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by: Ms. Adrian Buckridge


Marketplace > University of Florida > Astronomy > AST 1002 > DISCOVER THE UNIVERSE
Ms. Adrian Buckridge
GPA 3.72


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Class Notes
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This 2 page Class Notes was uploaded by Ms. Adrian Buckridge on Friday September 18, 2015. The Class Notes belongs to AST 1002 at University of Florida taught by Staff in Fall. Since its upload, it has received 23 views. For similar materials see /class/206979/ast-1002-university-of-florida in Astronomy at University of Florida.

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Date Created: 09/18/15
General Properties of Stars Question What are the properties of the average star Is the sun as typical as everyone says The answer requires measurements of several kinds and measurements of large numbers of stars Comparison of Intrinsic Properties Luminosity 7 Energy output of stars Size Mass Temperature which we have discussed earlier Other parameters of interest which we will consider later are Composition Abundances of the elements Age and Evolution Luminosity Observed brightness vs distance Inverse square law I x Measurement of distance Parallax and the parsec Ups 2 l is the observed brightness of the star we measure the distance D and we can therefore obtain the intrinsic brightness the luminosity from the inverse square law above Temperature Wien s Law Color Spectrum Spectral Classes OBAFGKM hottest to coolest Atoms ions energy levels and the spectral classes Temperature As we discussed in an earlier chapter knowledge about the physical conditions within a star temperature and density allows us to determine Composition We nd that Composition is essentially the same for all normal stars stars on the mainsequence The H R Diagram Put it all together Compare Luminosity with Temperature Normal Stars The main sequence A temperature sequence NOT a composition sequence 1 October 23 2003 Abnormal Stars Red Giants White Dwarfs Star Sizes Direct measurement 7 only a few available Indirect measurement Stefan s Law energy radiated per second of time per unit of area on the surface of the star E 0 391 Luminosity L x l li 2 The luminosityradiustemperature relation Most stars are smaller cooler and less massive than the sun Spectroscopic Parallax Using the HR Diagram to determine large distances The Mass of Stars Gravity and Kepler s Third Law Ml Mg 2 where a is the size of the orbit Visual Binaries The Orbit The period Spectroscopic Binaries The Velocities The Period Eclipsing Binaries The Light Curve The Period Eclipsing Spectroscopic Binaries The Period the Velocities the Orbit the Stellar Sizes In particular this class of binary stars provides us with The MassLuminosityRadius relations Size of stars MassRadius li Luminosity of stars MassLuminosity L x M The HR Diagram Revisited The MainSequence and the importance of Mass MASS is the single most important parameter in determining the properties of a star Mass determines the location of the star on the main sequence of the H R diagram its temperature luminosity and size and the rate of evolutionary change Conclude What is an average star Abundances of stars A census The nearest stars numerous and faint The brightest stars few in number and seen over large distances Thus the typical star is very faint compared to the sun on average about l X 10419 and therefore very small and under massive The sun is brighter and therefore larger and more massive than about 96 of the stars in the galactic neighborhood of the sun the local volume of space 2 October 23 2003


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