Photometry and models of selected main belt asteroids

Marciniak, A.; Michałowski, Tadeusz; Kaasalainen, M.; Ďurech, Josef; Polińska, M.; Kwiatkowski, T.; Kryszczyńska, A.; Hirsch, R.; Kamiński, K.; Fagas, M.; Colas, François; Fauvaud, S.; Santacana, G.; Behrend, R.; Roy, R.

doi:10.1051/0004-6361:20077694

Cited by 19 publications

(10 citation statements)

References 17 publications

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“…Similar observations and models for different asteroids can be found in the four previous papers of the present series: Michałowski et al (2004Michałowski et al ( , 2005Michałowski et al ( , 2006 and Marciniak et al (2007). The photometric measurements that we perform are relative, and are usually done on small telescopes, for example in Borowiec we use 0.4-m reflector.…”

Section: Photometry Of Three Main Belt Asteroidssupporting

confidence: 59%

Photometry and models of selected main belt asteroids

Marciniak¹,

Michałowski²,

Kaasalainen

et al. 2007

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We present photometric observations of three asteroids: 73 Klytia, 377 Campania, and 378 Holmia, together with their spin and shape models. The models were constructed with the lightcurve inversion method, using all available lightcurves of these objects. In the case of Campania, the long persisting doubts about its rotational period have been resolved. Various authors state periods between 8.48 and 16 h, while the period we determined is 11.664401 ± 0.000010 h.

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Section: Photometry Of Three Main Belt Asteroidssupporting

confidence: 59%

Photometry and models of selected main belt asteroids

Marciniak¹,

Michałowski²,

Kaasalainen

et al. 2007

A&A

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“…This sample is different from the previous ones (included in Michałowski et al 2004Michałowski et al , 2005Michałowski et al , 2006Marciniak et al 2007Marciniak et al , 2008Marciniak et al , 2009a in the way that it contains only objects with poles of low inclination with respect to the ecliptic. These asteroids were long thought to be nonexistent, because modelling with the amplitude, magnitude, and epoch methods (Zappala & Di Martino 1986, and references therein) did not result in asteroid models with poles lying in the proximity of the 1 Database of Asteroid Models from Inversion Techniques, available at: http://astro.troja.mff.cuni.cz/projects/asteroids3D, described inĎurech et al (2010).…”

Section: Introductionmentioning

confidence: 93%

Photometry and models of selected main belt asteroids

Marciniak

Michałowski

Polińska

et al. 2011

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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, λ p1 = 58• (pole 2 preferred after comparison with AO-resolved observations); (714) Ulula − P = 6.998376 h, λ p1 = 42 • , β p1 = −9 • ; λ p2 = 227 • , β p2 = −14 • . Conclusions. This work suggests that asteroid spin axes do not avoid the ecliptic plane, contrary to what the classical modelling suggested.

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“…We adopt here the spin-state solution from Marciniak et al (2007), which has a sidereal rotation period of 6.44111 h and two possible pole orientations, namely (λ, β) = (200…”

Section: (184) Dejopejamentioning

confidence: 99%

Low-frequency Slivan states in the outer main belt?

Vraštil

Vokrouhlický

2016

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Context. Spin states of several main belt asteroids have been recently found to reside in what is called the Slivan state, namely a secular spin-orbit resonance with the s 6 mode of their orbital precession in space. Aims. We examine a possibility of the Slivan states of asteroids with other than orbital s 6 precession frequency. Methods. The asteroids' orbital and spin states are numerically propagated using well-tested computer codes. We select parameter space favorable for the Slivan-state capture with the s 7 frequency mode of the orbital precession. The stability of these states is numerically verified. Results. We find that asteroid (184) Dejopeja has a spin state captured in (or very nearly) the Slivan state with the s 7 orbital frequency. In general, such a situation may favorably occur for low-inclination orbits in the outermost part of the main asteroid belt. We expect these states to be common among the Themis family members.

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Photometry and models of selected main belt asteroids

Cited by 19 publications

References 17 publications

Photometry and models of selected main belt asteroids

Photometry and models of selected main belt asteroids

Photometry and models of selected main belt asteroids

Low-frequency Slivan states in the outer main belt?

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