(5407) 1992 AX

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(5407) 1992 AX
Orbit of 1992 AX.gif
Orbital diagram of 1992 AX
Discovery [1]
Discovered by S. Ueda
H. Kaneda
Discovery site Kushiro Obs.
Discovery date4 January 1992
Designations
(5407) 1992 AX
1992 AX ·1987 BH2
Mars crosser [1] [2] [3]
binary [4] [5]
Orbital characteristics [2]
Epoch 27 April 2019 (JD 2458600.5)
Uncertainty parameter 0
Observation arc 66.90 yr (24,434 d)
Aphelion 2.3486 AU
Perihelion 1.3279 AU
1.8383 AU
Eccentricity 0.2776
2.49 yr (910 d)
263.87°
0° 23m 43.8s / day
Inclination 11.390°
117.74°
108.78°
Known satellites 1 (D: 780 m; P: 13.52 h) [4] [5]
Earth  MOID 0.377 AU (147 LD)
Physical characteristics
Mean diameter
2.78±0.55  km [6]
3.60±0.36 km [7]
3.8±0.4 km [8]
4.18±0.12 km [9]
2.5488  h [10] [11]
0.199 [8]
0.294 [9]
0.376 [7]
0.40 [6]
SMASS = S k [2]  · S [12]
B–V = 0.690 [10]
V–R = 0.500 [10]
V–I = 0.840 [10]
13.90 [7] [9]
14.0 [1] [2]
14.47 [8] [10]

    (5407) 1992 AX, provisional designation 1992 AX, is a stony asteroid and a synchronous binary Mars-crosser from the innermost region of the asteroid belt, approximately 3.6 kilometers (2.2 miles) in diameter. It was discovered on 4 January 1992, by Japanese astronomers Seiji Ueda and Hiroshi Kaneda at the Kushiro Observatory on Hokkaidō, Japan. [1] The S-type asteroid has a short rotation period of 2.5 hours. [4] Its sub-kilometer satellite was discovered in 1997. [5] As of 2018, the binary system has not been named. [1]

    Contents

    Orbit and classification

    1992 AX a member of the Mars-crossing asteroids, a dynamically unstable group between the main belt and the near-Earth populations, crossing the orbit of Mars at 1.66  AU. [1] [3] It orbits the Sun at a distance of 1.3–2.3  AU once every 2 years and 6 months (910 days; semi-major axis of 1.84 AU). Its orbit has an eccentricity of 0.28 and an inclination of 11° with respect to the ecliptic. [2]

    The asteroid makes occasional close approaches to Mars. Its next close approach, on 22 January 2027, will bring it 11,260,000 km (0.0753 AU) from Mars. [2] The body's observation arc begins with a precovery taken at Palomar Observatory in November 1951, or more than 40 years prior to its official discovery observation at Kushiro. [1]

    Naming

    This minor planet was numbered by the Minor Planet Center on 9 December 1992 ( M.P.C. 21249). [13] As of 2018, it has not been named. [1]

    Physical characteristics

    1992 AX has been characterized as a common, stony S-type asteroid. [12] In the SMASS taxonomy, it is an Sk-subtype, that transitions between the S and K-type asteroids. [2] The body's color indices of 0.690 (B–V), 0.500 (V–R) and 0.840 (V–I) were also determined. [10]

    Lightcurves

    Rotation period

    Since 1997, several rotational lightcurves of 1992 AX have been obtained from photometric observations by Petr Pravec and collaborating astronomers. Best-rated lightcurve analysis gave a rotation period of 2.5488 hours with a consolidated brightness amplitude between 0.10 and 0.12 magnitude ( U=2/3 ). [4] [10] [11] The results supersedes a tentative period determination of 3.6 hours by Marc Buie ( U=1 ). [4]

    Satellite

    During the observations in January 1997, it was also revealed that 1992 AX is a synchronous binary asteroid with a minor-planet moon in its orbit. [10] The satellite measures approximately 780 meters in diameter, or about 20% of its primary, and has an orbital period of 13.52 hours with an estimated semi-major axis of 5.8 kilometers for its very circular orbit. [5] Observations by Pravec in January and February 2012 confirmed the binary nature of this asteroid, as well as its rotational and orbital periods. [4] The satellite's provisional designation is S/1997 (5407) 1.

    Diameter and albedo

    According to the surveys carried out by the Japanese Akari satellite, the Spitzer Space Telescope and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer (WISE), 1992 AX measures between 2.78 and 4.18 kilometers in diameter and its surface has an albedo between 0.199 and 0.40. [6] [8] [9]

    In 2017, a study by WISE dedicated to Mars-crossing asteroids determined a diameter of 3.60 kilometers with a high albedo of 0.376. [7] The Collaborative Asteroid Lightcurve Link assumes an albedo of 0.20 and derives a diameter of 3.79 kilometers based on an absolute magnitude of 14.47. [4] The Johnston's archive gives an effective (combined) diameter of 3.98 kilometers with 3.9 and 0.78 kilometers for is primary and secondary body, respectively. [3] [5]

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    References

    1. 1 2 3 4 5 6 7 8 "5407 (1992 AX)". Minor Planet Center. Retrieved 19 November 2018.
    2. 1 2 3 4 5 6 7 "JPL Small-Body Database Browser: 5407 (1992 AX)" (2018-10-21 last obs.). Jet Propulsion Laboratory . Retrieved 19 November 2018.
    3. 1 2 3 "Asteroid (5407) 1992 AX". Small Bodies Data Ferret. Retrieved 19 November 2018.
    4. 1 2 3 4 5 6 7 "LCDB Data for (5407)". Asteroid Lightcurve Database (LCDB). Retrieved 19 November 2018.
    5. 1 2 3 4 5 Johnston, Wm. Robert (18 February 2017). "Asteroids with Satellites Database – (450894) 2008 BT18". Johnston's Archive. Retrieved 19 November 2018.
    6. 1 2 3 Nugent, C. R.; Mainzer, A.; Bauer, J.; Cutri, R. M.; Kramer, E. A.; Grav, T.; et al. (September 2016). "NEOWISE Reactivation Mission Year Two: Asteroid Diameters and Albedos". The Astronomical Journal. 152 (3): 12. arXiv: 1606.08923 . Bibcode:2016AJ....152...63N. doi: 10.3847/0004-6256/152/3/63 . S2CID   119289027.
    7. 1 2 3 4 Alí-Lagoa, V.; Delbo', M. (July 2017). "Sizes and albedos of Mars-crossing asteroids from WISE/NEOWISE data". Astronomy and Astrophysics. 603: 8. arXiv: 1705.10263 . Bibcode:2017A&A...603A..55A. doi:10.1051/0004-6361/201629917. S2CID   119224590.
    8. 1 2 3 4 Marchis, F.; Enriquez, J. E.; Emery, J. P.; Mueller, M.; Baek, M.; Pollock, J.; et al. (November 2012). "Multiple asteroid systems: Dimensions and thermal properties from Spitzer Space Telescope and ground-based observations". Icarus. 221 (2): 1130–1161. arXiv: 1604.05384 . Bibcode:2012Icar..221.1130M. doi:10.1016/j.icarus.2012.09.013. S2CID   161887.
    9. 1 2 3 4 Usui, Fumihiko; Kuroda, Daisuke; Müller, Thomas G.; Hasegawa, Sunao; Ishiguro, Masateru; Ootsubo, Takafumi; et al. (October 2011). "Asteroid Catalog Using Akari: AKARI/IRC Mid-Infrared Asteroid Survey". Publications of the Astronomical Society of Japan. 63 (5): 1117–1138. Bibcode:2011PASJ...63.1117U. doi: 10.1093/pasj/63.5.1117 . (online, AcuA catalog p. 153)
    10. 1 2 3 4 5 6 7 8 Pravec, Petr; Sarounová, Lenka; Rabinowitz, David L.; Hicks, Michael D.; Wolf, Marek; Krugly, Yurij N.; et al. (July 2000). "Two-Period Lightcurves of 1996 FG 3, 1998 PG, and (5407) 1992 AX: One Probable and Two Possible Binary Asteroids". Icarus. 146 (1): 190–203. Bibcode:2000Icar..146..190P. doi:10.1006/icar.2000.6375.
    11. 1 2 Pravec, P.; Scheirich, P.; Kusnirák, P.; Sarounová, L.; Mottola, S.; Hahn, G.; et al. (March 2006). "Photometric survey of binary near-Earth asteroids". Icarus. 181 (1): 63–93. Bibcode:2006Icar..181...63P. doi:10.1016/j.icarus.2005.10.014.
    12. 1 2 Sanchez, Juan A.; Michelsen, René; Reddy, Vishnu; Nathues, Andreas (July 2013). "Surface composition and taxonomic classification of a group of near-Earth and Mars-crossing asteroids". Icarus. 225 (1): 131–140. arXiv: 1302.4449 . Bibcode:2013Icar..225..131S. doi:10.1016/j.icarus.2013.02.036. S2CID   119207812.
    13. ↑ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 19 November 2018.
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