Astronomy:3494 Purple Mountain

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3494 Purple Mountain
Discovery [1]
Discovered byPurple Mountain Obs.
Discovery sitePurple Mountain Obs.
Discovery date7 December 1980
Designations
(3494) Purple Mountain
Named afterPurple Mountain Observatory [1]
(Discovering observatory)
1980 XW · 1962 WV1
1969 UD · 1972 OA
Minor planet categorymain-belt [1][2] · (inner)
Vesta [3][4] · Flora [5]
Orbital characteristics [2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc66.38 yr (24,247 d)
|{{{apsis}}}|helion}}2.6571 AU
|{{{apsis}}}|helion}}2.0419 AU
2.3495 AU
Eccentricity0.1309
Orbital period3.60 yr (1,315 d)
Mean anomaly237.24°
Mean motion0° 16m 25.32s / day
Inclination5.8320°
Longitude of ascending node234.42°
72.646°
Physical characteristics
Mean diameter6.507±0.091 km[6][7]
7.82 km (calculated)[5]
Rotation period2.928±0.001 h (​1⁄2-p.)[8]
5.857±0.001 h[9]
Geometric albedo0.24 (assumed)[5]
0.347±0.035[6][7]
V (SMASS-I Xu)[3] · V [4]
S (assumed)[5]
S/SV (SDSS-MOC)[10]
Absolute magnitude (H)12.7[2][5][7]


3494 Purple Mountain, provisional designation 1980 XW, is a bright Vestian asteroid and a formerly lost minor planet from the inner regions of the asteroid belt, approximately 6.5 kilometers (4 miles) in diameter. First observed in 1962, it was officially discovered on 7 December 1980, by Chinese astronomers at the Purple Mountain Observatory in Nanking, China, and later named in honor of the discovering observatory.[1] The V-type asteroid has a rotation period of 5.9 hours.[5]

Orbit and classification

Purple Mountain is a core member of the Vesta family (401),[3] a giant asteroid family of typically bright V-type asteroids. Vestian asteroids have a composition akin to cumulate eucrites (HED meteorites) and are thought to have originated deep within 4 Vesta's crust, possibly from the Rheasilvia crater, a large impact crater on its southern hemisphere near the South pole, formed as a result of a subcatastrophic collision. Vesta is the main belt's second-largest and second-most-massive body after Ceres.[11][4] Based on osculating Keplerian orbital elements, the asteroid has also been classified as a member of the Flora family (402), a giant asteroid family and the largest family of stony asteroids in the main-belt.[5]

Purple Mountain orbits the Sun in the inner asteroid belt at a distance of 2.0–2.7 AU once every 3 years and 7 months (1,315 days; semi-major axis of 2.35 AU). Its orbit has an eccentricity of 0.13 and an inclination of 6° with respect to the ecliptic.[2] The body's observation arc begins with a precovery taken at Palomar Observatory in December 1951, or 29 years prior to its official discovery observation.[1]

Lost asteroid

Purple Mountain has been a lost minor planet. In November 1962, Purple Mountain was observed as 1962 WV1 at Goethe Link Observatory. A total of three additional observations were taken at Crimea–Nauchnij in 1969 and 1972, when it was designated as 1969 UD and 1972 OA, respectively, but was subsequently lost with no follow-up observations until its official discovery at Nanking in 1980.[1]

Physical characteristics

Based on the Moving Object Catalog (MOC) of the Sloan Digital Sky Survey, Purple Mountain is a common, stony S-type asteroid, with a sequential best-type taxonomy of SV.[10] The Collaborative Asteroid Lightcurve Link (CALL) also assumes it to be a stony S-type.[5]

In the SMASS-I classification by Xu, the asteroid is a V-type. This agrees with its measured high albedo (see below) often seen among the core members of the Vesta family.[11]:23 In 2013, a spectroscopic analysis showed it to have a composition very similar to the cumulate eucrite meteorites, which also suggests that the basaltic asteroid has originated from the crust of 4 Vesta.[4]

Rotation period

In June 2015, a rotational lightcurve of Purple Mountain was obtained from photometric observations by astronomers at Texas A&M University, using the SARA-telescopes of the Southeastern Association for Research and Astronomy consortium. The 0.9-meter SARA-North telescope is located at Kitt Peak National Observatory, Arizona, while the 0.6-meter SARA-South telescope is hosted at the Cerro Tololo Inter-American Observatory in Chile. Lightcurve analysis gave a rotation period of 5.857 hours with a brightness variation of 0.32 magnitude ({{{1}}}).[9] One month later, in July 2015, another period of 2.928 hours and an amplitude of 0.40 magnitude was measured at MIT's George R. Wallace Jr. Observatory ({{{1}}}).[8] The results are in good agreement, apart from the fact that the latter is an alternative, monomodal solution with half the period of the former. CALL adopts the longer, bimodal period solution as the better result in its Lightcurve Data Base, due to the lightcurve's distinct amplitude and the small phase angle of the first observation.[5]

Diameter and albedo

According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Purple Mountain measures 6.507 kilometers in diameter and its surface has an albedo of 0.347,[6][7] while CALL assumes an albedo of 0.24 – derived from the body's classification into the Flora family – and consequently calculates a larger diameter of 7.82 kilometers based on an absolute magnitude of 12.7.[5]

Naming

This minor planet was named in honor of the Purple Mountain Observatory (PMO), an astronomical observatory located in Nanking (Nanjing), China. Built in 1934, the observatory is known for its astrometric observations and for its numerous discoveries of small Solar System bodies. It has played an important role in developing modern Chinese astronomy.[1] The official naming citation was published by the Minor Planet Center on 29 November 1993 (M.P.C. 22829).[12]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 "3494 Purple Mountain (1980 XW)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=3494. 
  2. ↑ 2.0 2.1 2.2 2.3 "JPL Small-Body Database Browser: 3494 Purple Mountain (1980 XW)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2003494. 
  3. ↑ 3.0 3.1 3.2 "Asteroid 3494 Purple Mountain – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=3494+Purple+Mountain#Asteroid%203494%20Purple%20MountainEAR-A-VARGBDET-5-NESVORNYFAM-V3.0. 
  4. ↑ 4.0 4.1 4.2 4.3 Kelley, Michael S.; Vilas, Faith; Gaffey, Michael J.; Abell, Paul A. (September 2003). "Quantified mineralogical evidence for a common origin of 1929 Kollaa with 4 Vesta and the HED meteorites". Icarus 165 (1): 215–218. doi:10.1016/S0019-1035(03)00149-0. Bibcode: 2003Icar..165..215K. https://zenodo.org/record/1259601. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 5.7 5.8 5.9 "LCDB Data for (3494) Purple Mountain". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=3494%7CPurple%20Mountain. 
  6. ↑ 6.0 6.1 6.2 Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Dailey, J. et al. (November 2011). "Main Belt Asteroids with WISE/NEOWISE. I. Preliminary Albedos and Diameters". The Astrophysical Journal 741 (2): 20. doi:10.1088/0004-637X/741/2/68. Bibcode: 2011ApJ...741...68M. 
  7. ↑ 7.0 7.1 7.2 7.3 Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D. et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal 741 (2): 25. doi:10.1088/0004-637X/741/2/90. Bibcode: 2011ApJ...741...90M.  (catalog)
  8. ↑ 8.0 8.1 Kosiarek, M.; Nisley, I.; Patra, K.; Hatano, R.; Bates, H.; Chavez, E. et al. (July 2017). "Rotation Period of Asteroid 3494 Purple Mountain". The Minor Planet Bulletin 44 (3): 171–172. ISSN 1052-8091. Bibcode: 2017MPBu...44..171K. 
  9. ↑ 9.0 9.1 Cantu, Sarah A.; Kozdon, Janus; Montgomery, Kent; Lyons, Vanessa (July 2016). "Lightcurves and Rotational Periods of Three Main-belt Asteroids". The Minor Planet Bulletin 43 (3): 210–212. ISSN 1052-8091. Bibcode: 2016MPBu...43..210C. 
  10. ↑ 10.0 10.1 Carvano, J. M.; Hasselmann, P. H.; Lazzaro, D.; Mothé-Diniz, T. (February 2010). "SDSS-based taxonomic classification and orbital distribution of main belt asteroids". Astronomy and Astrophysics 510: 12. doi:10.1051/0004-6361/200913322. Bibcode: 2010A&A...510A..43C. https://sbnarchive.psi.edu/pds3/non_mission/EAR_A_I0035_5_SDSSTAX_V1_1/data/sdsstax_ast_table.tab. Retrieved 30 October 2019.  (PDS data set)
  11. ↑ 11.0 11.1 Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). "Identification and Dynamical Properties of Asteroid Families". Asteroids IV. pp. 297–321. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131. Bibcode: 2015aste.book..297N. 
  12. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. https://www.minorplanetcenter.net/iau/ECS/MPCArchive/MPCArchive_TBL.html. 

External links



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