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720 Bohlinia is a minor planet orbiting the Sun that was discovered by Franz Kaiser, a German astronomer in 1911. It is named for Swedish astronomer Karl Petrus Theodor Bohlin, to mark his 65th birthday.[4] He had worked on the orbits of asteroids.[5]

720 Bohlinia
A three-dimensional model of 720 Bohlinia based on its light curve
Discovery
Discovered byFranz Kaiser
Discovery siteHeidelberg
Discovery date18 October 1911
Designations
MPC designation
(720) Bohlinia
Alternative designations
1911 MW
Orbital characteristics[1]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc117.11 yr (42775 d)
Aphelion2.9376 AU (439.46 Gm)
Perihelion2.8371 AU (424.42 Gm)
Semi-major axis
2.8873 AU (431.93 Gm)
Eccentricity0.017406
Orbital period (sidereal)
4.91 yr (1792.0 d)
Mean anomaly
350.275°
Mean motion
0° 12m 3.204s / day
Inclination2.3562°
Longitude of ascending node
35.706°
Argument of perihelion
118.762°
Physical characteristics
Mean radius
16.865±0.7 km[1]
17.32 ± 0.905 km[2]
Mass(5.97 ± 0.80) × 1016 kg[2]
Mean density
2.74 ± 0.56 g/cm3[2]
Synodic rotation period
8.919 h (0.3716 d)
Geometric albedo
0.203[3]
0.2029±0.018[1]
Absolute magnitude (H)
9.71[3]
9.6[1]

    It is one of the Koronis family of asteroids. A group of astronomers, including Lucy d’Escoffier Crespo da Silva and Richard P. Binzel, used observations made between 1998 through 2000 to determine the spin-vector alignment of these asteroids. The collaborative work resulted in the creation of 61 new individual rotation lightcurves to augment previous published observations.[6]

    Binzel and Schelte Bus further added to the knowledge about this asteroid in a lightwave survey published in 2003. This project was known as Small Main-belt Asteroid Spectroscopic Survey, Phase II or SMASSII, which built on a previous survey of the main-belt asteroids. The visible-wavelength (0.435-0.925 micrometre) spectra data was gathered between August 1993 and March 1999.[7]


    References


    1. "720 Bohlinia (1911 MW)". JPL Small-Body Database. NASA/Jet Propulsion Laboratory. Retrieved 6 May 2016.
    2. Carry, B. (December 2012), "Density of asteroids", Planetary and Space Science, 73 (1): 98–118, arXiv:1203.4336, Bibcode:2012P&SS...73...98C, doi:10.1016/j.pss.2012.03.009, S2CID 119226456. See Table 1.
    3. Delbo', Marco; Tanga, Paolo (February 2009), "Thermal inertia of main belt asteroids smaller than 100 km from IRAS data", Planetary and Space Science, 57 (2): 259–265, arXiv:0808.0869, Bibcode:2009P&SS...57..259D, doi:10.1016/j.pss.2008.06.015, S2CID 14517561.
    4. "Small-Body Database Lookup".
    5. Hockey, Thomas (2009). The Biographical Encyclopedia of Astronomers. Springer Publishing. ISBN 978-0-387-31022-0. Retrieved 22 August 2012.
    6. Slivan, S. M., Binzel, R. P., Crespo da Silva, L. D., Kaasalainen, M., Lyndaker, M. M., Krco, M.: “Spin vectors in the Koronis family: comprehensive results from two independent analyses of 213 rotation lightcurves,”Icarus, 162, 2003, pp. 285–307.
    7. Bus, S., Binzel, R. P. Small Main-belt Asteroid Spectroscopic Survey, Phase II. EAR-A-I0028-4-SBN0001/SMASSII-V1.0. NASA Planetary Data System, 2003.



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    На других языках

    [de] (720) Bohlinia

    (720) Bohlinia ist ein Asteroid des Hauptgürtels, der am 18. Oktober 1911 vom deutschen Astronomen Franz Kaiser in Heidelberg entdeckt wurde.
    - [en] 720 Bohlinia

    [es] (720) Bohlinia

    (720) Bohlinia es un asteroide perteneciente al cinturón de asteroides descubierto el 18 de octubre de 1911 por Franz Heinrich Kaiser desde el observatorio de Heidelberg-Königstuhl, Alemania. Está nombrado en honor del astrónomo sueco Karl Petrus Theodor Bohlin (1860-1939).[2] Forma parte de la familia asteroidal de Coronis.[3]

    [ru] (720) Болиния

    (720) Болиния (швед. Bohlinia) — небольшой астероид главного пояса, который принадлежит к светлому спектральному классу S и входит в состав семейства Корониды. Он был открыт 25 января 1914 года немецким астрономом Францем Кайзером в обсерватории Хайдельберг, Германия и назван в честь шведского астронома Карла Болина[3][4].


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