(5836) 1993 MF
Discovery[1]
Discovered byE. F. Helin
K. J. Lawrence
Discovery sitePalomar Obs.
Discovery date22 June 1993
Designations
(5836) 1993 MF
1993 MF
Amor · NEO[1][2]
Orbital characteristics[1]
Epoch 4 September 2017 (JD 2458000.5)
Uncertainty parameter 0
Observation arc35.90 yr (13,112 days)
Aphelion3.7489 AU
Perihelion1.1311 AU
2.4400 AU
Eccentricity0.5364
3.81 yr (1,392 days)
107.39°
0° 15m 30.96s / day
Inclination7.9497°
238.78°
77.974°
Earth MOID0.1842 AU · 71.8 LD
Physical characteristics
Dimensions2.79 km (derived)[3]
3.8 km[4]
4.948±0.005 h[lower-alpha 1]
4.9543±0.0002 h[lower-alpha 2]
4.959 h[4]
4.96±0.01 h[5]
0.20 (assumed)[3]
SMASS = S[1] · S[3]
14.65±0.2 (R)[lower-alpha 2] · 14.7[1] · 15.01±0.16[5] · 15.03±0.05[4] · 15.141±0.139[3][6] · 15.43±0.40[7]

    (5836) 1993 MF is a highly eccentric, stony asteroid, classified as a near-Earth object of the Amor group of asteroids, approximately 3 kilometers in diameter. It was discovered on 22 June 1993, by American astronomers Eleanor Helin and Kenneth Lawrence at the U.S. Palomar Observatory in California.[2]

    Classification and orbit

    The stony S-type asteroid orbits the Sun at a distance of 1.1–3.7 AU once every 3 years and 10 months (1,392 days). Its orbit has an eccentricity of 0.54 and an inclination of 8° with respect to the ecliptic.[1] It has an Earth minimum orbital intersection distance of nearly 0.184 AU (27,500,000 km), which corresponds to 71.8 lunar distances. As it crosses the orbit of Mars, it may also be classified as a Mars-crosser, and, on 28 November 2023, it will pass 0.02535 AU (3,792,000 km) from the Red Planet.[1] The first precovery was taken at the Australian Siding Spring Observatory in 1981, extending the body's observation arc by 12 years prior to its discovery.[2]

    Physical characteristics

    Since the 1990s, and up to June 2016, four well-defined rotational lightcurves were obtained for this asteroid from photometric observations, giving a rotation period of approximately 4.95 hours with a high brightness variation between 0.53 and 0.82 in magnitude, indicating that the asteroid has a non-spheroidal shape. In the 1990s, Italian astronomer Stefano Mottola obtained a lightcurve at La Silla during the EUNEASO, a European near-Earth object search and follow-up observation program to determine additional physical parameters (U=3).[4]

    Further lightcurves were obtained by Polish astronomer Wiesław Z. Wiśniewski at UA's LPL in October 1993, and by Czech astronomer Petr Pravec at Ondřejov Observatory in September 1997 (U=3/3).[5][lower-alpha 2] In June 2016, the fourth and most recent photometric observation was made by American astronomer Brian Warner at his Palmer Divide Station, Colorado, which gave a period of 4.948±0.005 hours with an amplitude of 0.82 in magnitude (U=3).[lower-alpha 1]

    Diameter

    While in the 1990s, Stefano Mottola estimated the asteroid to measure 3.8 kilometers in diameter (H = 15.03),[4] the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and derives a shorter diameter of 2.8 kilometers, based on an absolute magnitude of 15.14.[3]

    Notes

    1. 1 2 Warner (2016) web: observation date: 2016-06-07. Rotation period of 4.948±0.005 hours with a brightness amplitude of 0.82 mag (U=3). Summary figures at Collaborative Asteroid Lightcurve Link (CALL) for (5836)
    2. 1 2 3 Pravec (1997) web: observation date: 1997-11-04. Rotation period of 4.948±0.005 hours with a brightness amplitude of 0.74 mag and an absolute magnitude of 14.65 in the R-band (U=3). Summary figures at Collaborative Asteroid Lightcurve Link (CALL) for (5836) and Pravec, P.; Wolf, M.; Sarounova, L. (1997)

    References

    1. 1 2 3 4 5 6 7 "JPL Small-Body Database Browser: 5836 (1993 MF)" (2017-03-20 last obs.). Jet Propulsion Laboratory. Archived from the original on 11 December 2019. Retrieved 26 May 2017.
    2. 1 2 3 "5836 (1993 MF)". Minor Planet Center. Retrieved 30 August 2016.
    3. 1 2 3 4 5 "LCDB Data for (5836)". Asteroid Lightcurve Database (LCDB). Retrieved 30 August 2016.
    4. 1 2 3 4 5 Mottola, S.; de Angelis, G.; di Martino, M.; Erikson, A.; Harris, A. W.; Hahn, G.; et al. (March 1995). "The EUNEASO Photometric Follow-up Program". Abstracts of the Lunar and Planetary Science Conference. 26: 1003. Bibcode:1995LPI....26.1003M. Retrieved 30 August 2016.
    5. 1 2 3 Wisniewski, W. Z.; Michalowski, T. M.; Harris, A. W.; McMillan, R. S. (March 1995). "Photoelectric Observations of 125 Asteroids". Abstracts of the Lunar and Planetary Science Conference. 26: 1511. Bibcode:1995LPI....26.1511W. Retrieved 30 August 2016.
    6. ↑ Pravec, Petr; Harris, Alan W.; Kusnirák, Peter; Galád, Adrián; Hornoch, Kamil (September 2012). "Absolute magnitudes of asteroids and a revision of asteroid albedo estimates from WISE thermal observations". Icarus. 221 (1): 365–387. Bibcode:2012Icar..221..365P. doi:10.1016/j.icarus.2012.07.026. Retrieved 30 August 2016.
    7. ↑ 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. S2CID 53493339. Retrieved 30 August 2016.
    This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.