(33342) 1998 WT24

Sub-kilometer asteroid May 2020 yes (33342) 1998 WT 24 #FFC2E0 33342 1998 WT24.jpg Tracks of asteroid 1998 WT 24 LINEAR Lincoln Lab's ETS 25 November 1998 (33342) 1998 WT 24 Aten NEO PHA 28 June 2009 (JD 2455010.5) 0 18.98 yr (6,933 days) 1.0187 AU 0.4182 AU 0.7185 AU 0.4179 0.61 yr (222 days) 344.05° 1.6184 ms / day 7.3419° 82.000° 167.30° 0.0097 AU (3.8 LD) 0.35 0.04 km 0.410 km (taken) 0.415 0.040 km 3.6970 0.0002 h 3.697 0.0006 hlightcurve-plots-Warner 3.697 h 3.6977 0.0023 hlcdb-Pravec-2001 3.698 hlcdb-Robinson-2011 3.7 0.1 h 0.34 0.2 0.56 0.2 0.75 0.35 E S 17.9 18.5 0.3 18.69 18.69 0.3 (33342) 1998 WT 24 is a bright, sub-kilometer asteroid, classified as a near-Earth object and potentially hazardous asteroid (PHA) of the Aten group, located in Venus's zone of influence that has frequent close encounters with Mercury, Venus, and Earth. It made a close approach to Earth on 11 December 2015, passing at a distance of about 4.2 million kilometers (2.6 million miles, 11 lunar distances) and reaching about apparent magnitude 11. The asteroid was discovered on 25 November 1998 by LINEAR about four months after a close encounter with the planet Mercury (about 0.047 AU). It measures approximately 400 meters in diameter. It is also one of the best studied PHAs and was the 10th Aten asteroid to be numbered. Classification and orbit left|250px|thumb|Radar observation during 2001 encounter 1998 WT 24 orbits the Sun at a distance of 0.42–1.02 AU once every 7 months (222 days; semi-major axis of 0.72 AU). Its orbit has an eccentricity of 0.42 and an inclination of 7° with respect to the ecliptic. Low aphelion At the time of its discovery, astronomers were trying to find the first Apohele asteroid (one that is always closer to the Sun than Earth). All asteroids known at the time that got closer to the Sun than Earth also crossed Earth's orbit. Earlier that year, David J. Tholen claimed to have spotted the first Apohele asteroid, which was dubbed 1998 DK 36. However, the object was lost without being confirmed. Thus, 1993 DA remained the asteroid with the lowest known aphelion at 1.023 AU. When 1998 WT 24 was discovered, it was found to have a slightly smaller aphelion (1.019 AU) than 1993 DA, and was thus the closest thing to an Apohele asteroid known at the time.IAU Minor Planet Center https://www.minorplanetcenter.net/db_search/show_object?object_id=33342 2024-11-27 www.minorplanetcenter.net It lost its smallest aphelion title almost immediately when (415713) 1998 XX 2 was discovered only a few weeks later (aphelion = 1.014 AU). Asteroids with even smaller aphelions were discovered until February 2003, when finally, an asteroid with an aphelion smaller than 1.000 AU was discovered. This was 163693 Atira, the first confirmed Apohele asteroid. Venus zone of influence April 2021 1998 WT 24 was the second asteroid discovered to be close enough to Venus as to be within the major planet's zone of influence. It is located at about the inner edge of the zone, while (99907) 1989 VA, the first asteroid discovered there, is at about the outer edge. It is possible for planets to capture asteroids located in their sphere of influences into co-orbital relationships such as trojan and horseshoe asteroids. Because of its frequent close encounters with Mercury and Earth, however, it may prove difficult for Venus to keep 1998 WT 24 in a co-orbital relationship for any length of time. Of the six objects in Venus's zone of influence, only Zoozve is currently a co-orbital. Record close encounter 1998 WT 24 is a potentially hazardous asteroid. That means its orbit takes it very close to Earth and if it were to collide with our planet, it would cause devastation on at least a regional scale. On 16 December 2001, it became the first PHA to be observed passing within 5 Lunar Distances (the average distance between Earth and the Moon) from Earth. Other asteroids have come closer, and numerous have even come closer than the Moon, but these have all been small asteroids, incapable of causing much damage to the planet, or much concern. The 2001 encounter was the closest known approach to Earth any PHA had made since (192642) 1999 RD 32 passed by on 27 August 1969. However, 1999 RD 32 was not discovered until September 1999 many years after its closest approach, so no one knew about 1999 RD 32 in 1969. +Notable close-approaches to Earth Date Distance from Earth 1908-12-16 0.00907 AU km mi on on 1956-12-16 0.009054 AU km mi on off 2001-12-16 0.012485 AU km mi on off 2099-12-18 0.012640 AU km mi on off In September 2004, the well known PHA 4179 Toutatis came about 4 Lunar Distances from Earth. Due to its diameter being over ten times larger (5.7 km) and its closer approach, Toutatis at its closest (mag 8.9) was about half an apparent magnitude brighter than 1998 WT 24 was at its closest (mag 9.5). However, Toutatis arrived during a full moon, and thus 1998 WT 24's 2001 encounter is still the most easily observed flyby of an asteroid in history. It also made 1998 WT 24 the first near-Earth asteroid observed to be brighter than magnitude 10. left Frequent inner-planet encounters 1998 WT 24 is a Mercury-crosser asteroid, a Venus-crosser asteroid, and an Earth-crosser asteroid. Because of its relatively low inclination (7.34°), it is able to come close to each of these planets. Its orbit takes it within 0.021 AU of Mercury's orbit, 0.0368 AU of Venus's orbit, and 0.00989 AU of Earth's orbit. It makes frequent encounters with these inner planets. The last time it came close to Mercury, Venus and Earth was 2010, 1977, and 12 November 2004, respectively. The most recent close approach to Earth was on 11 December 2015 at about 4.2 million kilometers (2.6 million miles, 11 lunar distances). The next visit of the asteroid to Earth's neighborhood will be on 11 November 2018, when it will make a relatively distant pass at about 20 million kilometers (12.5 million miles, 52 lunar distances). These encounters perturb its orbit parameters slightly, and each pass reduces its inclination further. Physical characteristics During its close encounters in 2001 and 2015, astronomers were able to make radar images of its surface and determine physical properties that remain unknown for most asteroids. According to the ExploreNEOs Warm Spitzer Exploration Science program, 1998 WT 24 is a bright E-type asteroid with an exceptionally high albedo of 0.75 0.35. Diameter and albedo 1998 WT 24 measures between 350 and 415 meters in diameter and its surface has an albedo between 0.34 and 0.75.lcdb-Robinson-2011 The Collaborative Asteroid Lightcurve Link an albedo of 0.34 and takes a diameter of 410 meters based on an absolute magnitude of 18.69. The asteroid is modestly elongated, approximately 420 × 330 meters.January 2018 Rotation period Several rotational lightcurves of 1998 WT 24 have been obtained from radiometric and photometric observations.lcdb-Pravec-2001lcdb-Robinson-2011 Lightcurve analysis gave a consolidated rotation period of 3.697 hours with a brightness amplitude between 0.19 and 0.65 magnitude (U=3).lightcurve-plots-Warner Future flyby candidate 1998 WT 24 has an orbit that not only crosses Earth's orbit, but is roughly parallel to it at its furthest. This means that during favourable years it is easy to reach from Earth.July 2026 Several times this decade, it will be an easier target than Earth's own Moon. It is high on the list of possible near-Earth asteroid targets for future flybys, landings, mining, or orbit manipulations.July 2026 Numbering and naming This minor planet was numbered by the Minor Planet Center on 18 August 2002. As of 2018, it has not been named. See also List of asteroid close approaches to Earth in 2015 Notes lcdb-Robinson-2011 Robinson (2011) web: rotation period 3.698 hours with a brightness amplitude of 0.26 mag. Quality Code of 3. Summary figures for (33342) at the LCDB lcdb-Pravec-2001 Pravec (2001) web. Observations from December 2001. Rotation period 3.6977 0.0023 hours with a brightness amplitude of 0.28 mag. Quality Code of 3. Summary figures for (33342) at the LCDB and Pravec, P.; Wolf, M.; Sarounova, L. (2001), see Ondrejov data obtained by the NEO Photometric Program and collaborating projects lightcurve-plots-Warner Several lightcurve plots of (33342) obtained at the Center for Solar System Studies by B. D. Warner (2015). References 2017-11-17 last obs. JPL Small-Body Database Browser: 33342 (1998 WT24) https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2033342 Jet Propulsion Laboratory 30 January 2018 (33342) 1998 WT24 Minor Planet Center https://www.minorplanetcenter.net/db_search/show_object?object_id=33342 30 January 2018 MPC/MPO/MPS Archive Minor Planet Center https://www.minorplanetcenter.net/iau/ECS/MPCArchive/MPCArchive_TBL.html 24 February 2018 17 December 2015 Asteroid Looks Even Better Second Time Around https://www.jpl.nasa.gov/news/news.php?feature=4800 NASA JPL 18 December 2015 2001-12-14 Bright Asteroid http://science1.nasa.gov/science-news/science-at-nasa/2001/ast14dec_1/ NASA Science 2014-02-26 https://web.archive.org/web/20140302173107/http://science1.nasa.gov/science-news/science-at-nasa/2001/ast14dec_1/ 2014-03-02 dead (33342) 1998WT24 Ephemerides for December 2015 NEODyS-2 (Near Earth Objects Dynamic Site) https://newton.spacedys.com/neodys/index.php?pc=1.1.3.1&n=33342&oc=500&y0=2015&m0=12&d0=1&h0=0&mi0=0&y1=2015&m1=12&d1=20&h1=0&mi1=0&ti=1.0&tiu=days 2015-10-14 Asteroids and comets rotation curves – (33342) 1998 WT24 Behrend Raoul Geneva Observatory http://obswww.unige.ch/~behrend/page5cou.html#033342 30 January 2018 https://web.archive.org/web/20181111134209/http://obswww.unige.ch/~behrend/page5cou.html#033342 11 November 2018 dead 33342 30 January 2018 Alan W. Harris Michael Mueller Marco Delbó Schelte J. Bus June 2007 Physical characterization of the potentially hazardous high-albedo Asteroid (33342) 1998 WT 24 from thermal-infrared observations Icarus 188 2 414–424 2007Icar..188..414H 10.1016/j.icarus.2006.12.003 121472045 https://hal.archives-ouvertes.fr/hal-00499067/file/PEER_stage2_10.1016%252Fj.icarus.2006.12.003.pdf 6 Michael W. Busch Lance A. M. Benner Steven J. Ostro Jon D. Giorgini Raymond F. Jurgens Randy Rose Daniel J. Scheeres Christopher Magri Jean-Luc Margot Michael C. Nolan Alice A. Hine June 2008 Physical properties of near-Earth Asteroid (33342) 1998 WT24 [ Erratum: 2008Icar..197..375B ] Icarus 195 2 614–621 2008Icar..195..614B 10.1016/j.icarus.2008.01.020 Yu. N. Krugly I. N. Belskaya V. G. Chiorny V. G. Shevchenko N. M. Gaftonyuk November 2002 CCD photometry of near-Earth asteroids in 2001 In: Proceedings of Asteroids 500 903–906 2002ESASP.500..903K Warner, Brian D. April 2016 Near-Earth Asteroid Lightcurve Analysis at CS3-Palmer Divide Station: 2015 October–December The Minor Planet Bulletin 43 2 143–154 32455373 7243997 1052-8091 2016MPBu...43..143W 6 C. A. Thomas D. E. Trilling J. P. Emery M. Mueller J. L. Hora L. A. M. Benner B. Bhattacharya W. F. Bottke S. Chesley M. Delbó G. Fazio A. W. Harris A. Mainzer M. Mommert A. Morbidelli B. Penprase H. A. Smith T. B. Spahr J. A. Stansberry September 2011 ExploreNEOs. V. Average Albedo by Taxonomic Complex in the Near-Earth Asteroid Population The Astronomical Journal 142 3 12 2011AJ....142...85T 10.1088/0004-6256/142/3/85 free External links IMAGES OF ASTEROID 1998 WT24 NASA Physical properties of near-Earth Asteroid (33342) 1998 WT24 shape model of 1998 WT24 from Goldstone and Arecibo radar imaging 2001 Radar Investigations of Asteroid 33342 (1998 WT24) in December 2001 with Evpatoria-Medichina and Goldstone-Medichina Bistatic Systems 33342 33342 1998WT24 33342 (33341) 1998 WA5 33342 (33342) 1998 WT 24 33343 Madorobin 033342 033342 033342 033342 20151211 19981125 033342