1. The Nature of Light In Astronomy II

3. The Earth’s atmosphere absorbs most of EM spectrum, including all UV, X ray, gamma ray and most infrared. We have to build telescopes for these wavelengths in space. Only radio and visible light can get complete through the atmosphere.

4. How does light tell us the temperatures of planets and stars?

5. Thermal Radiation (blackbody radiation) Nearly all large or dense objects emit thermal radiation, including stars, planets, and you. An object’s thermal radiation spectrum is called a blackbody spectrum and only depends one property: its temperature. A Blackbody spectrum is an example of a continuous spectrum. The terms blackbody radiation and thermal radiation are equivalent and used interchangeably.

6. Properties of Thermal Radiation 1.Hotter objects emit more light at all frequencies per unit area. 2.Hotter objects emit photons with a higher average energy.

7. Wien’s Law

8. peak = b/T b is a constant = 2.9 (cm/K) T is the temperature in Kelvin. peak is the wavelength in centimeters of the peak of the BB curve. When we see a hot object we will see it at the color of its peak wavelength since this is the wavelength that is strongest. A large object and a small object at the same temperature have the same shape and peak of their blackbody curve, but the larger object emits more total energy.

9. Thought Question Which is hottest? A.A blue star B.A red star C.A planet that emits only infrared light

10. Thought Question Why don’t we glow in the dark? A.People do not emit any kind of light. B.People only emit light that is invisible to our eyes. C.People are too small to emit enough light for us to see. D.People do not contain enough radioactive material.

11. Interpreting an Actual Spectrum By carefully studying the features in a spectrum, we can learn a great deal about the object that created it.

12. What is this object? Reflected sunlight: Continuous spectrum of visible light is like the Sun’s except that some of the blue light has been absorbed—the object must look red.

13. What is this object? Thermal radiation: Infrared spectrum peaks at a wavelength corresponding to a temperature of 225 K.

14. What is this object? Carbon dioxide: Absorption lines are the fingerprint of CO 2 in the atmosphere.

15. What is this object? Ultraviolet emission lines: Indicate a hot upper atmosphere

16. What is this object? Mars!

17. How does light tell us the speed of a distant object? The Doppler Effect

18. Hearing the Doppler Effect as a Car Passes

19. Measuring the Shift We generally measure the Doppler effect from shifts in the wavelengths of spectral lines. Stationary Moving Away Away Faster Moving Toward Toward Faster

20. Doppler shift tells us ONLY about the part of an object’s motion toward or away from us.

21. Thought Question A.It is moving away from me. B.It is moving toward me. C.It has unusually long spectral lines. I measure a line in the lab at 500.7 nm. The same line in a star has wavelength 502.8 nm. What can I say about this star?

22. Measuring Redshift The Doppler Shift of an Emission Line Spectrum

23. Measuring Redshift Doppler Shift of Absorption Lines

24. Now work on the lecture tutorial sections. –Blackbody Radiation, page 57 onwards. –Doppler shift, page 73 onwards.