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Quantum effects in astrophysics
Quantum effects in astrophysics

... Although the spectral nature of light can be seen in a rainbow, it was not until 1666 that Newton showed that the white light from the sun could be dispersed into a continuous series of colors. Newton introduced the word "spectrum" to describe this phenomenon. (The word spectrum is from the Latin fo ...
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... The average human is made up of 100 thousand billion cells, according to some estimates. This means that there are approximately 125 billion miles of DNA in a human body – corresponding to 70 round-trips between Saturn and the Sun. You could travel your entire life in a Boeing 747 flying at top spee ...
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... amount of energy that is produced by a combination of He burning in the core and H burning in the shell. It ends when the core has been entirely transformed into C and O. B. Stars 1 − 1.8 M For stars from 1 − 1.8 M , the helium core becomes degenerate before it violates the Schönberg-Chandrasekha ...
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...  H-R diagrams are useful because they help astronomers categorize stars into groups:  Main sequence stars, like the Sun, are in a very stable part of their life cycle.  White dwarfs are hot and dim and cannot be seen without a telescope.  Red giants are cool and bright and some can be seen witho ...
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Participant Handout - Math Machines Home

... intense but short-lived source of additional energy for the star, enough to make it expand and become a red giant. After all their usable fuel is exhausted, stars blow off their outer layers and leave behind a small, hard-to-see remnant. Massive stars (perhaps including Betelgeuse) blow off their ou ...
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NuSeti-2015 - Department of Physics and Astronomy

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... Dead Core Evolution • They are not massive enough to compress the C core to T > 7 x 108 K at which it could fuse, so these CSPN's just cool off and fade in power, slowly shrinking in size • BUT, when density of the core reaches 106 g/cm3 (or one ton / teaspoon!) the PAULI EXCLUSION PRINCIPLE takes ...
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... swarm of stars orbiting around the center of the Milky Way Galaxy. (Other galaxies have globular Clusters too). Stars in globular clusters are extremely old. They may have been the first parts of the galaxy to form (Billions of years old). We find the age of the cluster by noting which stars have ha ...
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Overview of Astronomy 150

Slide 1
Slide 1

< 1 ... 47 48 49 50 51 52 53 54 55 ... 153 >

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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