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Yarkovsky effect and the dynamics of the Solar System

PhD Thesis

Miroslav Broz

supervisor: David Vokrouhlicky

Table of contents:
  1. An electronic version of the Thesis
  2. Supplementary material: Figures (in EPS and PNG formats)
  3. Supplementary material: Animations (with descriptions)
  4. Supplementary material: Tables
The Yarkovsky/YORP effect

1. An electronic version of the Thesis

yarkovsky_effect_phdth_broz.pdf [PDF, 37 MB]   Get Adobe Reader
yarkovsky_effect_phdth_broz.ps.gz [Gzipped PostScript, 22 MB]

yarkovsky_effect_phdth_broz_abstract.pdf [PDF, 1.2 MB]
yarkovsky_effect_phdth_broz_abstract.ps.gz [Gzipped PostScript, 1.7 MB]
yarkovsky_effect_phdth_broz_defence.pdf [PDF, slides 800×600 pxl, 1.5 MB]

phdth_200606291437.tar.gz [TeX source, 240 kB]
autoreferat_200606291438.tar.gz [TeX source, 20 kB]

The thesis was defended on Jun 28th 2006. This version was last updated on Jun 29th 2006.

2. Supplementary material: Figures (in EPS and PNG formats)

Figure 1 Figure 2 Figure 3a Figure 3b Figure 3c Figure 3d Figure 3e Figure 3f Figure 3g Figure 3h Figure 3i Figure 4a Figure 4b Figure 5 Figure 6 Figure 7 Figure 8 Figure 9a Figure 9b Figure 10 Figure 11a Figure 11b Figure 12 Figure 13 Figure 14 Figure 15 Figure 16 Figure 17a Figure 17b Figure 18 Figure 19 Figure 20 Figure 21 Figure 22a Figure 22b Figure 23 Figure 24 Figure 25 Figure 26 Figure 27 Figure 28 Figure 29 Figure 30 Figure 31a Figure 31b Figure 32a Figure 32b Figure 32c Figure 32d Figure 32e Figure 32f Figure 32g Figure 32h Figure 32i Figure 32j Figure 33a Figure 33b Figure 33c Figure 33d Figure 33e Figure 33f Figure 34 Figure 35 Figure 36a Figure 36b Figure 37a Figure 37b Figure 37c Figure 37d Figure 37e Figure 37f Figure 37g Figure 38a Figure 38b Figure 39a Figure 39b Figure 40 Figure 41a Figure 41b Figure 42 Figure 43 Figure 44 Figure 45 Figure 46 Figure 47 Figure 48 Figure 49 Figure 50a Figure 50b Figure 51a Figure 51b Figure 51c Figure 51d Figure 51e Figure 52 Figure 53a Figure 53b Figure 54a Figure 54b Figure 54c Figure 55 Figure 56 Figure 57a Figure 57b Figure 58a Figure 58b Figure 59 Figure 60a Figure 60b Figure 61a Figure 61b Figure 62 Figure 63 Figure 64 Figure 65 Figure 66 Figure 67 Figure 68 Figure 69a Figure 69b Figure 69c Figure 69d Figure 70 Figure 71 Figure 72 Figure 73 Figure 74 Figure 75a Figure 75b Figure 76a Figure 76b Figure 77a Figure 77b Figure 78a Figure 78b Figure 79 Figure 80 Figure 81 Figure 82a Figure 82b Figure 82c Figure 83 Figure 84a Figure 84b Figure 84c Figure 85a Figure 85b Figure 86a Figure 86b Figure 87a Figure 87b Figure 88 Figure 89 Figure 90 Figure 91 Figure 92a Figure 92b Figure 92c Figure 92d Figure 93 Figure 94 Figure 95 Figure 96 Figure 97 Figure 98a Figure 98b Figure 98c Figure 98d Figure 98e Figure 98f Figure 99 Figure 100 Figure 101 Figure 102 Figure 103a Figure 103b Figure 103c Figure 103d Figure 104 Figure 105a Figure 105b Figure 106 Figure 107 Figure 108 Figure 109 Figure 110

Click to obtain hi-resolution figures. Figure captions are included in the PDF file above.

3. Supplementary material: Animations (with descriptions)

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.

  1. 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.


  2. 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.


  3. 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.


  4. 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.


  5. 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.


  6. 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.


  7. 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.


  8. 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.


  9. 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.


4. Supplementary material: Tables

  1. List of asteroids in the 2/1 mean motion resonance with Jupiter

Last updated Apr 20th 2006, Miroslav Broz (miroslav.broz@email.cz).