Models of Twenty Asteroids from Photometric Data

Discovery of the triple asteroidal system 87 Sylvia

“…a/b = 1.46, b/c=1.14 with Re= 143 km) with a 4% error, very close to the shape model derived by lightcurve inversion 13 . The averaged size is 10% larger than the one determined by radiometric IRAS measurement in the far-IR 14 .…”

“…Considering the pole orientation determined by the analysis of the moonlet orbits which is also in agreement with lightcurve inversion pole solution 13 , the shape of Sylvia primary can be approximated considering an ellipsoid with a=192 km, b=132 km, and c=116 km (i.e. a/b = 1.46, b/c=1.14 with Re= 143 km) with a 4% error, very close to the shape model derived by lightcurve inversion 13 .…”

Photocentre offset in ultraprecise astrometry: Implications for barycentre determination and asteroid modelling

“…Note that even large asteroids typically have strong local irregularities even if their global shapes were "pseudoellipsoidal" (Kaasalainen et al 2002b;Torppa et al 2003). Simulations with such shapes produce results similar to those above.…”

Dynamical passage to approximate equilibrium shapes for spinning, gravitating rubble asteroids

“…To these diagrams we have added the positions of several asteroids. The rotation and the best-fit ellipsoidal shape of these asteroids were obtained by Kaasalainen et al (2002), Torppa et al (2003) and Kaasalainen et al (2004) from photometric data. The physical properties of all near-Earth objects (including 1036 Ganymed, 1580 Betulia, 2100 Ra-Shalom, 3103 Eger, 3199 Nefertiti, 4957 Brucemurray, 5587 1990 SB and 6053 1990 BW3, which are given in Figs.…”