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360 Carlova

From Wikipedia, the free encyclopedia

360 Carlova
Lightcurve-base 3D-model of Carlova on the top with an image of the asteroid on the bottom.
Discovery
Discovered byAuguste Charlois
Discovery date11 March 1893
Designations
1893 N
Main belt
AdjectivesCarlovian
Orbital characteristics[1]
Epoch 31 July 2016 (JD 2457600.5)
Uncertainty parameter 0
Observation arc111.79 yr (40832 d)
Aphelion3.53698 AU (529.125 Gm)
Perihelion2.46807 AU (369.218 Gm)
3.00253 AU (449.172 Gm)
Eccentricity0.17800
5.20 yr (1900.3 d)
350.473°
0° 11m 21.988s / day
Inclination11.6967°
132.551°
287.862°
Physical characteristics
Dimensions115.76±4.3 km
6.183 h (0.2576 d)
0.0535±0.004
C
8.48

360 Carlova is a very large main-belt asteroid.[1] It is classified as a C-type asteroid and is probably composed of carbonaceous material.[2] Dust activity due to sublimation has been detected on this asteroid, suggesting the presence of water ice in its interior.[3]

The asteroid has a convex, roughly ellipsoid shape.[2] The sidereal rotation period is 6.1873 hours with an axis of rotation along the ecliptic coordinates (l, b) = (95°±, 40°±).[4] It was discovered by Auguste Charlois on 11 March 1893 in Nice.

References

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  1. 1 2 "360 Carlova (1893 N)". JPL Small-Body Database. NASA/Jet Propulsion Laboratory. Retrieved 11 May 2016.
  2. 1 2 Wang, Xiaobin; et al. (September 2015), "Photometric analysis for the spin and shape parameters of the C-type main-belt asteroids (171) Ophelia and (360) Carlova", Astronomy & Astrophysics, 581: 5, Bibcode:2015A&A...581A..55W, doi:10.1051/0004-6361/201526523, A55.
  3. Busarev, V. V.; et al. (December 2024). "Sublimation-Driven Dust Activity of Primitive-Type Asteroids as a Sign of the Presence of H2O Ice". Solar System Research. 58 (6): 715–731. Bibcode:2024SoSyR..58..715B. doi:10.1134/S0038094624700503.
  4. Wang, Xiao-bin; Zhang, Xi-liang (October 2006), "Determination of rotational parameters of asteroid (360) Carlova", Chinese Astronomy and Astrophysics, 30 (4): 410–419, Bibcode:2006ChA&A..30..410W, doi:10.1016/j.chinastron.2006.10.007.
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