1207 Ostenia

1207 Ostenia

Light-curve-based 3D- model of 1207 Ostenia
Discovery [1]
Discovered by K. Reinmuth
Discovery site Heidelberg Obs.
Discovery date 15 November 1931
Designations
MPC designation 1207 Ostenia
Named after
 Hans Osten
(amateur astronomer)[2]
1931 VT · 1959 EF1
main-belt · Eos [3]
Orbital characteristics [1]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc 84.41 yr (30829 days)
Aphelion 3.2786 AU (490.47 Gm)
Perihelion 2.7644 AU (413.55 Gm)
3.0215 AU (452.01 Gm)
Eccentricity 0.085080
5.25 yr (1918.4 d)
51.698°
0° 11m 15.576s / day
Inclination 10.363°
20.130°
43.523°
Earth MOID 1.78513 AU (267.052 Gm)
Jupiter MOID 2.05644 AU (307.639 Gm)
Jupiter Tisserand parameter 3.216
Physical characteristics
Dimensions 22.93 km[4]
21.92±0.63 km[5]
23.05 km (derived)[3]
Mean radius
 11.465±0.65 km
9.073 h (0.3780 d)[1][6]
7.7 h[7]
8.4 h[8]
9.07129 h[9]
9.07129±0.00005 h[10]
0.1338[4]
0.176±0.024[5]
0.1591 (derived)[3]
0.1338±0.016[1]
S [3]
10.8

    1207 Ostenia, provisional designation 1931 VT, is a stony asteroid from the outer region of the asteroid belt, about 23 kilometers in diameter. It was discovered by German astronomer Karl Reinmuth at Heidelberg Observatory in southern Germany on 15 November 1931.[11]

    The S-type asteroid is a member of the Eos family, thought to have formed from a catastrophic collision of its parent body resulting in more than 4,000 known members of the family. It orbits the Sun at a distance of 2.8–3.3 AU once every 5 years and 3 months (1,919 days). Its orbit shows an eccentricity of 0.09 and is tilted by 10 degrees to the plane of the ecliptic. It has an albedo of 0.13–0.18, according to the space-based surveys carried out by the Infrared Astronomical Satellite, IRAS, and the Wide-field Infrared Survey Explorer missions.[4][5]

    Photometric observations of the asteroid during 2006 at the Palmer Divide Observatory in Colorado Springs, Colorado (see § External links), were used to generate a light-curve with a period of 9.073±0.004 hours and a variation in brightness of 0.60±0.02 magnitude.[6] Subsequent measurements in 2009 and 2011 confirmed the rotation period to be 9.07 hours[9][10] while two older observations made in the 1970s gave significant shorter periods of 7.7 and 8.4 hours, respectively.[7][8]

    The minor planet was named after Hans Osten (1875–1936) a German amateur astronomer, orbit computer and business man.[2] As a non-professional, Osten attracted attention with his precises calculations of comets and asteroids. He is known for calculating the orbit of 447 Valentine, taking into account perturbations by all major planets with such precision, that it was considered exemplary in the astronomical community. Osten received the silver Leibniz Medal in 1911.[12]

    References

    1. 1 2 3 4 "JPL Small-Body Database Browser: 1207 Ostenia (1931 VT)" (2015-09-28 last obs.). Jet Propulsion Laboratory. Retrieved 30 April 2016.
    2. 1 2 Schmadel, Lutz D. (2003). Dictionary of Minor Planet Names – (1207) Ostenia. Springer Berlin Heidelberg. p. 101. ISBN 978-3-540-29925-7. Retrieved 22 November 2015.
    3. 1 2 3 4 "LCDB Data for (1207) Ostenia". Asteroid Lightcurve Database (LCDB). Retrieved 22 November 2015.
    4. 1 2 3 Tedesco, E. F.; Noah, P. V.; Noah, M.; Price, S. D. (October 2004). "IRAS Minor Planet Survey V6.0". NASA Planetary Data System. Bibcode:2004PDSS...12.....T. Retrieved 22 November 2015.
    5. 1 2 3 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:1209.5794Freely accessible. Bibcode:2012ApJ...759L...8M. doi:10.1088/2041-8205/759/1/L8. Retrieved 22 November 2015.
    6. 1 2 Warner, Brian D. (September 2006). "Asteroid lightcurve analysis at the Palmer Divide Observatory - late 2005 and early 2006". The Minor Planet Bulletin. 33 (3): 58–62. Bibcode:2006MPBu...33...58W. ISSN 1052-8091. Retrieved 22 November 2015.
    7. 1 2 Lagerkvist, C.-I. (March 1978). "Photographic photometry of 110 main-belt asteroids". Astronomy and Astrophysics Supplement Series: 361–381. Bibcode:1978A&AS...31..361L. Retrieved 22 November 2015.
    8. 1 2 Lagerkvist, C. I. (April 1979). "A lightcurve survey of asteroids with Schmidt telescopes - Observations of nine asteroids during oppositions in 1977". Icarus: 106–114. Bibcode:1979Icar...38..106L. doi:10.1016/0019-1035(79)90090-3. Retrieved 22 November 2015.
    9. 1 2 Durech, J.; Kaasalainen, M.; Warner, B. D.; Fauerbach, M.; Marks, S. A.; Fauvaud, S.; et al. (January 2009). "Asteroid models from combined sparse and dense photometric data". Astronomy and Astrophysics. 493 (1): 291–297. Bibcode:2009A&A...493..291D. doi:10.1051/0004-6361:200810393. Retrieved 22 November 2015.
    10. 1 2 Hanus, J.; Durech, J.; Broz, M.; Warner, B. D.; Pilcher, F.; Stephens, R.; et al. (June 2011). "A study of asteroid pole-latitude distribution based on an extended set of shape models derived by the lightcurve inversion method". Astronomy & Astrophysics. 530: 16. arXiv:1104.4114Freely accessible. Bibcode:2011A&A...530A.134H. doi:10.1051/0004-6361/201116738. Retrieved 22 November 2015.
    11. ↑ "1207 Ostenia (1931 VT)". Minor Planet Center. Retrieved 22 November 2015.
    12. ↑ "Osten, Hans. Astronom, * 31.3.1875 Bremen, † 29.3.1936 Montevideo (Uruguay).". Deutsche Biographie.de (in German). Retrieved 22 November 2015.

    External links

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