Astronomy 101 week 4 notes
Astronomy 101 week 4 notes ASTR 101
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This 2 page Class Notes was uploaded by Breanab on Saturday January 23, 2016. The Class Notes belongs to ASTR 101 at University of New Mexico taught by Trace Tessier in Spring 2016. Since its upload, it has received 13 views. For similar materials see Introduction to Astronomy in Astronomy at University of New Mexico.
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Date Created: 01/23/16
Lecture 4 Notes Review • What is constant for all forms of EM radiation in a vacuum? o The speed • What is not a property of a blackbody? o It appears black, regardless of its temperature • What are properties of a black body? o It emits radiation in a continuum of wavelengths o Its spectrum peaks at a wavelength determined by its temperature o The total energy that it radiates increases rapidly with temperature • The suns observed spectrum is? o Nearly a continuum with some absorption lines Spectrum of the sun • Complicated objects = many different elements • Nearly continuous absorption spectrum • Why emission lines? o Photon absorption/ atomic collisions excite atoms o Electron drops back to lower level o Photons at specific frequencies emitted • Why absorption lines? o Gas clouds block specific photons and prevent specific light from being seen Stellar spectra • See lecture 6 slide review • How does the pitch or tome of a sound wave change when the source of the sound is moving towards or away from you? o The sound waves are more concentrated the closer they are to you creating a higher pitch, and when less concentrated created a lower pitch. • What about when you are moving towards or away from the source? o It would be the same, you receive each frequency more quickly the closer you get to the source of the waves with the opposite affect as you move away • Does this affect occur for all types of waves or just for sound waves? o This happens for all waves The frequency or wavelength of a wave depends on the relative motion of the source and the observer. Doppler shifted atomic spectra • Why don’t we see the color of everyday objects change as they move? o There isn’t enough difference in the color to be able to tell unless you spread out the spectra to see the emission lines and compare them • Redshift is farther away • Blueshift is closer It is possible to use spectra to find planets around other stars by finding a wobble in the stars from the pull in their orbit Star wobbling causes Doppler shift of its absorption lines, it only gives information about velocity along line of sight
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