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LECTURE 6, SEPTEMBER 9, 2010

LECTURE 6, SEPTEMBER 9, 2010. ASTR 101, SECTION 3 INSTRUCTOR, JACK BRANDT jcbrandt@unm.edu. Question 6. a) depend on its temperature. b) are identical to its absorption lines. c) depend on its density. d) are different than its absorption lines. e) depend on its intensity.

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LECTURE 6, SEPTEMBER 9, 2010

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  1. LECTURE 6, SEPTEMBER 9, 2010 ASTR 101, SECTION 3 INSTRUCTOR, JACK BRANDT jcbrandt@unm.edu ASTR 101-3, FALL 2010

  2. ASTR 101-3, FALL 2010

  3. ASTR 101-3, FALL 2010

  4. ASTR 101-3, FALL 2010

  5. ASTR 101-3, FALL 2010

  6. ASTR 101-3, FALL 2010

  7. ASTR 101-3, FALL 2010

  8. Question 6 a) depend on its temperature. b) are identical to its absorption lines. c) depend on its density. d) are different than its absorption lines. e) depend on its intensity. The wavelengths of emission lines produced by an element

  9. Question 6 a) depend on its temperature. b) are identical to its absorption lines. c) depend on its density. d) are different than its absorption lines. e) depend on its intensity. The wavelengths of emission lines produced by an element Elements absorb or emit the same wavelengths of light based on their electron energy levels.

  10. ASTR 101-3, FALL 2010

  11. ASTR 101-3, FALL 2010

  12. PHOTON-1 (See Page 59) • Photons are packets of electromagnetic radiation (Einstein 1905) • Each photon has a specific energy such that: (photon energy) is proportional to the (frequency) • A red-light photon has a frequency of 4 x 1014 Hz (or a wavelength of 750 nm) ASTR 101-3, FALL 2010

  13. PHOTON-2 (See Page 59) • A blue-light photon has a frequency of 7 x 1014 Hz (or a wavelength of 430 nm) • So, the red photon has 4/7 the energy of the blue photon • The energy of photons in the electromagnetic spectrum increases with increasing frequency and decreases with increasing wavelength ASTR 101-3, FALL 2010

  14. PHOTON-3 (See Page 60) • REMEMBER: LIGHT IS LIGHT ! ASTR 101-3, FALL 2010

  15. ASTR 101-3, FALL 2010

  16. ASTR 101-3, FALL 2010

  17. ASTR 101-3, FALL 2010

  18. ASTROMONICAL SPECTROSC0PY-1 • COMPOSITION • ABUNDANCES • TEMPERATURE (WIEN’S LAW, BLACKBODY, OR OTHER • PRESSURE (BROADENS LINES) ASTR 101-3, FALL 2010

  19. ASTRONOMICAL SPECTROSCOPY-2 • ROTATION (DOPPLER EFFECT) • MAGNETIC FIELD (ZEEMAN EFFECT) • ELECTRIC FIELD (STARK EFFECT) • DOPPLER EFFECT, MOTION TOWARD OR AWAY FROM THE OBSERVER ASTR 101-3, FALL 2010

  20. ASTR 101-3, FALL 2010

  21. ASTR 101-3, FALL 2010

  22. Question 5 a) its spectral lines are redshifted. b) the light is much brighter. c) its spectral lines are shorter in wavelength. d) the amplitude of its waves has increased. e) its photons have increased in speed. If a light source is approaching you, you will observe

  23. Question 5 a) its spectral lines are redshifted. b) the light is much brighter. c) its spectral lines are shorter in wavelength. d) the amplitude of its waves has increased. e) its photons have increased in speed. If a light source is approaching you, you will observe The Doppler Shift explains that wavelengths from sources approaching us are blueshifted.

  24. Question 7 a) its composition. b) its surface temperature. c) its transverse (side-to-side) motion. d) its rotation. e) its density. Analyzing a star’s spectral lines can tell us about all of these EXCEPT

  25. Question 7 a) its composition. b) its surface temperature. c) its transverse (side-to-side) motion. d) its rotation. e) its density. Analyzing a star’s spectral lines can tell us about all of these EXCEPT Only motion toward or away from us influences a star’s spectral lines. Spectra can also tell us about a star’s magnetic field.

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