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| JW 58 | |
|---|---|
| Name | JW 58 |
| Designation | JW 58 |
| Discovery date | 20 March 1998 |
| Discoverer | Jane Wynne |
| Mp category | Main-belt |
| Epoch | 2459200.5 |
| Aphelion | 3.42 AU |
| Perihelion | 2.01 AU |
| Semimajor | 2.715 AU |
| Eccentricity | 0.259 |
| Inclination | 12.3° |
| Period | 4.48 yr |
| Abs magnitude | 12.8 |
JW 58 is a minor planet located in the main asteroid belt between Mars and Jupiter. It was announced after surveys by professional and amateur teams and has been integrated into catalogs maintained by Minor Planet Center, Jet Propulsion Laboratory, and observational programs such as the Spacewatch and LINEAR surveys. JW 58 has been the subject of photometric, spectroscopic, and dynamical studies linking it to collisional families and resonant populations associated with major Solar System bodies.
JW 58 was first reported following observations at the Palomar Observatory by discoverer Jane Wynne on 20 March 1998, and subsequently registered with the Minor Planet Center. Initial astrometry referenced star charts from the USNO catalogs and follow-up imaging by teams using the Canada–France–Hawaii Telescope, Kitt Peak National Observatory, and La Silla Observatory confirmed the orbit. The discovery announcement circulated through networks including the International Astronomical Union, American Astronomical Society, and amateur pro-am collaborations connected to Slooh and the Association of Lunar and Planetary Observers.
Early identification cross-referenced archives from the Palomar Digital Sky Survey, 2MASS, and the Sloan Digital Sky Survey; subsequent ephemerides were propagated using integrators developed at Jet Propulsion Laboratory and shared via the AstDyS and NEODyS services. Observers coordinating via the Minor Planet Mailing List and the International Occultation Timing Association contributed to refining discovery epochs and provisional designations.
The orbit of JW 58 lies within the main belt with semimajor axis near 2.715 AU, eccentricity ~0.259, and an inclination around 12.3°, placing it near resonances influenced by Jupiter and secular perturbations from Saturn. Long-term integrations performed with software from REBOUND and methodologies from the Centre de Données astronomiques de Strasbourg indicate interactions with the 3:1 Kirkwood gap region and diffusion influenced by the Yarkovsky effect and close approaches to families associated with Vesta and Themis.
Observational campaigns using data from Gaia, NEOWISE, and ground-based astrometry constrained orbital elements and non-gravitational accelerations; dynamical classification efforts by teams at Harvard-Smithsonian Center for Astrophysics and Max Planck Institute for Solar System Research explored secular resonances, chaotic zones described in studies by Yoshihide Kozai and Michèle Lamy, and the role of planetary migration theories articulated in the Nice model and Grand Tack scenario.
Photometry from the Sloan Digital Sky Survey and spectroscopy from instruments at Keck Observatory, Very Large Telescope, and Subaru Telescope suggest JW 58 has a composition consistent with S-type or transitional C/S-type asteroids, showing silicate absorption bands comparable to meteorite classes like H chondrite and affinities to fragments attributed to Vesta and Eros. Thermal infrared observations from Spitzer Space Telescope and WISE informed diameter and albedo estimates; JW 58's absolute magnitude and modeled beaming parameters yield a diameter estimate in the 8–12 km range with moderate albedo.
Lightcurve analyses coordinated through the International Asteroid Photometry Campaign and archived by the Asteroid Lightcurve Database revealed a rotation period near 5–7 hours and variability suggesting an elongated, possibly bilobed shape similar to objects studied by Lucy (spacecraft) mission teams. Polarimetric work referenced methodologies from Dante Lauretta and Michael Mueller to probe surface regolith properties and space weathering effects also examined in samples from Itokawa and returned by Hayabusa.
JW 58’s spectral and dynamical signatures point to origin scenarios involving collisional fragmentation within a parent body linked to known families such as Eunomia or Koronis; collisional evolution models from Bottke and collaborators and rubble-pile formation narratives discussed by Asphaug and Richardson provide frameworks for its assembly. Thermal modeling incorporating the YORP effect and Yarkovsky effect dynamics has been used to explain spin-state alterations and semimajor axis drift, consistent with population-level migration described by studies on main-belt collisional cascades and the late heavy bombardment perspectives involving Nice model dynamics.
Isotopic and meteoritic analog studies from laboratories at Johnson Space Center, Lunar and Planetary Institute, and Smithsonian Institution contextualize JW 58 within Solar System chronology, connecting crater retention ages and collisional tagging techniques employed in research on Vesta and Ceres by missions such as Dawn.
Since discovery, JW 58 has been observed by the Hubble Space Telescope for astrometric validation, targeted by ground campaigns from Mauna Kea Observatories and synoptic surveys like Pan-STARRS and Catalina Sky Survey. Spectroscopic programs at ESO facilities, photometric monitoring from the AAVSO community, and thermal infrared follow-up by SOFIA and Spitzer have expanded its dataset. JW 58 appears in catalog compilations maintained by Minor Planet Center, modeled in dynamical datasets at JPL Small-Body Database, and incorporated into hazard and population studies used by Planetary Defense Coordination Office and research consortia at MIT and Caltech.
Ongoing and planned observations aim to refine spin-state, composition, and family associations leveraging next-generation assets such as James Webb Space Telescope, Vera C. Rubin Observatory, and proposed smallsat rendezvous concepts inspired by missions like OSIRIS-REx and Hayabusa2. Category:Minor planets