(10537) 1991 RY16

Main belt asteroid December 2025 yes (10537) 1991 RY 16 #D6D6D6 Henry E. Holt 15 September 1991 Palomar Observatory (10537) 1991 RY 16 1982 XP 11990 LF Main belt 21 November 2025 (JD 2461000.5) 0 3.04867 AU 2.64575 AU 2.84721 AU 0.070756 7.26027° 62.4603° 162.669° 167.329° 0.205152° / d 1.63537 AU 1.92981 AU 3.291 4.80438 y (1754.80 d) 5.5512 h 7.865 0.269 km 0.313 0.0532027 V-type232 or R-type? 12.83 (10537) 1991 RY 16 is an unnamed asteroid located in the main asteroid belt. It was discovered by astronomer Henry E. Holt at Palomar Observatory on 15 September 1991. It has an uncertain surface mineralogy, with indications that it may be basaltic in composition and thus came from a destroyed differentiated object. Despite this, it has not been confirmed to be a member of any known asteroid family or group, possibly due to past orbital migration. History 1991 RY 16 was first reported to the Minor Planet Center (MPC) by Kiso Observatory, an observatory operated by the University of Tokyo on Mount Ontake, Japan. It was observed on 13 and 14 December 1982, after which it was given the provisional designation 1982 XP 1 by the MPC in 1983.24–25 The asteroid then became lost, not being observed again until 14 June 1990 by Siding Spring Observatory in New South Wales, Australia. Since it was not recognized as the same asteroid, the MPC provisionally designated it 1990 LF.85 It was again observed on 15 and 17 September 1991 by astronomer Henry E. Holt at Palomar Observatory in California, United States. Reported as a new asteroid, its 1991 observations were given the provisional designation 1991 RY 16.52 By June 1992, the asteroid's 1982 and 1991 observations were linked together,149 and its 1990 observation was linked a year later in June 1993.145 Once the asteroid was sufficiently observed, the MPC numbered it (10537) and assigned 1991 RY 16 as its primary provisional designation on 4 May 1999.62 2025, it has yet to be given a name. Orbit 1991 RY 16 orbits the Sun at an average distance—its semi-major axis—of 2.85 astronomical units (AU), placing it in the outer main belt and exterior to the 3:1 mean-motion resonance with Jupiter at 2.5 AU.14L59 It takes 4.8 years to complete one orbit, and it has an orbital inclination of 7.26° with respect to the ecliptic plane. Along its orbit, its distance from the Sun varies between 2.65 AU at perihelion to 3.05 AU at aphelion due to its orbital eccentricity of 0.07. 1991 RY 16 does not belong to any known asteroid family, despite its spectral characteristics indicating that it is a fragment of a larger parent asteroid.14L59 N-body simulations show that its orbit is currently stable and non-resonant, though it lies near two nonlinear secular resonances that have influenced its past orbital migration. Destabilizing mean-motion resonances with Jupiter, such as the 5:2 resonance and the 7:3 resonance, limit how far 1991 RY 16 could have migrated. The upper limit of Yarkovsky effect migration is ~0.1 AU, further constraining where 1991 RY 16 could have originated from.L59 Physical characteristics 1991 RY 16 has an estimated diameter of 7.865 km mi, with an uncertainty of 0.269 km mi. Observations of its lightcurve, or variations in its observed brightness, by the Transiting Exoplanet Survey Satellite (TESS) suggests that it has a rotation period of 5.55 hours. 1991 RY 16 is an asteroid with an ambiguous mineralogy,L58 receiving conflicting assignments as either a V-type asteroid or an R-type asteroid.3873 Its near-infrared spectral features do not match those of V-type asteroids 1459 Magnya and 4 Vesta or R-type asteroid 349 Dembowska, though it shows stronger similarities to the latter. In the 1 and 2 μm absorption bands, it lies between the mineralogies of ordinary chondrites and basaltic achondrites, indicating that it originated from a differentiated parent body. It also lies above the olivine–orthopyroxene mixing line, suggesting that its surface is composed of low- and high-Ca pyroxene and olivine.L58 1991 RY 16 shows an unusually deep absorption at 0.63 μm, which may be caused by the presence of contaminating cations such as Mn2+, Cr3+, and Fe3+.232 Though its mineralogy and location in the asteroid belt restrict where it could have come from, a possible parent body is Dembowska. Dembowska is a 140 km mi on sized asteroid that also has an uncertain surface mineralogy, and past studies have suggested that it may have experienced igneous processes in the past. However, Dembowska is not known for certain to be related to 1991 RY 16.L59–60 See also 7472 Kumakiri – a spectrally similar asteroid References (10537) = 1982 XP1 = 1990 LF = 1991 RY16 https://minorplanetcenter.net/db_search/show_object?object_id=10537 Minor Planet Center 15 December 2025 (7283 obs) 2025-11-25 last obs. JPL Small-Body Database Lookup: 10537 (1991 RY16) https://ssd.jpl.nasa.gov/tools/sbdb_lookup.html#/?sstr=10537 Jet Propulsion Laboratory 15 December 2025 MPC 8323–8436 https://minorplanetcenter.net/iau/ECS/MPCArchive/1983/MPC_19831220.pdf Minor Planet Center Staff Minor Planet Circular Minor Planet Center 20 December 1983 15 December 2025 MPC 17853–18000 https://minorplanetcenter.net/iau/ECS/MPCArchive/1991/MPC_19910330.pdf Minor Planet Center Staff Minor Planet Circular Minor Planet Center 30 March 1991 15 December 2025 MPC 19559–19722 https://minorplanetcenter.net/iau/ECS/MPCArchive/1992/MPC_19920218.pdf Minor Planet Center Staff Minor Planet Circular Minor Planet Center 18 February 1992 15 December 2025 MPC 20191–20366 https://minorplanetcenter.net/iau/ECS/MPCArchive/1992/MPC_19920615.pdf Minor Planet Center Staff Minor Planet Circular Minor Planet Center 15 June 1992 15 December 2025 MPC 22089–22274 https://minorplanetcenter.net/iau/ECS/MPCArchive/1993/MPC_19930604.pdf Minor Planet Center Staff Minor Planet Circular Minor Planet Center 4 June 1993 15 December 2025 MPC 34385–34672 https://minorplanetcenter.net/iau/ECS/MPCArchive/1999/MPC_19990504.pdf Minor Planet Center Staff Minor Planet Circular Minor Planet Center 4 May 1999 15 December 2025 How Are Minor Planets Named? https://www.minorplanetcenter.net/iau/info/HowNamed.html Minor Planet Center Staff Minor Planet Center 15 December 2025 Overview https://www.ioa.s.u-tokyo.ac.jp/kisohp/OVERVIEW/overview_e.html Kiso Observatory Institute of Astronomy, School of Science, The University of Tokyo 15 April 2016 Moskovitz Nicholas A. Lawrence Samuel Jedicke Robert Willman Mark Haghighipour Nader Bus Schelte J. Gaidos Eric A Spectroscopically Unique Main-Belt Asteroid: 10537 (1991 RY16) July 2008 The Astrophysical Journal Letters 682 1 L57–L60 10.1086/591030 0806.2185 2008ApJ...682L..57M Duffard R. Roig F. Two new V-type asteroids in the outer Main Belt? February 2009 Planetary and Space Science 57 2 229–234 10.1016/j.pss.2008.07.009 2009P&SS...57..229D Hardersen Paul S. et al Basalt or Not? Near-infrared Spectra, Surface Mineralogical Estimates, and Meteorite Analogs for 33 Vp-type Asteroids July 2018 The Astronomical Journal 156 1 11 11 10.3847/1538-3881/aac3d2 free 1805.03315 2018AJ....156...11H Medeiros H. et al Compositional characterization of V-type candidate asteroids identified using the MOVIS catalogue September 2019 Monthly Notices of the Royal Astronomical Society 488 3 3866–3875 10.1093/mnras/stz2001 free 2019MNRAS.488.3866M Pál András et al Solar System Objects Observed with TESS—First Data Release: Bright Main-belt and Trojan Asteroids from the Southern Survey March 2020 The Astrophysical Journal Supplement Series 247 1 26 26 10.3847/1538-4365/ab64f0 free 2001.05822 2020ApJS..247...26P Migliorini Alessandra et al. Characterization of V-type asteroids orbiting in the middle and outer main belt June 2021 Monthly Notices of the Royal Astronomical Society 504 2 2019–2032 10.1093/mnras/stab332 free 2021MNRAS.504.2019M 11577/3395033 free External links 10537 (10536) 1991 RZ8 10537 10538 Torode 010537 Category:Discoveries by Henry E. Holt 19910915