Week 3 in Class Notes
Week 3 in Class Notes ASTR 101
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This 2 page Class Notes was uploaded by Evan Kirkpatrick on Sunday October 18, 2015. The Class Notes belongs to ASTR 101 at University of Washington taught by Ana Larson in Fall 2015. Since its upload, it has received 47 views. For similar materials see ASTRONOMY (NW,QSR) in Environmental Science at University of Washington.
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Date Created: 10/18/15
Week 3 in Class Notes wwwastrowashingtoneduundergradastroclub Electromagnetic Radiation Oscillation of electric and magnetic elds Propagates through space and some materials 0 Produced by blackbody radiation thermal 0 Emission as electrons lose energy in an atom o Electrons spiraling in a magnetic eld Continuous Spectrum Created by thermal Radiator blackbody radiation Hotter stars look more bluewhite than cooler stars because hot stars emit most of their light at shorter wavelengths Wien s Law Temperature in Kelvin and Wavelength in nm Wavelength peak 29E6T T 29E6Wavelength Peak Energy Gravitational Potential Energy 0 GPE mass x gravity x height Kinetic Energy 0 KE 12 mass x velocityquot2 Electrons jump energy levels If we see a certain light pattern emission from a star then we can tell what elements are on the star s surface We can tell what is in the atmosphere of a star by seeing which wavelengths of light are being absorbed Absorption and Emission Distinguish between emission and absorption spectra by what is happening with the electron in the atom Star Formation Interstellar Medium and Star Birth Rosette Nebula Emission nebula with new open cluster of about 2000 stars Dark Nebula dark section of a nebula of dust Re ection Nebula The glowing re ection in a nebula Infrared Telescopes allows us to see the stars because the dust doesn t absorb this light Massive stars form and push gas away which allows for other large stars to form in a continuing process to form star clusters Eagle Nebula We see pillars of dust in the infrared The light from this nebula takes 6000 years to get to Earth so it is thought that the pillars are currently not present Why do Stars Form Given enough time gas and dust in interstellar medium will gather together Any small region that is slightly cooler and denser it will start to collapse under gravity How They Form Gravity compresses star Gas heats up due to compression and conservation of energy Increase in temperature stalls contraction What Slows Contraction Interior of star heats and creates outward pressure Interior of star grows more dense Opacity of star s interior increases Radiation struggles to get out Gravity keeps compressing the star Center of the star gets hotter and hotter Protostar becomes fully convective Fusion begins in the core Collapse stops Equilibrium sets in Conservation of Angular Momentum As the protostar collapses it creates a disk of dust around it in order to conserve angular momentum Story Time Once upon a time there was a little girl named payal Payal didn t have any friends because she was a loner Then one day she died The end Once upon a time there was a little boy named Evan Everyone loved him cuz he was awesome He was just the best person that ever existed The end Once upon a time there was a little boy named lvanoh wait maybe it was Miles Payal never remembered because she was so mean The end Once upon a time there was a little boy named Zac The end