1727 Mette

1727 Mette
Discovery [1]
Discovered by A. D. Andrews
Discovery site Boyden Observatory
Discovery date 25 January 1965
Designations
MPC designation 1727 Mette
Named after
 Mette Andrews
(wife of discoverer) [2]
1965 BA · 1955 DC
Mars-crosser · Hungarian [3]
Orbital characteristics [1]
Epoch 13 January 2016 (JD 2457400.5)
Uncertainty parameter 0
Observation arc 61.06 yr (22303 days)
Aphelion 2.0431 AU (305.64 Gm)
Perihelion 1.6652 AU (249.11 Gm)
1.8542 AU (277.38 Gm)
Eccentricity 0.10190
2.52 yr (922.20 d)
88.442°
0° 23m 25.332s / day
Inclination 22.896°
133.04°
313.09°
Known satellites 1 (see 2nd infobox)[lower-alpha 1]
Earth MOID 0.716685 AU (107.2145 Gm)
Jupiter MOID 3.09933 AU (463.653 Gm)
Jupiter Tisserand parameter 3.900
Physical characteristics
Dimensions 9.40 km (calculated) [3]
2.98109 h (0.124212 d) [1][4][5]
2.63 h [6]
2.637 h [7]
3.22 h [8]
2.981±0.001 h [9]
2.427 h [lower-alpha 2]
2.98125±0.00004 h [9]
2.981±0.001 h [10]
2.981±0.003 h [11]
2.9814±0.0001 h [9]
2.9808±0.0002 h [12]
0.20 (assumed) [3]
Tholen = S
S [3]
12.6

    1727 Mette, provisional designation 1965 BA, is a stony, binary asteroid[lower-alpha 1] and Mars-crosser from the inner regions of the asteroid belt, about 9 kilometers in diameter. It was discovered by English astronomer David Andrews at Boyden Observatory near Bloemfontein in Free State, South Africa on 25 January 1965.[13]

    The S-type asteroid is a member of the Hungaria family, which form the innermost dense concentration of asteroids in the Solar System. It orbits the Sun at a distance of 1.7–2.0 AU once every two and a half years (922 days). Its orbit shows an eccentricity of 0.10 and is significantly tilted by 23 degrees to the plane of the ecliptic. It has been observed numerous times with light-curve analysis indicating a moderately elongated body and rendering a rotation period of close to 3 hours.[9][12] The body has an assumed geometric albedo of 0.20, typical for stony asteroids.[3] Being a Mars-crosser, it will make a relatively close approach to Mars on April 15, 2023, when it will pass near the Red Planet at a distance of less than 0.08 AU, or 12 million kilometers.[1]

    In 2013, a satellite orbiting the asteroid was discovered. The moon measures about 2 kilometers in diameter and orbits Mette once every 20 hours and 59 minutes.[4][5][14] There are several hundreds of asteroids known to have satellites (also see Category:Binary asteroids).[15]

    The minor planet was named by the discoverer after his wife, Mette Andrews for her comprehension of his nocturnal working hours and absence from home.[2]

    S/2013 (1727) 1
    Discovery
    Discovery date 17 January 2013 [lower-alpha 1]
    Light-curve
    Orbital characteristics
    21 km
    0.8746±0.0008 days
    (20 hours, 59±1 minutes)
    31 mas (maximum)
    Satellite of 1727 Mette
    Physical characteristics
    Dimensions 2.14 km [14]
    3.4 ± 0.2 fainter than primary[14]
    15.7

      References

      1. 1 2 3 Central Bureau for Astronomical Telegrams (No.3402), 5 February 2013 for (1727) METTE: "CCD photometric observations made between Jan. 17 and 21 show that minor planet (1727) Mette is a binary system with an orbital period of 21.05 +/- 0.03 hr. The light-curve of the primary has a period of 2.98091 +/- 0.00009 hr with an amplitude of 0.33 +/- 0.01 mag, indicating a moderately elongated body. Assuming a triaxial ellipsoidal shape and equatorial view, this gives an a/b ratio of 1.36 +/- 0.02. This makes the object unusual in that the primaries of most small binary systems are nearly spheroidal. The depth of the events ranges from 0.04 to 0.07 mag. The depth of the secondary event gives a lower limit for the effective secondary-to-primary diameter ratio of Ds/Dp = 0.20 +/- 0.02. A general "bowing" of the secondary period light curve (amplitude 0.01–0.02 mag) indicates that the satellite is probably tidally-locked to the orbital period." — Reported by B. D. Warner, Palmer Divide Observatory, Colorado Springs, CO, USA; R. D. Stephens, Center for Solar System Studies, Landers, CA, USA; and A. W. Harris, MoreData!, La Canada, CA, USA.
      2. ↑ Monson (2011) web: rotation period 2.427 hours with a brightness amplitude of 0.29. Summary figures at Asteroid Lightcurve Database for (1727) Mette
      1. 1 2 3 4 "JPL Small-Body Database Browser: 1727 Mette (1965 BA)" (2015-01-14 last obs.). Jet Propulsion Laboratory. Retrieved 21 April 2016.
      2. 1 2 Schmadel, Lutz D. (2003). Dictionary of Minor Planet Names – (1727) Mette. Springer Berlin Heidelberg. p. 137. ISBN 978-3-540-29925-7. Retrieved 16 November 2015.
      3. 1 2 3 4 5 "LCDB Data for (1727) Mette". Asteroid Lightcurve Database (LCDB). Retrieved 16 November 2015.
      4. 1 2 Warner, B. D.; Stephens, R. D.; Harris, A. W. (February 2013). "(1727) Mette". Central Bureau Electronic Telegrams. Bibcode:2013CBET.3402....1W. Retrieved 16 November 2015.
      5. 1 2 Warner, Brian D.; Stephens, Robert D. (July 2013). "1727 Mette: A New Hungaria Binary". The Minor Planet Bulletin. 40 (3): 129–130. Bibcode:2013MPBu...40..129W. ISSN 1052-8091. Retrieved 16 November 2015.
      6. ↑ Wisniewski, W. Z.; McMillan, R. S. (May 1987). "Differential CCD photometry of faint asteroids in crowded star fields and nonphotometric sky conditions". Astronomical Journal: 1264–1267. Bibcode:1987AJ.....93.1264W. doi:10.1086/114408. ISSN 0004-6256. Retrieved 16 November 2015.
      7. ↑ Prokof'eva, V. V.; Demchik, M. I.; Golub', A. I. (December 1991). "TV photometry of asteroids: brightness curve of asteroid 1727 Mette.". Solar System Research. 26 (4): 373–375. Bibcode:1992SoSyR..26..373P. Retrieved 16 November 2015.
      8. ↑ Sárneczky, K.; Szabó, Gy.; Kiss, L. L. (June 1999). "CCD observations of 11 faint asteroids". Astronomy and Astrophysics Supplement: 363–368. Bibcode:1999A&AS..137..363S. doi:10.1051/aas:1999251. Retrieved 16 November 2015.
      9. 1 2 3 4 Behrend, Raoul. "Asteroids and comets rotation curves – (1727) Mette". Geneva Observatory. Retrieved 16 November 2015.
      10. ↑ Gandolfi, D.; Cigna, M.; Fulvio, D.; Blanco, C. (January 2009). "CCD and photon-counting photometric observations of asteroids carried out at Padova and Catania observatories". Planetary and Space Science. 57 (1): 1–9. arXiv:0810.1560Freely accessible. Bibcode:2009P&SS...57....1G. doi:10.1016/j.pss.2008.09.014. Retrieved 16 November 2015.
      11. ↑ Warner, Brian D. (October 2011). "Asteroid Lightcurve Analysis at the Palmer Divide Observatory: 2011 March - July". The Minor Planet Bulletin. 38 (4): 190–195. Bibcode:2011MPBu...38..190W. ISSN 1052-8091. Retrieved 16 November 2015.
      12. 1 2 Warner, Brian D.; Stephens, Robert D.; Harris, Alan W. (January 2015). "A Trio of Binary Asteroids". The Minor Planet Bulletin. 42 (1): 31–34. Bibcode:2015MPBu...42...31W. ISSN 1052-8091. Retrieved 16 November 2015.
      13. ↑ "1727 Mette (1965 BA)". Minor Planet Center. Retrieved 16 November 2015.
      14. 1 2 3 Johnston, Robert. "(1727) Mette". johnstonsarchive.net. Retrieved 28 May 2015.
      15. ↑ Wm. Robert Johnston (1 November 2015). "Asteroids with Satellites". Johnston's Archive. Retrieved 16 November 2015.

      External links

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