Jump to content

5905 Johnson

From Wikipedia, the free encyclopedia

This is an old revision of this page, as edited by Tom.Reding (talk | contribs) at 14:52, 25 December 2023 (+{{Authority control}} (2 IDs from Wikidata); WP:GenFixes & cleanup on). The present address (URL) is a permanent link to this revision, which may differ significantly from the current revision.

5905 Johnson
Discovery [1]
Discovered byE. F. Helin
Discovery sitePalomar Obs.
Discovery date11 February 1989
Designations
(5905) Johnson
Named after
Lindley N. Johnson
(astronomer, engineer)[2]
1989 CJ1
main-belt · (inner) [1]
Hungaria [3][4] · background [5]
Orbital characteristics [1]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc28.96 yr (10,576 days)
Aphelion2.0476 AU
Perihelion1.7727 AU
1.9102 AU
Eccentricity0.0720
2.64 yr (964 days)
174.14°
0° 22m 23.88s / day
Inclination27.521°
141.28°
208.81°
Known satellites1 (P: 21.78 h; 0.4 Ds/Dp)[6][a]
Physical characteristics
3.62±0.67 km[7]
3.85±0.66 km[8]
4.1±0.5 km[9]
4.728±0.064 km[10]
4.791±0.065 km[11]
4.797 km[12]
4.80 km (taken)[4]
3.78142±0.0002 h[b]
3.78222±0.0001 h[13]
3.7823±0.0002 h[14]
3.7824±0.0001 h[6]
3.7827±0.0002 h[15][c]
0.1524[12]
0.1939±0.0278[11]
0.198±0.022[10]
0.25±0.10[8]
0.266±0.100[9]
0.44±0.17[7]
S (assumed)[4]
13.6±0.3 (R)[13] · 14.0[1][7][11][15] · 14.00±0.1[9] · 14.15±0.92[16] · 14.21[8] · 14.255±0.13[4][12]

5905 Johnson, provisional designation 1989 CJ1, is a Hungaria asteroid and synchronous binary system[a] from the innermost regions of the asteroid belt, approximately 4 kilometers (2.5 miles) in diameter. It was discovered on 11 February 1989, by American astronomer Eleanor Helin at Palomar Observatory in California, United States.[3] Its satellite measures approximately 1.6 km (1 mi) in diameter and orbits its primary every 21.8 hours.[6] It was named after American astronomer and engineer Lindley N. Johnson.[2]

Classification and orbit

Johnson is a stony S-type asteroid and member of the dynamical Hungaria group, which forms the innermost dense concentration of asteroids in the Solar System.[3][4] It is, however, not a member of collisional Hungaria family, but a non-family asteroid of the main belt's background population when applying the hierarchical clustering method to its proper orbital elements.[5]

It orbits the Sun in the inner asteroid belt at a distance of 1.8–2.0 AU once every 2 years and 8 months (964 days; semi-major axis of 1.91 AU). Its orbit has an eccentricity of 0.07 and an inclination of 28° with respect to the ecliptic.[1] As no precoveries were taken, and no prior identifications were made, the body's observation arc begins at Palomar with its official discovery observation in February 1989.[3]

Diameter and albedo

According to the surveys carried out by NASA's space-based Spitzer and WISE telescopes, and the NEOWISE mission, Johnson measures between 3.62 and 4.791 kilometers in diameter, and its surface has an albedo between 0.19 and 0.44.[7][8][9][10][11] The Collaborative Asteroid Lightcurve Link adopts Petr Pravec's revised WISE-data, that is, an albedo of 0.1524 and a diameter of 4.80 kilometers for an absolute magnitude of 14.255.[4]

Moon and lightcurves

Between 1 and 11 April 2005, the first ever rotational lightcurve was obtained from photometric observations taken by astronomers Brian Warner at the Palmer Divide Observatory, Colorado, by Petr Pravec and Peter Kušnirák at Ondřejov Observatory, Czech Republic, by Adrián Galád and Štefan Gajdoš at Modra Observatory, Slovakia, and by P. Brown and Z. Krzeminski of the Department of Physics and Astronomy at UWO in Ontario, Canada.[6][a]

These observations revealed, that Johnson is a synchronous binary asteroid with a moon orbiting its primary every 21.785 hours. The observed mutual asteroid occultation and eclipsing events had a magnitude of between 0.15 and 0.18 magnitude, suggesting that the satellite's diameter measures 40% of that of Johnson (a secondary-to-primary diameter ratio of 0.4), which translates into a mean-diameter of 1.4–1.9 kilometer.[6][a]

Since Johnson's first observation in April 2005, astronomer Brian Warner and Petr Pravec have obtained additional lightcurves.[d][c] They gave a revised rotation period for the primary of 3.7814 to 3.7824 hours with a brightness variation between 0.10 and 0.20 magnitude (U=3/3/3/3/3). These observations also confirmed that Johnson is a binary system, giving a concurring orbital period of 21.78 to 21.797 hours for the satellite.[13][14][15][b] For an asteroid of its size, Johnson has a somewhat fast spin rate, but still significantly above those of fast rotators. CALL adopts a rotation period of 3.7824 hours with an amplitude of 0.20 magnitude.[4]

Naming

This minor planet was named after American astronomer and engineer Lindley N. Johnson at NASA's Jet Propulsion Laboratory. A space enthusiast since the age of 12, Johnson has been instrumental for the Near-Earth Asteroid Tracking program, which became operational at GEODSS on Hawaii (Haleakala-NEAT; 566) in December 1995.[2] The approved naming citation was published by the Minor Planet Center on 3 May 1996 (M.P.C. 27128).[17]

Notes

  1. ^ a b c d Central Bureau for Astronomical Telegrams – IAUC 8511
    Photometric observations obtained between 1 and 11 April 2005, reveal, that 5905 Johnson is a binary system with an orbital period of 21.78 hours. The primary rotates with a period of 3.783 hours. The lightcurve's amplitude of 0.11 magnitude suggests a nearly spheroidal shape. Mutual eclipse and occultation events between 0.15 and 0.18 magnitude, suggest a secondary-to-primary mean-diameter ratio of 0.4. The system's mean absolute R magnitude is 12.8±0.1.
    Reported by: Brian Warner (Palmer Divide Obs.) Petr Pravec and Peter Kušnirák (Ondřejov Obs., Czech Republic) Donald P. Pray (Carbuncle Hill Obs.); Adrián Galád and Štefan Gajdoš (Modra Obs., Slovakia) and P. Brown and Z. Krzeminski, Department of Physics and Astronomy, University of Western Ontario
  2. ^ a b Pravec (2011) web: rotational lightcurves with a rotation period of 3.7814±0.0002, 3.7814±0.0001 and 3.78142±0.00005 hours, respectively. Brightness amplitude varies between 0.18 and 0.20 mag. Summary figures at Collaborative Asteroid Lightcurve Link and Ondrejov Asteroid Photometry Project
  3. ^ a b Lightcurve plot of (5905) Johnson, with a rotation period of 3.7834 hours from the Palmer Divide Observatory, B. D. Warner (2008). Summary figures at LCDB
  4. ^ List of 8 lightcurve plots of (5905) Johnson:  a · b · c · d · e · f · g · h. Source: unpublished periods of asteroids at the Ondrejov NEO Photometric Program

References

  1. ^ a b c d e "JPL Small-Body Database Browser: 5905 Johnson (1989 CJ1)" (2018-01-26 last obs.). Jet Propulsion Laboratory. Retrieved 28 February 2018.
  2. ^ a b c Schmadel, Lutz D. (2007). "(5905) Johnson". Dictionary of Minor Planet Names – (5905) Johnson. Springer Berlin Heidelberg. p. 496. doi:10.1007/978-3-540-29925-7_5520. ISBN 978-3-540-00238-3.
  3. ^ a b c d "5905 Johnson (1989 CJ1)". Minor Planet Center. Retrieved 16 March 2017.
  4. ^ a b c d e f g "LCDB Data for (5905) Johnson". Asteroid Lightcurve Database (LCDB). Retrieved 16 March 2017.
  5. ^ a b "Asteroid 5905 Johnson – Proper Elements". AstDyS-2, Asteroids – Dynamic Site. Retrieved 29 October 2019.
  6. ^ a b c d e Warner, B.; Pravec, P.; Kusnirak, P.; Pray, D.; Galad, A.; Gajdos, S.; et al. (April 2005). "(5905) Johnson". IAU Circ. 8511 (8511): 2. Bibcode:2005IAUC.8511....2W. Retrieved 16 March 2017.
  7. ^ a b c d Nugent, C. R.; Mainzer, A.; Masiero, J.; Bauer, J.; Cutri, R. M.; Grav, T.; et al. (December 2015). "NEOWISE Reactivation Mission Year One: Preliminary Asteroid Diameters and Albedos". The Astrophysical Journal. 814 (2): 13. arXiv:1509.02522. Bibcode:2015ApJ...814..117N. doi:10.1088/0004-637X/814/2/117. S2CID 9341381. Retrieved 16 March 2017.
  8. ^ a b c d 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.
  9. ^ a b c d 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. hdl:2060/20130014861. S2CID 161887. Retrieved 16 March 2017.
  10. ^ a b c Masiero, Joseph R.; Grav, T.; Mainzer, A. K.; Nugent, C. R.; Bauer, J. M.; Stevenson, R.; et al. (August 2014). "Main-belt Asteroids with WISE/NEOWISE: Near-infrared Albedos". The Astrophysical Journal. 791 (2): 11. arXiv:1406.6645. Bibcode:2014ApJ...791..121M. doi:10.1088/0004-637X/791/2/121. S2CID 119293330. Retrieved 16 March 2017.
  11. ^ a b c d Mainzer, A.; Grav, T.; Masiero, J.; Hand, E.; Bauer, J.; Tholen, D.; et al. (November 2011). "NEOWISE Studies of Spectrophotometrically Classified Asteroids: Preliminary Results". The Astrophysical Journal. 741 (2): 25. arXiv:1109.6407. Bibcode:2011ApJ...741...90M. doi:10.1088/0004-637X/741/2/90. S2CID 35447010.
  12. ^ a b c 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 16 March 2017.
  13. ^ a b c Pravec, P.; Scheirich, P.; Vokrouhlický, D.; Harris, A. W.; Kusnirák, P.; Hornoch, K.; et al. (March 2012). "Binary asteroid population. 2. Anisotropic distribution of orbit poles of small, inner main-belt binaries". Icarus. 218 (1): 125–143. Bibcode:2012Icar..218..125P. doi:10.1016/j.icarus.2011.11.026. Retrieved 16 March 2017.
  14. ^ a b Pravec, P.; Scheirich, P.; Kusnirák, P.; Hornoch, K.; Galád, A.; Naidu, S. P.; et al. (March 2016). "Binary asteroid population. 3. Secondary rotations and elongations". Icarus. 267: 267–295. Bibcode:2016Icar..267..267P. doi:10.1016/j.icarus.2015.12.019. Retrieved 16 March 2017.
  15. ^ a b c Warner, Brian D.; Harris, Alan W.; Pravec, Petr; Cooney, Walter R. Jr.; Gross, John; Terrell, Dirk; et al. (July 2009). "5905 Johnson: A Hungaria Binary". The Minor Planet Bulletin. 36 (3): 89–90. Bibcode:2009MPBu...36...89W. ISSN 1052-8091. Retrieved 16 March 2017.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  16. ^ 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 16 March 2017.
  17. ^ "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 16 March 2017.
Retrieved from "https://en.wikipedia.org/w/index.php?title=5905_Johnson&oldid=1191750952"