Component properties and mutual orbit of binary main-belt comet 288P/(300163) 2006 VW139

被引:8
|
作者
Agarwal, J. [1 ,2 ]
Kim, Y. [1 ]
Jewitt, D. [3 ,4 ]
Mutchler, M. [5 ]
Weaver, H. [6 ]
Larson, S. [7 ]
机构
[1] Max Planck Inst Sonnensystemforsch, Justus von Liebig Weg 3, D-37077 Gottingen, Germany
[2] Tech Univ Carolo Wilhelmina Braunschweig, Inst Geophys & Extraterr Phys, Mendelssohnstr 3, D-38106 Braunschweig, Germany
[3] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, 595 Charles Young Dr East,Box 951567, Los Angeles, CA 90095 USA
[4] Univ Calif Los Angeles, Dept Phys & Astron, 430 Portola Plaza, Los Angeles, CA 90095 USA
[5] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 USA
[6] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA
[7] Univ Arizona, Lunar & Planetary Lab, 1629 E Univ Blvd, Tucson, AZ 85721 USA
基金
欧洲研究理事会;
关键词
minor planets; asteroids: individual: 288P; (300163); POPULATION; ASTEROIDS;
D O I
10.1051/0004-6361/202038195
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Context. The binary asteroid 288P/(300163) is unusual both for its combination of wide-separation and high mass ratio and for its comet-like activity. It is not currently known whether there is a causal connection between the activity and the unusual orbit or if instead the activity helped to overcome a strong detection bias against such sub-arcsecond systems.Aims. We aim to find observational constraints discriminating between possible formation scenarios and to characterise the physical properties of the system components.Methods. We measured the component separation and brightness using point spread function fitting to high-resolution Hubble Space Telescope/Wide Field Camera 3 images from 25 epochs between 2011 and 2020. We constrained component sizes and shapes from the photometry, and we fitted a Keplerian orbit to the separation as a function of time.Results. Approximating the components A and B as prolate spheroids with semi-axis lengths a < b and assuming a geometric albedo of 0.07, we find a(A) <less than or equal to> 0.6 km, b(A) >= 1.4 km, a(B) <= 0.5 km, and b(B) >= 0.8 km. We find indications that the dust production may have concentrated around B and that the mutual orbital period may have changed by 1-2 days during the 2016 perihelion passage. Orbit solutions have semi-major axes in the range of (105-109) km, eccentricities between 0.41 and 0.51, and periods of (117.3-117.5) days pre-perihelion and (118.5-119.5) days post-perihelion, corresponding to system masses in the range of (6.67-7.23) x 10(12) kg. The mutual and heliocentric orbit planes are roughly aligned.Conclusions. Based on the orbit alignment, we infer that spin-up of the precursor by the Yarkovsky-O'Keefe-Radzievskii-Paddack (YORP) effect led to the formation of the binary system. We disfavour (but cannot exclude) a scenario of very recent formation where activity was directly triggered by the break-up, because our data support a scenario with a single active component.
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页数:38
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