Hostname: page-component-cd9895bd7-gvvz8 Total loading time: 0 Render date: 2024-12-26T07:05:37.695Z Has data issue: false hasContentIssue false
  • English
  • Français

Shape and spin of asteroid 967 Helionape

Published online by Cambridge University Press:  07 March 2018

G. Apostolovska ,
A. Kostov ,
Z. Donchev ,
E. Vchkova Bebekovska  and
O. Kuzmanovska
G. Apostolovska
Affiliation:
Institute of Physics, Faculty of Science, Ss. Cyril and Methodius University, Skopje, Republic of Macedonia, Arhimedova 3, 1000 Skopje, Republic of Macedonia email: gordanaaspostolovska@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
E. Vchkova Bebekovska
Affiliation:
Institute of Physics, Faculty of Science, Ss. Cyril and Methodius University, Skopje, Republic of Macedonia, Arhimedova 3, 1000 Skopje, Republic of Macedonia email: gordanaaspostolovska@gmail.com
O. Kuzmanovska
Affiliation:
Institute of Physics, Faculty of Science, Ss. Cyril and Methodius University, Skopje, Republic of Macedonia, Arhimedova 3, 1000 Skopje, Republic of Macedonia email: gordanaaspostolovska@gmail.com
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Knowledge of the spin and shape parameters of the asteroids is very important for understanding of the conditions during the creation of our planetary system and formation of asteroid populations. The main belt asteroid and Flora family member 967 Helionape was observed during five apparitions. The observations were made at the Bulgarian National Astronomical Observatory (BNAO) Rozhen, since March 2006 to March 2016. Lihtcurve inversion method (Kaasalainen et al. (2001)), applied on 12 relative lightcurves obtained at various geometric conditions of the asteroid, reveals the spin vector, the sense of rotation and the preliminary shape model of the asteroid. Our aim is to contribute in increasing the set of asteroids with known spin and shape parameters. This could be done with dense lightcurves, obtained during small number of apparitions, in combination with sparse data produced by photometric asteroid surveys such as the Gaia satellite (Hanush (2011)).

Keywords

Minor planetsasteroidsphotometric-Asteroids: individual: 967 Helionape
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S330: Astrometry and Astrophysics in the Gaia sky , April 2017 , pp. 393 - 394
Copyright
Copyright © International Astronomical Union 2018 

References

Apostolovska, G., Ivanova, V., & Kostov, A., 2009, MPB, 36, 27 Google Scholar
Buie, M., 1998, http://www.boulder.swri.edu/~buie/idl/ccdphot.html Google Scholar
Ďurech, J., Sidorin, V., & Kaasalainen, M., 2010, A&A, 513, 46 Google Scholar
Hanush, J., 2011, Astron. Astrophys., 530, 134 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
Mainzer, A., Bauer, J., Cutri, R., et al., 2016, PDSS, 247 Google Scholar
Warner, B., Harris, A., & Pravec, P., 2009, Icarus, 202, 134, Updated 2017 April. http://www.minorplanet.info/lightcurvedatabase.html CrossRefGoogle Scholar
Warner, B., 2011, MPO Canopus Software. http://www.MinorPlanetObserver.com Google Scholar