1 / 26

Spiral Galaxies

Spiral Galaxies. Elliptical Galaxies. Irregular Galaxies. Classification of Galaxies. Properties of Galaxies. Other galaxy types : Peculiar, Interacting, Ring, Starburst, Dwarf, Luminous Infrared, Active Nuclei, Damped Lyman-alpha. Stephan’s Quintet – Colliding galaxies.

yoshiko
Télécharger la présentation

Spiral Galaxies

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Spiral Galaxies

  2. Elliptical Galaxies

  3. Irregular Galaxies

  4. Classification of Galaxies

  5. Properties of Galaxies Other galaxy types : Peculiar, Interacting, Ring, Starburst, Dwarf, Luminous Infrared, Active Nuclei, Damped Lyman-alpha

  6. Stephan’s Quintet – Colliding galaxies

  7. The “Anntenae” Galaxies – a case study

  8. Galactic Train Wrecks

  9. Collisional Aftermath

  10. Ring Galaxies – the “splash” Head-on collisions can produce a “ripple” of star formation that expands outwards.

  11. Galactic Superwinds

  12. The Magellanic Clouds Southern Hemisphere only Large Magellanic Cloud Small Magellanic Cloud

  13. The Galactic Neighborhood

  14. The “Local Group” of Galaxies

  15. Members of the Local Group

  16. And outward…

  17. Galaxy Clusters Virgo Notice the giant ellipticals at the centers of many clusters. These are an example of “galactic cannibalism”. Coma

  18. Galactic Cannibals – Central CD Ellipticals At the heart of rich clusters, galaxies pass through the center and are disrupted and collected.

  19. Making a CD galaxy

  20. into the Universe…

  21. Large Scale Structure On the largest scales (100 million ly) the Universe takes on a “foamy” appearance, with great filaments and walls of galaxies and clusters, surrounding great “voids” that are relatively empty.

  22. Dark Matter - rotation curves Rotation curves imply the mass-to-light ratios of galaxies go up as we look on larger scales: Sun M/L=1, solar neighborhood  M/L=3, galaxy  M/L=50

  23. Dark Matter – cluster speeds galaxy clusters  M/L=200-500 From average speed of galaxies – the cluster would fly apart From X-ray gas held in – several million degrees and extensive

  24. What could the dark matter be? • Normal but dark matter (“baryonic”) : rocks, white or brown dwarfs? 2) Black holes or neutron stars? Too much metals would have been produced. Anyway, there is a fundamental reason from the Big Bang this can’t be it…

  25. Dark Matter :gravitational lensing The mass required to produce the observed lensing is much higher than the luminous mass. This is a direct observation of gravity due to dark matter.

  26. WIMPS and Cold Dark Matter Could dark matter be some kind of new particles which interact very weakly with matter (like neutrinos do) but massive, and not moving relativistically? Experiments at Berkeley and elsewhere are looking for them (guaranteed Nobel prize!).

More Related