(5407) 1992 AX

(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]

(5407) 1992 AX
Orbital diagram of 1992 AX
Discovery [1]
Discovered byS. Ueda
H. Kaneda
Discovery siteKushiro 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 arc66.90 yr (24,434 d)
Aphelion2.3486 AU
Perihelion1.3279 AU
1.8383 AU
Eccentricity0.2776
2.49 yr (910 d)
263.87°
0° 23m 43.8s / day
Inclination11.390°
117.74°
108.78°
Known satellites1 (D: 780 m; P: 13.52 h)[4][5]
Earth MOID0.377 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 = Sk [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]

    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]

    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]

    References
    1. "5407 (1992 AX)". Minor Planet Center. Retrieved 19 November 2018.
    2. "JPL Small-Body Database Browser: 5407 (1992 AX)" (2018-10-21 last obs.). Jet Propulsion Laboratory. Retrieved 19 November 2018.
    3. "Asteroid (5407) 1992 AX". Small Bodies Data Ferret. Retrieved 19 November 2018.
    4. "LCDB Data for (5407)". Asteroid Lightcurve Database (LCDB). Retrieved 19 November 2018.
    5. Johnston, Wm. Robert (18 February 2017). "Asteroids with Satellites Database – (450894) 2008 BT18". Johnston's Archive. Retrieved 19 November 2018.
    6. 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.
    7. 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.
    8. 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.
    9. 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. Retrieved 19 November 2018. (online, AcuA catalog p. 153)
    10. 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. 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. 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.
    13. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 19 November 2018.

    This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.