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supervisor: David Vokrouhlicky
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[PDF, 37 MB]
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[PDF, slides 800×600 pxl, 1.5 MB]
[TeX source, 240 kB]
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The thesis was defended on Jun 28th 2006. This version was last updated on Jun 29th 2006.
Click to obtain hi-resolution figures. Figure captions are included in the PDF file above.
You can use MPlayer to play the following animations. Compiled executables for i386/Linux and Windows are at disposal, a bash script or a batch file can be used to start the Mplayer.
Yarkovsky_effect_1d_regolith.avi[AVI, DIV-X codec, 545 kB]
An estimate of the temperature T (colour coded) in the depth x (vertical coordinate) - some sort of `an asteroid cross-section' for a regolith-like material with the thermal conductivity K = 0.01 W/m/K. The situation depicted here corresponds to the 1-D analytical toy model.
Golevka_temperature_Capek.avi[AVI, M-JPEG codec, 30 MB]
The temperature distribution on the surface of the asteroid (6489) Golevka, calculated by a numerical solution of the 1-dimensional heat diffusion equation, individually for all 4092 surface elements of the shape model. Data kindly provided by David Capek.
r21_distmap33.avi[AVI, M-JPEG, 109 MB]
The comparison of the positions of J2/1 resonant asteroids, calculated in the space of pseudo-proper resonant elements, with the analytical borders of the 2/1 mean motion resonance with Jupiter and the secular resonances embedded inside (data from Moons et al.). Zhongguos are denoted by open circles, Griquas by squares, the unstable asteroids by crosses.
r21_distmap31.avi[AVI, M-JPEG, 47 MB]
The observed positions of Zhongguos, Griquas and unstable asteroids in the pseudo-proper elements space and the 2-dimensional number densities QTP of the simulated Yarkovsky-driven test particles in the (ap, ep), (ap, sin ip), and (ep, sin ip) planes.
r21_distmap26.avi[AVI, M-JPEG, 134 MB]
The comparsion of the observed positions of Zhongguos, Griquas and unstable asteroids to the 3-dimensional number densities nTP of the Yarkovsky-driven test particles originated in the Themis family. Two semi-transparent iso-surfaces (corresponding to nTP = 100 and nTP = 1000) are depicted. The blue arrow denotes the approximate position, where the test particles enter the J2/1 resonance. There is one selected trajectory of a test particle visible at the beginning of the animation.
r21_MCmodel_job6n.avi[AVI, M-JPEG, 49 MB]
The Monte-Carlo model of the J2/1 resonant population. (Left) The number larger resonant asteroids, which can be observed, vs time (from 0 to 4 Gy); the numbers of bodies originating in three source populations (Main Belt, Themis and Hygeia) are discriminated by colors. (Right) The corresponding size-frequency distribution of the simulated population at the given time and the comparsion to the source Main Belt population. A systematic change of the SFD slope corresponds to the size dependence of the Yarkovsky effect.
Eos_family_aei.avi[AVI, M-JPEG, 42 MB]
The observed Eos family (identified by the hierarchical clustering method with the cut-off velocity 55 m/s) and the evolution of three selected test particles in the space of proper elements ap, ep, sin ip. Three processes, how the Yarkovsky drifting orbits interact with resonances are demonstrated: `bracketing' by the J7/3 mean motion resonance, `crossing' of the J9/4 resonance and `trapping' in the z1 secular resonance.
Eos_family_ae.avi[AVI, M-JPEG, 26 MB]
The simulated 600 My evolution of the Eos family asteroids in the proper semimajor axis vs. proper eccentricity plot and the comparison to the observed family members. The positions of mean motion and secular resonances are denoted by thin lines.
Merxia_family.avi[AVI, M-JPEG, 65 MB]
The observed Merxia family asteroids (big orange dots) in the (ap, ep, sin ip) proper element space and simulated asteroids (black lines) drifting due to the Yarkovsky effect from the centre to larger semimajor axes (i.e., in the direction of the blue arrow). The 3J-1S-1 three-body resonance (which position is indicated by the gray plane at 2.752 AU) spreads the drifting bodies in eccentricity and inclination. The distribution of simulated asteroids behind the resonance then corresponds to the observed positions of the Merxia family members.