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Towson - ASTR 161 - Astr Study Guide 2.2 - Study Guide

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Towson - ASTR 161 - Astr Study Guide 2.2 - Study Guide

School: Towson University
Department: Astronomy
Course: General Astronomy I
Professor: Christian Ready
Term: Fall 2016
Tags:
Name: Astr Study Guide 2.2
Description: Half of the study guide filled out.
Uploaded: 11/14/2016
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background image 5.1: Anatomy of Light
­ wavelength and frequency are inversely proportional ­ shorter wavelength = higher frequency 
& energy / longer wavelength = lower frequency & energy
electromagnetic spectrum (from shorter wavelength / higher frequency to longer wavelength / 
lower frequency) ­ gamma ray, x ray, uv ray, visible light, infrared waves, microwaves, radio 
waves
all of electromagnetic spectrum travels at the same speed of light
measured in Angstroms 
light is both like a wave and a particle, but is neither
5.2: The Quantum Nature of Light and Matter
­ understand how an atom is structured, and the Bohr model of hydrogen in particular
­ the relationship between electrons and photons
­ what happens when electrons in an atom absorb or release energy, and how that is 
represented in a spectrum
­ Kirchoff's laws ­ what conditions produce different kinds of spectra?
5.3: Light & Motion
­ what is the doppler effect, and what it means for the light coming from an approaching object
­ what the doppler effect tells us how light from a receding object
­ radial velocity, and how it relates to the doppler effect
­ how radial velocity affects the amount of blueshift and redshift
­ how radial velocity is measured relative to the amount of blueshift and redshift
5.4: Light & Temperature
­ understand what we mean by a "blackbody", and the sort of real­life things that radiate like 
blackbodies
­ what a Planck or Blackbody curve is, and how Wein's Law works
­ the relationship of Luminosity to Temperature and Radius (Stefan­Boltzmann Law or "star 
equation")
­ the difference between luminosity and brightness
­ how the inverse square law determines how bright a luminous star appears at a given distance
6.1: Telescope
refracting telescope ­ objective lens is convex and bends light along the edge. aperture is the 
diameter of the objective, which gathers more light than the eye can. image appears inverted. 
minimum light is used because light is lost when more glass is added
shorter focal length gives wider field of view but smaller images / longer focal length gives larger
images but less field of view
chromatic aberration ­ color becomes skewed because R G & B light bbd differently. to fix, add 
concave glass. unique to refracting telescope
background image reflecting telescope ­ uses a mirror to capture images
cheaper, no chromatic aberration
diffraction ­ any wave that bends in a way other than reflection or refraction. inversely 
proportional to wavelength. smaller opening, greater diffraction
diffraction limit ­ best resolution in a telescope before diffraction occurs
angular resolution ­ smallest angle that can be achieved with a given aperture
single mirror design ­ modern manufacturing allows for light mirrors. can only be so big before 
mirror sinks under its own weight
binocular telescope ­ 2 giant telescopes get more image than one and combine to make one 
large image
adaptive optics ­ adjusts hexagon mirrors to accommodate disturbances in atmosphere. can be 
extremely large. 
­ observatories are typically in higher locations away from water, such as mountain tops, to get 
as close to space as possible and to minimize atmospheric distortion. 
­ atmospheric distortion ­ light passes through atmosphere and hits bubbles of warm or cold air, 
distorting the image. is why stars seem to twinkle
13.1: Star Distances
­ how distance is determined via parallax
­ the relationship between a star's distance and the parallactic angle
­ the relationship between a star's apparent brightness, distance, and luminosity
­ the difference between a star's apparent magnitude and absolute magnitude
­ how the inverse square law determines how bright a luminous star appears at a given distance
13.2: Stars' Luminosity, Temperature, & Distance
­ what color index is, and how it indicates a star's temperature
­ how a star's temperature and radius affects a star's luminosity
­ the different spectral types and how they rank in terms of temperature from hottest to coolest
13.3: The Hertzsprung­Russell Diagram
­ how to read the diagram, what it plots
­ the different regions of the H­R diagram, and what kinds of stars are plotted there
­ the relationship between a star's location on the H­R diagram (its temperature and luminosity) 
and its radius
­ how stars with the same temperature can have different radii and spectral type
­ what a star's luminosity class represents, and what the different classes represent for stars of 
a given spectral type
­ how spectroscopic parallax works and how a star's distance can be determined from its 
apparent and absolute magnitudes
­ the relationship between a main­sequence star's mass and its luminosity, temperature, size 
(radius), & lifetime

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School: Towson University
Department: Astronomy
Course: General Astronomy I
Professor: Christian Ready
Term: Fall 2016
Tags:
Name: Astr Study Guide 2.2
Description: Half of the study guide filled out.
Uploaded: 11/14/2016
3 Pages 37 Views 29 Unlocks
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  • 24/7 Homework help
  • Notes, Study Guides, Flashcards + More!
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