10476 Los Molinos

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10476 Los Molinos
Discovery [1]
Discovered by S. J. Bus
Discovery site Siding Spring Obs.
Discovery date 2 March 1981
Designations
MPC designation (10476) Los Molinos
Named after
Los Molinos Observatory[2]
(Uruguayan observatory)
1981 EY38 · 1978 NB3
main-belt · (inner)[3]
background [4]
Orbital characteristics[1]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc 39.31 yr (14,358 days)
Aphelion 2.9165 AU
Perihelion 1.7185 AU
2.3175 AU
Eccentricity 0.2585
3.53 yr (1,289 days)
95.559°
0° 16m 45.84s / day
Inclination 9.4472°
249.86°
38.678°
Physical characteristics
Dimensions 2.853±0.014 km[5][6]
2.96 km (calculated)[3]
267.906±1.9703 h[7]
0.20 (assumed)[3]
0.3424±0.0425[5][6]
S[3]
14.4[6] · 14.556±0.003 (R)[7] · 14.6[1] · 15.01[3] · 15.33±0.50[8]

10476 Los Molinos, provisional designation 1981 EY38, is a stony background asteroid and slow rotator from the inner regions of the asteroid belt, approximately 2.9 kilometers (1.8 miles) in diameter. It was discovered on 2 March 1981, by American astronomer Schelte Bus at the Siding Spring Observatory in Australia. The asteroid was named for the Los Molinos Observatory in Uruguay.[2]

Orbit and classification[edit]

Los Molinos is a non-family asteroid from the main belt's background population. It orbits the Sun in the inner asteroid belt at a distance of 1.7–2.9 AU once every 3 years and 6 months (1,289 days; semi-major axis of 2.32 AU). Its orbit has an eccentricity of 0.26 and an inclination of 9° with respect to the ecliptic.[1] The body's observation arc begins with its first observations as 1978 NB3 at Crimea–Nauchnij in July 1978.[2]

Physical characteristics[edit]

Based on its high albedo and its location within the asteroid belt, Los Molinos is an assumed S-type asteroid.[3]

Rotation period[edit]

In August 2010, a rotational lightcurve of Los Molinos was obtained from photometric observations in the R-band by astronomers at the Palomar Transient Factory in California. Lightcurve analysis gave a rotation period of 267.906±1.9703 hours with a brightness amplitude of 0.33 magnitude (U=2).[7] This makes Los Molinos one of the top 200 slow rotators known to exist.[3]

Diameter and albedo[edit]

According to the survey carried out by the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Los Molinos measures 2.853 kilometers in diameter and its surface has a high albedo of 0.34.[5][6]

The Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 2.96 kilometers based on an absolute magnitude of 15.01.[3]

Naming[edit]

This minor planet was named after the Los Molinos Observatory (844) located near Montevideo in Uruguay. The observatory is known for its astrometric follow-up observations of asteroids and comets.[2] The official naming citation was published by the Minor Planet Center on 13 April 2017 (M.P.C. 103975/103976).[9]

References[edit]

  1. ^ a b c d "JPL Small-Body Database Browser: 10476 Los Molinos (1981 EY38)" (2017-10-30 last obs.). Jet Propulsion Laboratory. Retrieved 20 February 2018. 
  2. ^ a b c d "10476 Los Molinos (1981 EY38)". Minor Planet Center. Retrieved 20 February 2018. 
  3. ^ a b c d e f g h "LCDB Data for (10476) Los Molinos". Asteroid Lightcurve Database (LCDB). Retrieved 20 February 2018. 
  4. ^ "Small Bodies Data Ferret". Nesvorny HCM Asteroid Families V3.0. Retrieved 20 February 2018. 
  5. ^ a b c 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" (PDF). The Astrophysical Journal. 741 (2): 20. arXiv:1109.4096Freely accessible. Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68. Retrieved 20 February 2018. 
  6. ^ a b c d Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results" (PDF). The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407Freely accessible. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. Retrieved 20 February 2018. 
  7. ^ a b c 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" (PDF). The Astronomical Journal. 150 (3): 35. arXiv:1504.04041Freely accessible. Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75. Retrieved 20 February 2018. 
  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. arXiv:1506.00762Freely accessible. Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007. Retrieved 20 February 2018. 
  9. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 20 February 2018. 

External links[edit]