636) mp|2002 TX|300, a fresh icy surface in the outer Solar System." 2006, A&A,457,329-333 [http://adsabs.harvard.edu/abs/2006A&A...457..329L Abstract] ] .Mineralogical analysis indicates a substantial fraction of large ice (H₂O) particles.Pinilla-Alonso, N.; Licandro, J.; Campins, H. "Mineralogical analysis of two different kind of icy surfaces in the trans-neptunian belt, TNOs (50000) Quaoar and mp|2002 TX|300", American Astronomical Society, DPS meeting #36, #11.07 (2004). [http://adsabs.harvard.edu/abs/2004DPS....36.1107P Abstract.] ] The signal/noise ratio of the observations was insufficient to differentiate between amorphous or crystalline ice (crystalline ice was reported on Charon, (50000) Quaoar and Haumea). The proportion of highly processed organic materials (tholins), typically present on numerous trans-Neptunian objects, is very low. This lack of irradiated mantle suggest either a recent collision or comet activity.

Origin

Common physical characteristics with the dwarf planet Haumea together with similar orbit elements led to suggestion that mp|2002 TX|300 is 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 (~1660 km) body.Michael E. Brown, Kristina M. Barkume, Darin Ragozzine & Emily L. Schaller, "A collisional family of icy objects in the Kuiper belt", Nature, 446, (March 2007), pp 294-296.]

External links

* [http://hamilton.dm.unipi.it/cgi-bin/astdys/astibo?objects:2002TX300;main AstDys] orbital elements
* [http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2002TX300;orb=1;view=Far Orbital simulation] from JPL (Java) / [http://ssd.jpl.nasa.gov/horizons.cgi?find_body=1&body_group=sb&sstr=2002TX300 Ephemeris]

References