Chaos in Astronomy: Conference 2007 by G. Contopoulos (auth.), G. Contopoulos, P. A. Patsis (eds.)

By G. Contopoulos (auth.), G. Contopoulos, P. A. Patsis (eds.)

The convention "Chaos in Astronomy" used to be held in Athens on 17-20 Sep 2007. overseas leaders within the box addressed the themes

  • Chaos in huge N-body structures and in galactic dynamics
  • Chaos in sun approach dynamics
  • Statistical mechanics of platforms with normal and chaotic orbits
  • Chaos within the formation of large-scale constitution within the Universe
  • Fundamental options, equipment and instruments.

The publication comprises conscientiously edited refereed contributions. It serves as a connection with researchers and may supply an summary to scholars and beginners getting into any box of dynamical astronomy.

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Patsis, P. A. , Patsis, P. , & Pompei, E. 2004, A&A, 423, 849 Hohl, F. 1971, ApJ, 168, 343 Kaufmann, D. E. & Contopoulos, G. 1996, A&A, 309, 381 Lin, C. C. & Shu, F. H. , & Dickinson, M. 1998, ApJ, 498, 106 Merrifield, M. R. & Kuijken, K. 1995, MNRAS, 274, 933 Patsis, P. A. , Gordon, K. , Witt, A. , & Madsen, G. J. 2004, ApJ, 617, 1022 Roberts, W. W. 1969, ApJ, 158, 123 Sandage, A. & Tammann, G. A. 1981, A Revised Shapley–Ames Catalog of Bright Galaxies, Carnegie Inst. of Wash. Publ. No. ) Schwarzschild, M.

387, 1264. 41. Voglis, N. (2003), Mon. Not. R. Astron. Soc. 344, 575. 42. , Stavropoulos, I. and Kalapotharakos, C. (2006), Mon. Not. R. Astron. Soc. 372, 901. 43. , Tsoutsis, P. and Efthymiopoulos, C. (2006), Mon. Not. R. Astron. Soc. 373, 280. 44. , Harsoula, M. and Contopoulos, G. (2007), Mon. Not. R. Astron. Soc. 381, 757. Order and Chaos in Spiral Galaxies Seen through their Morphology P. org Summary. It is clear from dynamical considerations and N-body models that both order and chaos are important for spiral galaxies.

Artificial bar structures) and may bias the analysis. Population effects and attenuation by dust make it difficult to compare images taken in visual bands with models especially for late-type spirals with significant star formation. This is illustrated in Fig. 1 which shows B- and Kband images of NGC 5085. It is more difficult to trace the spiral arms on the B-band image due to the heavy dust absorption in them and their inner parts appear very different due to the strong dust lanes which reach all the way into the bulge region.

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