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Quiz 2 Lecture 12
Quiz 2 Lecture 12

... d. none of these choices. Astronomers don't know why galaxies form and evolve the way they do. answer: b ...
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... NGC 3603 is shown at the right in Fig. 2. We overlayed the theoretical isochrones of pre-main sequence stars from Palla & Stahler (1999) down to 0.1M . We assumed a distance modulus of (m − M )o = 13.9 based on the distance of 6 kpc (De Pree et al. 1999) and an average foreground extinction of AV = ...
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Solar-like oscillations in intermediate red giants
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Space and Time: From Antiquity to Einstein and Beyond

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The Pennsylvanian Period in Alabama: Looking Up Astronomy and

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Chapter 8: The Pennsylvanian Period in Alabama: Looking Up
Chapter 8: The Pennsylvanian Period in Alabama: Looking Up

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High resolution spectroscopy: what`s next?

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... into the interstellar medium. Eventually the white dwarf remains as the stellar core end product. If the white dwarf is in a multiple star system and a companion star evolves into a red giant then the white dwarf might not be the final product – it could accrete enough materials from the red giant t ...
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Between the Stars: Gas and Dust in Space

... Reflection Nebulae Some dense clouds of dust are close to luminous stars and scatter enough starlight to become visible Such a cloud is called a reflection nebula because the light that we see from it is starlight reflected off grains of dust Since dust grains are tiny, they scatter light with blue ...
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How to Plot the H-R Diagram and Use its Applications

... and die sooner. Jrmtryn full of stars for several million years bring. Those with less mass, they can shine up to tens of billion years. Interstellar matter: the distance between stars in each galaxy, interstellar medium is filled with a gas containing mainly hydrogen and helium, a small amount of o ...
WSN 42 (2016) 132-142
WSN 42 (2016) 132-142

... and die sooner. Jrmtryn full of stars for several million years bring. Those with less mass, they can shine up to tens of billion years. Interstellar matter: the distance between stars in each galaxy, interstellar medium is filled with a gas containing mainly hydrogen and helium, a small amount of o ...
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Stars - cayugascience

... explosion is directed not only outward, but also inward. This force causes the atoms in the star’s core to compress and collapse. When an atom collapses, it forms neutrons, particles that are at the centre of most atoms already. When the star’s core becomes little more than a ball of neutrons only a ...
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Future of an expanding universe

Observations suggest that the expansion of the universe will continue forever. If so, the universe will cool as it expands, eventually becoming too cold to sustain life. For this reason, this future scenario is popularly called the Big Freeze.If dark energy—represented by the cosmological constant, a constant energy density filling space homogeneously, or scalar fields, such as quintessence or moduli, dynamic quantities whose energy density can vary in time and space—accelerates the expansion of the universe, then the space between clusters of galaxies will grow at an increasing rate. Redshift will stretch ancient, incoming photons (even gamma rays) to undetectably long wavelengths and low energies. Stars are expected to form normally for 1012 to 1014 (1–100 trillion) years, but eventually the supply of gas needed for star formation will be exhausted. And as existing stars run out of fuel and cease to shine, the universe will slowly and inexorably grow darker, one star at a time. According to theories that predict proton decay, the stellar remnants left behind will disappear, leaving behind only black holes, which themselves eventually disappear as they emit Hawking radiation. Ultimately, if the universe reaches a state in which the temperature approaches a uniform value, no further work will be possible, resulting in a final heat death of the universe.
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