(612620) 2003 SQ317

Trans-Neptunian object in the Haumea family September 2019 yes (612620) 2003 SQ 317 #C2E0FF (612620) 2003 SQ317 hst.jpg Hubble Space Telescope image of 2003 SQ 317 taken in 2009 CFEPS Mauna Kea Obs. 23 September 2003(first observed only) (612620) 2003 SQ 317 TNOcubewanoSCATEXTD 4 September 2017 (JD 2458000.5) 4 10.12 yr (3,698 days) 45.746 AU 39.231 AU 42.489 AU 0.0767 276.96 yr (101,159 days) 6.9467° 0.0036 ms / day 28.619° 176.34° 191.81° 300 150 km 0.8–2.7 g/cm3 7.210 0.001 h7.5 h B−R1.05 0.18 0.05–0.50 6.2 (612620) 2003 SQ 317 is a classical trans-Neptunian object and member of the Haumea family from the Kuiper belt located in the outermost regions of the Solar System, approximately 300 kilometers in diameter. It was first observed on 23 September 2003, by astronomers of the Canada–France Ecliptic Plane Survey at Mauna Kea Observatories on Hawaii. The surface of 2003 SQ 317 is made of water ice. Physical properties thumb|left|The orbits of multiple objects in the Haumea family. 2003 SQ 317 is not shown in the diagram, though its orbit is similar to that of other objects in the Haumea family. 2003 SQ 317 is a classical Kuiper belt object (cubewano) belonging to the hot population. Its size estimated to lie between 150 and 450 km based on a range of plausible albedos. The object has a large light curve amplitude of about 0.85, which indicates that it has an extremely elongated shape or is a contact binary.https://lacerdapedro.wordpress.com/the-unusual-kbo-2003-sq317/ The Unusual KBO 2003 SQ317 14 November 2013 In the former case the density of 2003 SQ 317 is estimated at 0.86 g/cm3 and its axis ratios at 0.55 and 0.41. If 2003 SQ 317 is a contact binary, which is actually more likely, the density is estimated at 2.67 g/cm3. In the latter case, the components are also thought to be unequal in size with the mass ratio of about 0.3 and axis ratios of about 0.8 and 0.5, respectively, for the primary and secondary components. Origin 2003 SQ 317 was identified as a member of the Haumea family, which is defined based on a common pattern of IR water-ice absorption, neutral visible spectrum and the clustering of the orbital elements. The Haumea family members including (19308) 1996 TO 66, (55636) 2002 TX 300, (120178) 2003 OP 32, (145453) 2005 RR 43 and others all appear to be collisional fragments broken off of the dwarf planet Haumea. See also (139775) 2001 QG 298 References 2012-10-20 last obs. JPL Small-Body Database Browser: (2003 SQ317) http://ssd.jpl.nasa.gov/sbdb.cgi?sstr=3330206 Jet Propulsion Laboratory 14 October 2017 2003 SQ317 Minor Planet Center http://www.minorplanetcenter.net/db_search/show_object?object_id=2003+SQ317 14 October 2017 MPEC P22: DISTANT MINOR PLANETS (2006 Aug. 23.0 TT) 6 August 2006 IAU Minor Planet Center http://www.brera.mi.astro.it/pipermail/mpec/2006-August/002431.html 17 February 2016 https://web.archive.org/web/20160225092651/http://www.brera.mi.astro.it/pipermail/mpec/2006-August/002431.html 25 February 2016 dead Snodgrass, Carry Dumas, Hainaut Characterisation of candidate members of (136108) Haumea's family 10.1051/0004-6361/200913031 Astronomy and Astrophysics 16 December 2009 511 A72 0912.3171 2010A&A...511A..72S 62880843 The unusual Kuiper belt object 2003 SQ317 Pedro Lacerda Andrew McNeill Nuno Peixinho 2014 MNRAS 2014MNRAS.437.3824L 10.1093/mnras/stt2180 437 4 3824–3831 free 1309.1671 Conversion of Absolute Magnitude to Diameter for Minor Planets Department of Physics & Astronomy (Stephen F. Austin State University) Dan Bruton http://www.physics.sfasu.edu/astro/asteroids/sizemagnitude.html 27 December 2009 https://web.archive.org/web/20100323180835/http://www.physics.sfasu.edu/astro/asteroids/sizemagnitude.html 23 March 2010 Marc W. Buie Marc W. Buie Orbit Fit and Astrometric record for 03SQ317 SwRI (Space Science Department) http://www.boulder.swri.edu/~buie/kbo/astrom/03SQ317.html 17 February 2018 External links 3330206 612620 (612620) 2003 SQ 317 612620 612620 20030823 612620