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Asteroid collisions as origin of debris disks: Asteroid shape reconstruction from BNAO Rozhen photometry

Published online by Cambridge University Press:  12 October 2020

G. Apostolovska Open the ORCID record for G. Apostolovska [Opens in a new window] ,
E. Vchkova Bebekovska Open the ORCID record for E. Vchkova Bebekovska [Opens in a new window] ,
A. Kostov  and
Z. Donchev
G. Apostolovska
Affiliation:
Institute of Physics, Faculty of Science, Ss. Cyril and Methodius University, Arhimedova 3, 1000 Skopje, Republic of Macedonia email: gordanaapostolovska@gmail.com
E. Vchkova Bebekovska
Affiliation:
Institute of Physics, Faculty of Science, Ss. Cyril and Methodius University, Arhimedova 3, 1000 Skopje, Republic of Macedonia email: gordanaapostolovska@gmail.com
A. Kostov
Affiliation:
Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Tsarigradsko Chaussee Blvd. 72, BG-1784, Sofia, Bulgaria
Z. Donchev
Affiliation:
Institute of Astronomy and National Astronomical Observatory, Bulgarian Academy of Sciences, Tsarigradsko Chaussee Blvd. 72, BG-1784, Sofia, Bulgaria
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Abstract

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As a result of collisions during their lifetimes, asteroids have a large variety of different shapes. It is believed that high velocity collisions or rotational spin-up of asteroids continuously replenish the Sun’s zodiacal cloud and debris disks around extrasolar planets (Jewitt (2010)). Knowledge of the spin and shape parameters of the asteroids is very important for understanding collision asteroid processes. Lately photometric observations of asteroids showed that variations in brightness are not accompanied by variations in colour index which indicate that the shape of the lightcurve is caused by varying illuminations of the asteroid surface rather than albedo variations over the surface. This conclusion became possible when photometric investigations were combined with laboratory experiments (Dunlap (1971)). In this article using the convex lightcurve inversion method we obtained the sense of rotation, pole solutions and preliminary shape of 901 Brunsia.

Keywords

Minor planetsasteroidsdebris disks: individual: 901 Brunsia
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S350: Laboratory Astrophysics: From Observations to Interpretation , April 2019 , pp. 451 - 453
Copyright
© International Astronomical Union 2020

References

Ďurech, J., Sidorin, V., & Kaasalainen, M. 2010, A&A, 513, 46 Google Scholar
Dunlap, J. 1971, in: Gehrels, T. (eds.), Physical Studies of Minor Planets, NASSP, 267, p. 147 Google Scholar
Jewitt, D., Weaver, H., Agarwal, J., Mutchler, M., & Drahus, M. 2010, Nature, 467, 817 CrossRefGoogle Scholar
Kaasalainen, M., Torppa, J., & Muinonen, K. 2001, Icarus, 153, 37 CrossRefGoogle Scholar
Kryszczyńska, A., Colas, F., Polińska, M., et al. 2012, A&A, 546, 72 Google Scholar
Warner, B., Harris, A., Pravec, P. 2009, Icarus, 202, 134 10.1016/j.icarus.2009.02.003CrossRefGoogle Scholar
Warner, B. 2011, MPO Canopus Software. http://www.MinorPlanetObserver.com Google Scholar