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: 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: 2This lecture outlines the Spectroscopic Method and gives a detailed explanation of the emission and absorption of photos by atoms.
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Pages: 2Spectroscopy and two of the Kirchoff's Laws are introduced in today's lecture. While examining the properties of light, students are able to better understand the laws surrounding its place in the spectrum.
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Pages: 2All objects absorb and emit EM radiation. Black Body Curves are introduced and Temperature Scales are explained in this lecture.
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Pages: 2In this lecture, we are introduced to the structure and properties of a wave, as well as several basic formulas that relate the speed of a wavelength to frequency. Colors of visible light and spectra, as well as properties of photons, are defined.
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Pages: 2Astronomy and astrology are often terms that are confused because they sound so alike. In reality, however, they mean two very different things. This important difference leads to today's discussion about light and matter. Students also learn how to use the scientific method.