1. The Origin of Modern Astronomy Chapter 4:

2. Isaac Newton 1689

3. Geo- synchronous Orbits: If the period of a satellite’s orbit is exactly 24 hours, the satellite can always remain over the same point on the Earth’s surface.

4. The Tides Caused by the difference of the Moon’s gravitational attraction on the water on Earth → 2 tidal maxima Excess gravity pulls water towards the moon on the near side. Forces are balanced at the center of the Earth. → 12-hour cycle Excess centrifugal force pushes water away from the moon on the far side.

5. Spring and Neap Tides The Sun is also producing tidal effects, about half as strong as the Moon. Near Full and New Moon, those two effects add up to cause spring tides. Near first and third quarter, the two effects work at a right angle, causing neap tides. Spring tides Neap tides

6. Acceleration of the Moon’s Orbital Motion Earth’s tidal bulges are slightly tilted in the direction of Earth’s rotation. Gravitational force pulls the moon slightly forward along its orbit.

7. Light and Telescopes Chapter 5

8. Astronomical Telescopes Primary objective: to gather large amounts of light. => Large Telescopes! The southern Gemini Telescope in Chile has a mirror with a diameter of 8.1 m (26.5 ft)! Other forms of radiation (other than visible light) can also be observed, but very different telescope designs are needed.

9. Radiation: Information from Space The Electromagnetic Spectrum In astronomy, we cannot perform experiments with our objects (stars, galaxies, …). The only way to investigate them, is by analyzing the light (and other radiation) which we observe from them.

10. Light as a Wave (I) Light waves are characterized by a wavelength and a frequency f. f = c/ c = 300,000 km/s = 3*10 8 m/s f and are related through

11. Wavelengths and Colors Different colors of visible light correspond to different wavelengths.

12. Light as a Wave (II) Wavelengths of light are measured in units of nanometers (nm) or Ångström (Å): 1 nm = 10 -9 m 1 Å = 10 -10 m = 0.1 nm Visible light has wavelengths between 4000 Å and 7000 Å (= 400 – 700 nm).

13. Light as Particles Light can also appear as particles, called photons (explains, e.g., photoelectric effect). A photon has a specific energy E, proportional to the frequency f: E = h*f h = 6.626x10 -34 J*s is the Planck constant. The energy of a photon does not depend on the intensity of the light!!!

14. The Electromagnetic Spectrum Need satellites to observe Wavelength Frequency High flying air planes or satellites

15. Refracting / Reflecting Telescopes Refracting Telescope: Lens focuses light onto the focal plane Reflecting Telescope: Concave Mirror focuses light onto the focal plane Almost all modern telescopes are reflecting telescopes. Focal length

16. The Focal Length Focal length = distance from the center of the lens to the plane onto which parallel light is focused.

17. Secondary Optics In reflecting telescopes: Secondary mirror, to re- direct light path towards back or side of incoming light path. Eyepiece: To view and enlarge the small image produced in the focal plane of the primary optics.

18. Disadvantages of refracting telescopes Chromatic aberration: Different wavelengths are focused at different focal lengths (prism effect). Can be corrected, but not eliminated by second lens out of different material. Difficult and expensive to produce: All surfaces must be perfectly shaped; glass must be flawless; lens can only be supported at the edges.

19. The Powers of a Telescope: Size does matter! 1. Light-gathering power: Depends on the surface area A of the primary lens / mirror, proportional to diameter squared: A =  (D/2) 2 D

20. The Powers of a Telescope (II) 2. Resolving power: Wave nature of light => The telescope aperture produces fringe rings that set a limit to the resolution of the telescope.  min = 1.22 ( /D) Resolving power = minimum angular distance  min between two objects that can be separated. For optical wavelengths, this gives  min = 11.6 arcsec / D[cm]  min

21. Seeing Weather conditions and turbulence in the atmosphere set further limits to the quality of astronomical images. Bad seeingGood seeing

22. The Powers of a Telescope (III) 3. Magnifying Power = ability of the telescope to make the image appear bigger. The magnification depends on the ratio of focal lengths of the primary mirror/lens (F o ) and the eyepiece (F e ): M = F o /F e A larger magnification does not improve the resolving power of the telescope!

23. The Best Location for a Telescope Far away from civilization – to avoid light pollution

24. The Best Location for a Telescope (II) On high mountain-tops – to avoid atmospheric turbulence (→ seeing) and other weather effects Paranal Observatory (ESO), Chile

25. Infrared Telescopes Most infrared radiation is absorbed in the lower atmosphere. However, from high mountain tops or high-flying air planes, some infrared radiation can still be observed. NASA infrared telescope on Mauna Kea, Hawaii

26. Infrared Telescopes Infrared observations can also be performed form high-flying aircraft. Infrared detectors must be cooled to very low temperatures.

27. Traditional Telescopes (I) Secondary mirror Traditional primary mirror: sturdy, heavy to avoid distortions.

28. Traditional Telescopes The 4-m Mayall Telescope at Kitt Peak National Observatory (Arizona)