2443 Tomeileen

2443 Tomeileen, provisional designation A906 BJ, is a stony Eoan asteroid from the outer regions of the asteroid belt, approximately 32 kilometers (20 miles) in diameter. It was discovered on 24 January 1906, by German astronomer Max Wolf at the Heidelberg-Königstuhl State Observatory in Heidelberg, Germany. The S-type asteroid was named after the parents of British astronomer Brian G. Marsden.[1] It has a rotation period of 3.97 hours.[3]

2443 Tomeileen
Discovery [1]
Discovered byM. F. Wolf
Discovery siteHeidelberg Obs.
Discovery date24 January 1906
Designations
(2443) Tomeileen
Named after
parents of British astronomer Brian G. Marsden [1]
A906 BJ · 1927 DD
1934 PS · 1949 MV
1950 RD1 · 1950 TF3
1953 CH · 1953 EO
1957 WH · 1959 JR
1961 TE1 · 1961 TW1
1965 OE · 1974 DQ1
1974 FC1 · 1981 NN1
main-belt [1][2] · (outer)
Eos [3][4][5]
Orbital characteristics [2]
Epoch 23 March 2018 (JD 2458200.5)
Uncertainty parameter 0
Observation arc111.76 yr (40,821 d)
Aphelion3.1804 AU
Perihelion2.8297 AU
3.0050 AU
Eccentricity0.0584
5.21 yr (1,903 d)
138.10°
0° 11m 21.12s / day
Inclination11.444°
118.77°
68.441°
Physical characteristics
Mean diameter
28.44±0.76 km[6]
30.89±1.6 km[7]
31.878±0.412 km[8]
34.07±0.65 km[9]
37.577±0.236 km[10]
3.974 h[5]
4.0±0.1 h[lower-alpha 1]
6.822±0.001 h[11]
0.1042±0.0091[10]
0.127±0.005[9]
0.1539 (derived)[3]
0.1541±0.017[7]
0.199±0.025[6]
S (SDSS-MFB)[3][lower-alpha 2]
10.10[6] · 10.20[2][3][7][9][10]
10.34±0.41[12]

    Orbit and classification

    Tomeileen is a member the Eos family (606),[3][4] the largest asteroid family of the outer main belt consisting of nearly 10,000 asteroids.[13] It orbits the Sun in the outer main-belt at a distance of 2.8–3.2 AU once every 5 years and 3 months (1,903 days; semi-major axis of 3.01 AU). Its orbit has an eccentricity of 0.06 and an inclination of 11° with respect to the ecliptic.[2] The body's observation arc begins with its official discovery observation at Heidelberg in January 1906.[1]

    Physical characteristics

    Tomeileen has been characterized as a stony S-type asteroid in the SDSS-MFB (Masi Foglia Binzel) taxonomy.[3][lower-alpha 2]

    Rotation period

    Between 2004 and 2010, three rotational lightcurves of Tomeileen were obtained from photometric observations by Brazilian and Argentine astronomers,[5] Amadeo Aznar at Puzol Observatory (J42),[lower-alpha 1] and Laurent Bernasconi in France.[11] Lightcurve analysis gave a rotation period of 3.974, 4.0 and 6.822 hours with a brightness amplitude of 0.1, 0.10 and 0.13 magnitude, respectively (U=2/2/2).[3] A low amplitude is indicative of a spherical rather than elongated shape.

    Diameter and albedo

    According to the surveys carried out by the Infrared Astronomical Satellite IRAS, the Japanese Akari satellite and the NEOWISE mission of NASA's Wide-field Infrared Survey Explorer, Tomeileen measures between 28.44 and 37.577 kilometers in diameter and its surface has an albedo between 0.1042 and 0.199.[6][7][8][9][10]

    The Collaborative Asteroid Lightcurve Link derives an albedo of 0.1539 and a diameter of kilometers based on an absolute magnitude of 10.2.[3]

    Naming

    This minor planet was named after Thomas Marsden (1905–1980) and Eileen (née West) Marsden (1905–1981), the parents of British astronomer and longtime director of the Minor Planet Center (MPC), Brian G. Marsden (1937–2010).[1] The official naming citation was published by the MPC on 8 April 1982 (M.P.C. 6833).[14]

    Notes
    1. Aznar (2011) web: observation from February 2010, rotation period 4.0±0.1 hours with a brightness amplitude of 0.10±0.02 mag. Quality code of 2. Summary figures for (2443) Tomeileen at the LCDB
    2. Search for Unusual Spectroscopic Candidates Among 40313 minor planets from the 3rd Release of the Sloan Digital Sky Survey Moving Object Catalog (publication). SDSS-MFB (Masi Foglia Binzel) taxonomy (catalog).
    gollark: To actually use it you do need to know more than how to install it, though.
    gollark: Much more convenient than multiplying by powers of 10.
    gollark: I use imperial because I just *love* memorizing tables of incomprehensible unit conversions!
    gollark: Randomly delayed *wrongly*, then.
    gollark: Just assume government responses will randomly be delayed, too limited in scope, or cancelled after not being around for long! Although this is more <#689911928411521099>.

    References
    1. "2443 Tomeileen (A906 BJ)". Minor Planet Center. Retrieved 4 April 2018.
    2. "JPL Small-Body Database Browser: 2443 Tomeileen (A906 BJ)" (2017-10-29 last obs.). Jet Propulsion Laboratory. Retrieved 4 April 2018.
    3. "LCDB Data for (2443) Tomeileen". Asteroid Lightcurve Database (LCDB). Retrieved 4 April 2018.
    4. "Asteroid 2443 Tomeileen – Nesvorny HCM Asteroid Families V3.0". Small Bodies Data Ferret. Retrieved 26 October 2019.
    5. Alvarez-Candal, Alvaro; Duffard, René; Angeli, Cláudia A.; Lazzaro, Daniela; Fernández, Silvia (December 2004). "Rotational lightcurves of asteroids belonging to families". Icarus. 172 (2): 388–401. Bibcode:2004Icar..172..388A. doi:10.1016/j.icarus.2004.06.008.
    6. Masiero, Joseph R.; Mainzer, A. K.; Grav, T.; Bauer, J. M.; Cutri, R. M.; Nugent, C.; et al. (November 2012). "Preliminary Analysis of WISE/NEOWISE 3-Band Cryogenic and Post-cryogenic Observations of Main Belt Asteroids". The Astrophysical Journal Letters. 759 (1): 5. arXiv:1209.5794. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8.
    7. Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. 12: IRAS-A-FPA-3-RDR-IMPS-V6.0. Bibcode:2004PDSS...12.....T. Retrieved 22 October 2019.
    8. 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.
    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 17 October 2019. (online, AcuA catalog p. 153)
    10. 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.
    11. Behrend, Raoul. "Asteroids and comets rotation curves – (2443) Tomeileen". Geneva Observatory. Retrieved 4 April 2018.
    12. 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.
    13. Nesvorný, D.; Broz, M.; Carruba, V. (December 2014). Identification and Dynamical Properties of Asteroid Families. Asteroids IV. pp. 297–321. arXiv:1502.01628. Bibcode:2015aste.book..297N. doi:10.2458/azu_uapress_9780816532131-ch016. ISBN 9780816532131.
    14. "MPC/MPO/MPS Archive". Minor Planet Center. Retrieved 4 April 2018.

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