Colonel William A. Phillips

1139 Atami, provisional designation 1929 XE, is a stony asteroid and sizable Mars-crosser, as well as a synchronous binary system[5] near the innermost region of the asteroid belt, approximately 9 kilometers in diameter. It was discovered on 1 December 1929, by Japanese astronomers Okuro Oikawa and Kazuo Kubokawa at the Tokyo Astronomical Observatory (389) near Tokyo.[3] It was named after the Japanese city of Atami.[2] It has the lowest Minimum orbit intersection distance (MOID) to Mars of any asteroid as large as it, its orbit intersecting only 0.03 astronomical units from the planet.

Classification and orbit

Atami is a Mars-crossing asteroid, a dynamically unstable group between the main belt and the near-Earth populations, crossing the orbit of Mars at 1.666 AU. It orbits the Sun at a distance of 1.5–2.4 AU once every 2 years and 9 months (993 days). Its orbit has an eccentricity of 0.26 and an inclination of 13° with respect to the ecliptic.[1] The body's observation arc begins with its official discovery observation at Tokyo in 1929.[3]

Physical characteristics

Spectral type

Atami is a common stony S-type asteroid in both the Tholen and SMASS classification.[1] It has also been characterized as a S-type by Pan-STARRS photometric survey.[11]

Binary system

In 2005, two rotational lightcurves obtained at the U.S. Antelope Hills Observatory in New Mexico and by a collaboration of several European astronomers gave a rotation period of 27.56±0.01 and 27.446±0.001 hours with a brightness variation of 0.45 and 0.40 in magnitude, respectively (U=3/3).[9][10][a]

Photometric and Arecibo echo spectra observations in 2005 confirmed a 5 kilometer satellite orbiting at least 15 kilometers from its primary.[5] Due to the similar size of the primary and secondary the Minor Planet Center lists this as a binary companion.[12]

Diameter and albedo

According to the survey carried out by NASA's Wide-field Infrared Survey Explorer and its subsequent NEOWISE mission, Atami measures 8.24 kilometers in diameter and its surface has an albedo of 0.258,[6] while the Collaborative Asteroid Lightcurve Link assumes a standard albedo for stony asteroids of 0.20 and calculates a diameter of 9.35 kilometers based on an absolute magnitude of 12.51.[4]

This makes Atami one of the largest mid-sized Mars-crossing asteroids comparable with 1065 Amundsenia (9.75 km), 1474 Beira (8.73 km), 1011 Laodamia (7.5 km), 1727 Mette (est. 9 km), 1131 Porzia (7.13 km), 1235 Schorria (est. 9 km), 985 Rosina (8.18 km), 1310 Villigera (15.24 km) and 1468 Zomba (7 km), but far smaller than the largest members of this dynamical group, namely, 132 Aethra, 323 Brucia, 1508 Kemi, 2204 Lyyli and 512 Taurinensis, which are all larger than 20 kilometers in diameter.

Naming

The minor planet was named after Atami, a Japanese city and harbor near Tokyo, Japan.[2] The naming citation was first mentioned in The Names of the Minor Planets by Paul Herget in 1955 (H 106).[2]

Notes

  1. ^ a b Lightcurve plot of (1139) Atami, Robert Koff, Antelope Hills Observatory (H09). Summary figures at LCDB

References

  1. ^ a b c d e f g h i j "JPL Small-Body Database Browser: 1139 Atami (1929 XE)" (2017-06-02 last obs.). Jet Propulsion Laboratory. Retrieved 20 October 2017.
  2. ^ a b c d Schmadel, Lutz D. (2007). "(1139) Atami". Dictionary of Minor Planet Names – (1139) Atami. Springer Berlin Heidelberg. p. 96. doi:10.1007/978-3-540-29925-7_1140. ISBN 978-3-540-00238-3.
  3. ^ a b c "1139 Atami (1929 XE)". Minor Planet Center. Retrieved 20 October 2017.
  4. ^ a b c d e f "LCDB Data for (1139) Atami". Asteroid Lightcurve Database (LCDB). Retrieved 7 February 2017.
  5. ^ a b c "Electronic Telegram No. 430". IAU Central Bureau for Astronomical Telegrams. 14 March 2006. Retrieved 7 February 2017.
  6. ^ a b c d Alí-Lagoa, V.; Delbo', M. (July 2017). "Sizes and albedos of Mars-crossing asteroids from WISE/NEOWISE data" (PDF). Astronomy and Astrophysics. 603: 8. arXiv:1705.10263. Bibcode:2017A&A...603A..55A. doi:10.1051/0004-6361/201629917. Retrieved 20 October 2017.
  7. ^ a b 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 22 August 2016.
  8. ^ Lupishko, D. F.; Velichko, F. P.; Shevchenko, V. G. (June 1988). "Photometry of the AMOR type asteroids 1036 Ganymede and 1139 Atami". Astronomicheskii Vestnik. 22: 167–173.InRussian. Bibcode:1988AVest..22..167L. ISSN 0320-930X. Retrieved 22 August 2016.
  9. ^ a b c d e f g Behrend, Raoul. "Asteroids and comets rotation curves – (1139) Atami". Geneva Observatory. Retrieved 7 February 2017.
  10. ^ a b Koff, Robert A. (June 2006). "Lightcurves of asteroids 141 Lumen, 259 Alatheia, 363 Padua, 455 Bruchsalia 514 Armida, 524 Fidelio, and 1139 Atami". The Minor Planet Bulletin. 33 (2): 31–33. Bibcode:2006MPBu...33...31K. ISSN 1052-8091. Retrieved 22 August 2016.
  11. ^ a b c 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. Retrieved 22 August 2016.
  12. ^ "Satellites and Companions of Minor Planets". IAU Central Bureau for Astronomical Telegrams. 17 September 2009. Retrieved 7 February 2017.

External links

source: https://en.wikipedia.org/wiki/1139_Atami