10476 Los Molinos

Last updated
10476 Los Molinos
Discovery [1]
Discovered by S. J. Bus
Discovery site Siding Spring Obs.
Discovery date2 March 1981
Designations
(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
Dimensions2.853±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]

    Contents

    Orbit and classification

    Los Molinos is a non-family asteroid from the main belt's background population. [4] 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

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

    Rotation period

    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

    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

    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]

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    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 10476 Los Molinos (1981 EY38)" (2017-10-30 last obs.). Jet Propulsion Laboratory . Retrieved 20 February 2018.
    2. 1 2 3 4 "10476 Los Molinos (1981 EY38)". Minor Planet Center. Retrieved 20 February 2018.
    3. 1 2 3 4 5 6 7 8 "LCDB Data for (10476) Los Molinos". Asteroid Lightcurve Database (LCDB). Retrieved 20 February 2018.
    4. 1 2 "Asteroid 10476 Los Molinos – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 29 October 2019.
    5. 1 2 3 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. arXiv: 1109.4096 . Bibcode:2011ApJ...741...68M. doi:10.1088/0004-637X/741/2/68.
    6. 1 2 3 4 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. arXiv: 1109.6407 . Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90.
    7. 1 2 3 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. arXiv: 1504.04041 . Bibcode:2015AJ....150...75W. doi:10.1088/0004-6256/150/3/75.
    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: 1506.00762 . Bibcode:2015Icar..261...34V. doi:10.1016/j.icarus.2015.08.007.
    9. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 20 February 2018.
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