Volume 529, May 2011
|Number of page(s)||14|
|Section||Planets and planetary systems|
|Published online||12 April 2011|
Photometry and models of selected main belt asteroids
Astronomical Observatory, Adam Mickiewicz University, Słoneczna 36, 60-286 Poznań, Poland
2 Geneva Observatory, 1290 Sauverny, Switzerland
3 Les Engarouines Observatory, 84570 Mallemort-du-Comtat, France
4 Collonges Observatory, 90 allée des résidences, 74160 Collonges, France
5 “Le Florian”, Villa 4, 880 chemin de Ribac-Estagnol, 06600 Antibes, France
6 AUDE Association (User association of electronic detectors) Paris, France
7 Agrupación Astronómica de Sabadell, Apartado de Correos 50, PO Box 50, 08200 Sabadell, Barcelona, Spain
8 l’Observatoire de Cabris, 408 chemin Saint Jean Pape, 06530 Cabris, France
9 Stazione Astronomica di Sozzago, 28060 Sozzago, Italy
10 Blauvac Observatory, 84570 St-Estève, France
11 N. Copernicus Astronomical Centre, Polish Academy of Sciences, Bartycka 18, 00-716 Warsaw, Poland
12 Forte Software, Os. Jagiełły 28/28 60-685 Poznań, Poland
13 Ludick Observatory, Krugersdorp, South Africa
Received: 8 July 2010
Accepted: 16 February 2011
Context. The set of more than 100 asteroids, for which spin parameters have been modelled using an amplitude, magnitude or epoch methods, showed a pronounced gap in the distribution of the asteroid spin axes. These spin axes are rarely aligned with the ecliptic plane.
Aims. The number of asteroids with known spin parameters should be increased to allow for statistical investigations.
Methods. We gathered extensive photometric datasets on four selected main-belt asteroids to model their spin and shape parameters using the lightcurve inversion method. Our only criterion of selection was their observability for small telescopes.
Results. All four of the modelled asteroids happened to have rotational poles that lie close to the ecliptic plane (periods and J2000 north pole coordinates): (94) Aurora − P = 7.226191 h, λp1 = 58°, βp1 = + 16°; λp2 = 242°, βp2 = + 4°; (174) Phaedra − P = 5.750249 h, λp = 265°, βp = + 5°; (679) Pax − P = 8.456016 h, λp1 = 42°, βp1 = −5°; λp2 = 220°, βp2 = + 32° (pole 2 preferred after comparison with AO-resolved observations); (714) Ulula − P = 6.998376 h, λp1 = 42°, βp1 = −9°; λp2 = 227°, βp2 = −14°.
Conclusions. This work suggests that asteroid spin axes do not avoid the ecliptic plane, contrary to what the classical modelling suggested.
Key words: techniques: photometric / minor planets, asteroids: general
Photometric data are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/529/A107
© ESO, 2011
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.