Astronomy:10001 Palermo

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10001 Palermo
Discovery[1][2]
Discovered byL. Chernykh
Discovery siteCrimean Astrophysical Obs.
Discovery date8 October 1969
Designations
(10001) Palermo
Named afterPalermo (Italian city)[1]
1969 TM1 · 1991 RS27
Minor planet categorymain-belt[1][3] · (inner)
Vestian[4][5]
Orbital characteristics[3]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc63.50 yr (23,192 d)
|{{{apsis}}}|helion}}2.6955 AU
|{{{apsis}}}|helion}}2.0579 AU
2.3767 AU
Eccentricity0.1341
Orbital period3.66 yr (1,338 d)
Mean anomaly66.907°
Mean motion0° 16m 8.4s / day
Inclination7.4247°
Longitude of ascending node40.160°
357.81°
Physical characteristics
Mean diameter4.123±0.657 km[6]
4.31 km (calculated)[4]
Rotation period213.368±2.0136 h[7]
Geometric albedo0.20 (assumed)[4]
0.341±0.134[6]
S (assumed)[4]
Absolute magnitude (H)13.71±0.42[8]
13.745±0.006 (R)[7]
13.80[6] · 13.9[3] · 14.19[4]


10001 Palermo, provisional designation 1969 TM1, is a Vestian asteroid and a slow rotator from the inner regions of the asteroid belt, approximately 4 kilometers (2.5 miles) in diameter. It was discovered on 8 October 1969, by Soviet–Russian astronomer Lyudmila Chernykh using a 0.4-meter double astrograph at the Crimean Astrophysical Observatory in Nauchnij on the Crimean peninsula.[2] The asteroid is likely elongated in shape and has a long rotation period of 213 hours.[4] It was named for the Italian city of Palermo to commemorate the discovery of Ceres two hundred years earlier.[1]

Orbit and classification

Orbit of Palermo (blue), the inner planets and Jupiter

Palermo is a member of the Vesta family (401).[4][5] Vestian asteroids have a composition akin to cumulate eucrites. They are thought to have originated deep within 4 Vesta's crust – the family's parent body – possibly from the large Rheasilvia crater on its southern hemisphere near the South pole, formed as a result of a subcatastrophic collision. Vesta is also the asteroid belt's second-largest and second-most-massive body after Ceres.[9][10]

It orbits the Sun in the inner asteroid belt at a distance of 2.1–2.7 AU once every 3 years and 8 months (1,338 days; semi-major axis of 2.38 AU). Its orbit has an eccentricity of 0.13 and an inclination of 7° with respect to the ecliptic.[3] The body's observation arc begins with a precovery taken at the Palomar Observatory on July 1954, more than 12 years prior to its official discovery observation at Nauchnij.[1]

Physical characteristics

Palermo is an assumed S-type,[4] while the overall spectral type for members of the Vesta family is that of a V-type.[9]:23

Slow rotator

In September 2013, a rotational lightcurve of Palermo was obtained from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave an exceptionally long rotation period of 213.368 hours with a high brightness amplitude of 0.97 magnitude, indicative for an elongated shape ({{{1}}}).[7]

Palermo is a slow rotator as most asteroids have periods shorter than 20 hours. There are more than 600 known slow rotators with a spin rate of more than 100 hours.

Diameter and albedo

According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Palermo measures 4.12 kilometers in diameter and its surface has a high albedo of 0.34.[6] The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 4.31 kilometers based on an absolute magnitude of 14.19.[4]

Naming

This minor planet was named after the Italian city of Palermo, capital of Sicily and location of the Palermo Observatory, where the dwarf planet and first asteroid Ceres was discovered by Giuseppe Piazzi on 1 January 1801. The official naming citation was published by the Minor Planet Center on the 200th anniversary of that discovery on 9 January 2001 (M.P.C. 41937).[1][2][11]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 "10001 Palermo (1969 TM1)". Minor Planet Center. https://www.minorplanetcenter.net/db_search/show_object?object_id=10001. Retrieved 28 March 2018. 
  2. ↑ 2.0 2.1 2.2 Chernykh, L. I. (September 2002). "Minor Planet(10001) is named Palermo". In Memorie della Società' Astronomica Italiana 73 (3): 624. Bibcode: 2002MmSAI..73..624C. 
  3. ↑ 3.0 3.1 3.2 3.3 "JPL Small-Body Database Browser: 10001 Palermo (1969 TM1)". Jet Propulsion Laboratory. https://ssd.jpl.nasa.gov/sbdb.cgi?sstr=2010001. Retrieved 28 March 2018. 
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 4.7 4.8 "LCDB Data for (10001) Palermo". Asteroid Lightcurve Database (LCDB). http://www.minorplanet.info/PHP/generateOneAsteroidInfo.php?AstInfo=10001%7CPalermo. Retrieved 28 March 2018. 
  5. ↑ 5.0 5.1 "Asteroid 10001 Palermo – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. https://sbntools.psi.edu/ferret/SimpleSearch/results.action?targetName=10001+Palermo#Asteroid%2010001%20PalermoEAR-A-VARGBDET-5-NESVORNYFAM-V3.0. Retrieved 27 October 2019. 
  6. ↑ 6.0 6.1 6.2 6.3 Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T. et al. (December 2015). "NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos". The Astrophysical Journal 814 (2): 13. doi:10.1088/0004-637X/814/2/117. Bibcode: 2015ApJ...814..117N. 
  7. ↑ 7.0 7.1 7.2 Waszczak, Adam; Chang, Chan-Kao; Ofek, Eran O.; Laher, Russ; Masci, Frank; Levitan, David et al. (September 2015). "Asteroid Light Curves from the Palomar Transient Factory Survey: Rotation Periods and Phase Functions from Sparse Photometry". The Astronomical Journal 150 (3): 35. doi:10.1088/0004-6256/150/3/75. Bibcode: 2015AJ....150...75W. 
  8. ↑ Veres, Peter; Jedicke, Robert; Fitzsimmons, Alan; Denneau, Larry; Granvik, Mikael; Bolin, Bryce et al. (November 2015). "Absolute magnitudes and slope parameters for 250,000 asteroids observed by Pan-STARRS PS1 - Preliminary results". Icarus 261: 34–47. doi:10.1016/j.icarus.2015.08.007. Bibcode: 2015Icar..261...34V. 
  9. ↑ 9.0 9.1 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. 
  10. ↑ 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. 
  11. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. https://www.minorplanetcenter.net/iau/ECS/MPCArchive/MPCArchive_TBL.html. Retrieved 28 March 2018. 

External links



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