2011
DOI: 10.1051/0004-6361/201015365
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Photometry and models of selected main belt asteroids

Abstract: 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 parameter… Show more

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Cited by 12 publications
(10 citation statements)
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References 28 publications
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“…The short time span between the observational epoches and the small amplitudes of the light curves in the 2006 and 2010 apparitions should lower the estimation accuracy of the rotation period, and therefore cause the difference from the result of Marciniak et al (). Based on a similar inversion process as mentioned above, however, we directly fixed the rotation period as P = 8.456016 hr and then obtained the orientation of the pole (220°, 34°), which is not substantially different from (219°, 29°).…”
Section: Resultsmentioning
confidence: 86%
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“…The short time span between the observational epoches and the small amplitudes of the light curves in the 2006 and 2010 apparitions should lower the estimation accuracy of the rotation period, and therefore cause the difference from the result of Marciniak et al (). Based on a similar inversion process as mentioned above, however, we directly fixed the rotation period as P = 8.456016 hr and then obtained the orientation of the pole (220°, 34°), which is not substantially different from (219°, 29°).…”
Section: Resultsmentioning
confidence: 86%
“…Shevchenko et al () first evaluated Pax's orientation of pole ( λ p = 65° ± 2°, β p = −5° ± 3°) or ( λ p = 245° ± 2°, β p = 5° ± 2°). Marciniak et al () obtained the photometric data of (679) Pax during six apparitions: in 2002, 2004, 2005, 2006, 2009, and 2010, and then determined two group solutions of its spin state: the orientation of pole ( λ p = 220° ± 5°, β p = 32° ± 5°) and ( λ p = 42° ± 5°, β p = −5° ± 5°) with a sidereal rotation period P = 8.456016 hr. Comparing to the image of Pax from the adaptive optics observation that was made by Marchis et al (), Marciniak et al () inferred that the first solution (220°, 32°) should be preferred.…”
Section: Resultsmentioning
confidence: 99%
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“…This inversion technique has been used by several authors during the last decade (e.g. [13], [24], [25]) resulting in around a hundred of convex asteroid models based on dense lightcurves.…”
Section: Shape Modelsmentioning
confidence: 99%
“…Since the publication of the method, models of about 500 asteroids were derived by this technique (Ďurech et al, 2009;Ďurech et al, 2011;Hanuš et al, 2011Hanuš et al, , 2013bMarciniak et al, 2011, for example); most of them are publicly available in the Database of Asteroid Models from Inversion Techniques (DAMIT 1 , Durech et al, 2010). At this site, the source codes for the lightcurve inversion called convexinv can be downloaded.…”
Section: Asteroid Lightcurve Inversionmentioning
confidence: 99%