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by: Breanab

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Astronomy 101 week 3 notes ASTR 101

Marketplace > University of New Mexico > Astronomy > ASTR 101 > Astronomy 101 week 3 notes
Breanab
UNM
GPA 4.1

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COURSE
Introduction to Astronomy
PROF.
Trace Tessier
TYPE
Class Notes
PAGES
2
WORDS
CONCEPTS
astronomy
KARMA
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This 2 page Class Notes was uploaded by Breanab on Friday January 8, 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: 01/08/16
Lecture 3 notes Spectroscopy and Atoms • How do you make a spectrum? o By refraction of light § When you bend light, bending angle depends on wavelength, or color. • What does the spectrum of an astronomical objects radiation look like? o Many objects like stars have roughly a “black-body” spectrum also known as the Planck spectrum or planck curve. (plotting the electromagnetic radiation)(brightness vs frequency graph) • How is temperature related to the amount of energy radiated? o As the frequency goes up the temperature is going up as well o The wavelength of peak emission tells us the temperature of the object o Temperature scale of molecules mimics the black body graph and correlates with the color • How is temperature related to the color of the object? o As the temperature goes up the color goes from red to blue to white • Types of spectra o Continuous spectrum o Emission spectrum o Absorption spectrum § Pattern of lines is a fingerprint of the element § For a given element, emission and absorption lines occur at the same wavelengths Spectrum of the sun • Absorption spectrum • Helium was discovered in suns spectrum before being found on earth • What causes emission/absorption of light at specific wavelengths? o Photons carrying just enough energy for the interaction to occur • The particle Nature of light o Light interacts with matter as individual packets of energy, called photons o Photon energy is proportional to frequency o Ex. Ultraviolet photons are more harmful than visible photons • The nature of Atoms o The bohr model of the hydrogen atom – on slide lecture 5 o When an atom absorbs a photon, it moves to a higher energy state briefly o When it jumps back to lower energy state, it emits photon(s) in a random direction, conserving the total energy of the system • Other elements Each element has its own allowed energy levels yielding a unique spectral fingerprint

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