1st Edition
AST-A 105: Stars and Galaxies
School: Indiana University, Bloomington (IUB )
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Pages: 2The Extragalactic Distance Scale uses standard candles and applies the inverse square law to find galaxy distances.
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Pages: 2Galaxy Collisions take place when galaxy mergers combine to form small groups of galaxies in space.
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Pages: 3In this lecture, a historical understanding of galaxies, as well as the basic types of galaxies, are outlined.
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Pages: 2In this outline, we finish learning about dark matter, globular clusters, and cluster evolution as it takes place in the Milky Way Galaxy.
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Pages: 3This outline continues exploring the details and workings of our Milky Way Galaxy.
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Pages: 2Our very own planet Earth is located in the Milky Way Galaxy.
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Pages: 2A black hole is an object with such strong gravity that nothing can escape from its vicinity- not even light.
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Pages: 2This outline describes Star Clusters and the Equinoxes.
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Pages: 2This outline explains in great detail the process of evolution for a main sequence star.
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Pages: 2As stars go through their life cycle, they follow the evolutionary track to perform Stellar Evolution.
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Pages: 2Stellar Evolution is explained in detail as stars form from cold, dense interstellar clouds.
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Pages: 2This is the Study Guide for Exam 2, covering the information on stars, luminosity, and the Sun that we have been taught thus far.
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Pages: 2The various and unique temperatures of a star are what determines its color and stellar spectra.
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Pages: 2A star is a fixed luminous point in the night sky that is a large, remote incandescent body like the Sun. Luminosity is an intrinsic property of every star.
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Pages: 2A Solar Neutrino is a very low mass, neutral particle that travels near the speed of light.
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Pages: 2In this lecture, we explore the various solar activities that take place on the surface of the Sun, such as sunspots, solar cycles, and solar storms.
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Pages: 2In this lecture, we explore the inner structure of the Sun's photosphere, chromosphere, transition zone and corona.
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Pages: 2Nuclear fusion is the process of generating energy to power the Sun. This process, combined with Hydrogen Fusion, will keep the Sun burning for another 5 billion years.
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Pages: 4Study Guide covering the most important of materials for Exam 1 from Lectures 1-6 of this class.
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Pages: 2This lecture outlines the Spectroscopic Method and gives a detailed explanation of the emission and absorption of photos by atoms.