https://prancer.physics.louisville.edu/astrowiki/index.php?title=Periodic_Table_of_the_Elements&feed=atom&action=historyPeriodic Table of the Elements - Revision history2024-03-29T14:06:41ZRevision history for this page on the wikiMediaWiki 1.38.2https://prancer.physics.louisville.edu/astrowiki/index.php?title=Periodic_Table_of_the_Elements&diff=859&oldid=prevWikiSysop: moved Period Table of the Elements to Periodic Table of the Elements2012-02-20T19:45:04Z<p>moved <a href="/astrowiki/index.php?title=Period_Table_of_the_Elements&action=edit&redlink=1" class="new" title="Period Table of the Elements (page does not exist)">Period Table of the Elements</a> to <a href="/astrowiki/index.php/Periodic_Table_of_the_Elements" title="Periodic Table of the Elements">Periodic Table of the Elements</a></p>
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</td></tr></table>WikiSysophttps://prancer.physics.louisville.edu/astrowiki/index.php?title=Periodic_Table_of_the_Elements&diff=807&oldid=prevWikiSysop at 09:58, 20 February 20122012-02-20T09:58:36Z<p></p>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Olivine ((Mg,Fe)<del style="font-weight: bold; text-decoration: none;">2SiO4</del>) would also form in the protoplanetary nebula. If a planet or asteroid is large enough, it forms layers differentiating different minerals, with heaviest elements, usually iron, in the center. In a powerful enough collision, the iron, with a lower melting point than olivine, melts around the fragments of olivine. Together they fly out making beautiful pallasites. It is possible to get an idea of the energy in an impact of this sort by the heat that is generated, which would be above the melting point of iron, 1535 C, but not so hot as to melt olivine,1760 C.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Olivine ((Mg,Fe)<ins style="font-weight: bold; text-decoration: none;"><sub>2</sub>SiO<sub>4</sub></ins>) would also form in the protoplanetary nebula. If a planet or asteroid is large enough, it forms layers differentiating different minerals, with heaviest elements, usually iron, in the center. In a powerful enough collision, the iron, with a lower melting point than olivine, melts around the fragments of olivine. Together they fly out making beautiful pallasites. It is possible to get an idea of the energy in an impact of this sort by the heat that is generated, which would be above the melting point of iron, 1535 C, but not so hot as to melt olivine, 1760 C.</div></td></tr>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[File:imilac-meteorite6494-cp.jpg|600px]]</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>[[File:imilac-meteorite6494-cp.jpg|600px]]</div></td></tr>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Carbonaceous chondrites are a type of meteorite known to contain high concentrations of water and organic compounds. The Murchison Meteorite, which fell near Murchison, Australia, in 1969, has been found to contain over 100 amino acids, some rarely seen on Earth, and also purines and pyrimidines, nucleotide bases that are building blocks of DNA and RNA. This discovery shows that amino acids and components of the genetic code, were already present in the early solar system, available not only to Earth but to other planets and moons as well.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">[http://en.wikipedia.org/wiki/Carbonaceous_chondrite </ins>Carbonaceous chondrites<ins style="font-weight: bold; text-decoration: none;">] </ins>are a type of meteorite known to contain high concentrations of water and organic compounds. The <ins style="font-weight: bold; text-decoration: none;">[http://en.wikipedia.org/wiki/Murchison_meteorite </ins>Murchison Meteorite<ins style="font-weight: bold; text-decoration: none;">]</ins>, which fell near Murchison, Australia, in 1969, has been found to contain over 100 <ins style="font-weight: bold; text-decoration: none;">[http://en.wikipedia.org/wiki/Amino_acid </ins>amino acids<ins style="font-weight: bold; text-decoration: none;">]</ins>, some rarely seen on Earth, and also <ins style="font-weight: bold; text-decoration: none;">[http://en.wikipedia.org/wiki/Purine </ins>purines<ins style="font-weight: bold; text-decoration: none;">] </ins>and <ins style="font-weight: bold; text-decoration: none;">[http://en.wikipedia.org/wiki/Pyrimidine </ins>pyrimidines<ins style="font-weight: bold; text-decoration: none;">]</ins>, nucleotide bases that are building blocks of DNA and RNA. This discovery shows that amino acids and components of the genetic code, were already present in the early solar system, available not only to Earth but to other planets and moons as well.</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>In addition to organic chemicals coming via meteorites, seventeen of the twenty amino acids have been produced in the laboratory, in experiments simulating the early Earth, complete with water, heat, and an electric spark for lightning.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>In addition to organic chemicals coming via meteorites, seventeen of the twenty amino acids have been produced in the laboratory, in <ins style="font-weight: bold; text-decoration: none;">[http://news.bbc.co.uk/2/hi/science/nature/7675193.stm </ins>experiments simulating the early Earth<ins style="font-weight: bold; text-decoration: none;">]</ins>, complete with water, heat, and an electric spark for lightning.</div></td></tr>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Amino acids are made up simply of hydrogen (H), carbon (C), oxygen (O), and nitrogen (N), and occasionally sulfur (S).</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>Amino acids are made up simply of hydrogen (H), carbon (C), oxygen (O), and nitrogen (N), and occasionally sulfur (S).</div></td></tr>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>While amino acids are the building blocks of proteins, purines and pyrimidines (also called nucleobases or nucleotide bases) are the building blocks of DNA and RNA. They, also, are simple compounds of hydrogen (H), carbon (C), oxygen (O), and nitrogen (N), all found in the interstellar gas from which stars and planets form.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>While amino acids are the building blocks of <ins style="font-weight: bold; text-decoration: none;">'''</ins>proteins<ins style="font-weight: bold; text-decoration: none;">'''</ins>, purines and pyrimidines (also called nucleobases or nucleotide bases) are the building blocks of <ins style="font-weight: bold; text-decoration: none;">'''</ins>DNA<ins style="font-weight: bold; text-decoration: none;">''' </ins>and <ins style="font-weight: bold; text-decoration: none;">'''</ins>RNA<ins style="font-weight: bold; text-decoration: none;">'''</ins>. They, also, are simple compounds of hydrogen (H), carbon (C), oxygen (O), and nitrogen (N), all found in the interstellar gas from which stars and planets form.</div></td></tr>
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<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>These nucleotide bases are abbreviated A,G,C, T, and U.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>These <ins style="font-weight: bold; text-decoration: none;">[http://en.wikipedia.org/wiki/Nucleobases </ins>nucleotide bases<ins style="font-weight: bold; text-decoration: none;">] </ins>are abbreviated A,G,C, T, and U.</div></td></tr>
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</table>WikiSysophttps://prancer.physics.louisville.edu/astrowiki/index.php?title=Periodic_Table_of_the_Elements&diff=806&oldid=prevWikiSysop: /* Origins of Chemical Compounds */2012-02-20T09:54:41Z<p><span dir="auto"><span class="autocomment">Origins of Chemical Compounds</span></span></p>
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<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Everyone's favorite compound is water. <del style="font-weight: bold; text-decoration: none;">H2O </del>forms naturally in space, through chemical reactions on the surface of dust grains and in cold dense gas. Water on the cold dust remains ice as long as it is cold, eventually finding its way into the disk from which planets form. NASA has an airborn observatory to study how this happens.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Everyone's favorite compound is water. <ins style="font-weight: bold; text-decoration: none;">H<sub>2</sub>O </ins>forms naturally in space, through chemical reactions on the surface of dust grains and in cold dense gas. Water on the cold dust remains ice as long as it is cold, eventually finding its way into the disk from which planets form. NASA has an <ins style="font-weight: bold; text-decoration: none;">[http://www.sofia.usra.edu/ </ins>airborn observatory<ins style="font-weight: bold; text-decoration: none;">] </ins>to study how this happens.</div></td></tr>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The processes that determine water formation and destruction depend on temperature. You know that hydrogen "burns", and in the presence of oxygen it will self ignite at 550 C (1022 F) and form water. In the protoplanetary disk, from which the solar system formed, water was present in large quantities. It was ice in the cold outer regions, and gas was where it was warmer, closer to the early Sun. Above 3000 C water will dissociate into OH and H, so there is no water in the atmosphere of the Sun or close to it. However, even when it is cold, unprotected by a planetary atmosphere or by dust in the disk, water is dissociated by sunlight. Its oxygen and hydrogen atoms are ionized, and blown out by the solar wind. Small bodies like Mercury or the Moon had too little gravity to hold on to water, and no atmosphere to prevent its dissociation and loss. In the outer solar system, water and ice were retained by some of the satellites of Jupiter and Saturn. The Oort Cloud, a remant of the solar nebula, is where icy comets still reside.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The processes that determine water formation and destruction depend on temperature. You know that hydrogen "burns", and in the presence of oxygen it will self ignite at 550 C (1022 F) and form water. In the protoplanetary disk, from which the solar system formed, water was present in large quantities. It was ice in the cold outer regions, and gas was where it was warmer, closer to the early Sun. Above 3000 C water will dissociate into OH and H, so there is no water in the atmosphere of the Sun or close to it. However, even when it is cold, unprotected by a planetary atmosphere or by dust in the disk, water is dissociated by sunlight. Its oxygen and hydrogen atoms are ionized, and blown out by the solar wind. Small bodies like Mercury or the Moon had too little gravity to hold on to water, and no atmosphere to prevent its dissociation and loss. In the outer solar system, water and ice were retained by some of the satellites of Jupiter and Saturn. The Oort Cloud, a remant of the solar nebula, is where icy comets still reside.</div></td></tr>
</table>WikiSysophttps://prancer.physics.louisville.edu/astrowiki/index.php?title=Periodic_Table_of_the_Elements&diff=805&oldid=prevWikiSysop: /* Origins of Chemical Compounds */2012-02-20T09:52:50Z<p><span dir="auto"><span class="autocomment">Origins of Chemical Compounds</span></span></p>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>'''''But where did water ( H<sub>2</sub>O ), olivine ( ( Mg, Fe )<sub>2</sub>SiO<sub>4</sub> ), and amino acids (such as C<<del style="font-weight: bold; text-decoration: none;">/</del>sub>3</sub>H<sub>5</sub>NO ) come from?'''''</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>'''''But where did water ( H<sub>2</sub>O ), olivine ( ( Mg, Fe )<sub>2</sub>SiO<sub>4</sub> ), and amino acids (such as C<sub>3</sub>H<sub>5</sub>NO ) come from?'''''</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>When dying stars explode and make beautiful planetary nebulae and supernova remnants, they spew out heavy elements that had been fused in their cores.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>When dying stars explode and make beautiful planetary nebulae and supernova remnants, they spew out heavy elements that had been fused in their cores.</div></td></tr>
</table>WikiSysophttps://prancer.physics.louisville.edu/astrowiki/index.php?title=Periodic_Table_of_the_Elements&diff=804&oldid=prevWikiSysop: /* Origins of Chemical Compounds */2012-02-20T09:52:28Z<p><span dir="auto"><span class="autocomment">Origins of Chemical Compounds</span></span></p>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><del style="font-weight: bold; text-decoration: none;"><center></del>'''''But where did water ( H<sub>2</sub>O ), olivine ( ( Mg, Fe )<sub>2</sub>SiO<sub>4</sub> ), and amino acids (such as C</sub>3</sub>H<sub>5</sub>NO ) come from?'''''<del style="font-weight: bold; text-decoration: none;"></center></del></div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>'''''But where did water ( H<sub>2</sub>O ), olivine ( ( Mg, Fe )<sub>2</sub>SiO<sub>4</sub> ), and amino acids (such as C</sub>3</sub>H<sub>5</sub>NO ) come from?'''''</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>When dying stars explode and make beautiful planetary nebulae and supernova remnants, they spew out heavy elements that had been fused in their cores.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>When dying stars explode and make beautiful planetary nebulae and supernova remnants, they spew out heavy elements that had been fused in their cores.</div></td></tr>
</table>WikiSysophttps://prancer.physics.louisville.edu/astrowiki/index.php?title=Periodic_Table_of_the_Elements&diff=803&oldid=prevWikiSysop: /* Origins of Chemical Compounds */2012-02-20T09:51:59Z<p><span dir="auto"><span class="autocomment">Origins of Chemical Compounds</span></span></p>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div><center>'''''But where did water ( H<sub>2</sub>O ), olivine ( ( Mg, Fe )<sub>2</sub>SiO<sub>4</sub> ), and amino acids (such as C</sub>3</sub>H<sub>5</sub>NO ) come from?'''''<<del style="font-weight: bold; text-decoration: none;">.</del>center></div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><center>'''''But where did water ( H<sub>2</sub>O ), olivine ( ( Mg, Fe )<sub>2</sub>SiO<sub>4</sub> ), and amino acids (such as C</sub>3</sub>H<sub>5</sub>NO ) come from?'''''<<ins style="font-weight: bold; text-decoration: none;">/</ins>center></div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>When dying stars explode and make beautiful planetary nebulae and supernova remnants, they spew out heavy elements that had been fused in their cores.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>When dying stars explode and make beautiful planetary nebulae and supernova remnants, they spew out heavy elements that had been fused in their cores.</div></td></tr>
</table>WikiSysophttps://prancer.physics.louisville.edu/astrowiki/index.php?title=Periodic_Table_of_the_Elements&diff=802&oldid=prevWikiSysop: /* Origins of Chemical Compounds */2012-02-20T09:51:47Z<p><span dir="auto"><span class="autocomment">Origins of Chemical Compounds</span></span></p>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div> </div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;"><center>'''''</ins>But where did water ( <ins style="font-weight: bold; text-decoration: none;">H<sub>2</sub>O </ins>), olivine ( ( Mg, Fe )<ins style="font-weight: bold; text-decoration: none;"><sub>2</sub>SiO<sub>4</sub> </ins>), and amino acids (such as <ins style="font-weight: bold; text-decoration: none;">C</sub>3</sub>H<sub>5</sub>NO </ins>) come from?<ins style="font-weight: bold; text-decoration: none;">'''''<.center></ins></div></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>But where did water ( <del style="font-weight: bold; text-decoration: none;">H2O </del>), olivine ((Mg,Fe)<del style="font-weight: bold; text-decoration: none;">2SiO4 </del>), and amino acids (such as <del style="font-weight: bold; text-decoration: none;">C3H5NO </del>) come from?</div></td><td colspan="2" class="diff-side-added"></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>When dying stars explode and make beautiful planetary nebulae and supernova remnants, they spew out heavy elements that had been fused in their cores.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>When dying stars explode and make beautiful planetary nebulae and supernova remnants, they spew out heavy elements that had been fused in their cores.</div></td></tr>
</table>WikiSysophttps://prancer.physics.louisville.edu/astrowiki/index.php?title=Periodic_Table_of_the_Elements&diff=801&oldid=prevWikiSysop: /* Origins of Elements */2012-02-20T09:49:05Z<p><span dir="auto"><span class="autocomment">Origins of Elements</span></span></p>
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<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>When giant stars die, they not only send out elements up to iron, but in the shockwaves from their explosive supernova, create elements heavier than iron, such as silver (Ag), gold (Au), and platinum (Pt).</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>When giant stars die, they not only send out elements up to iron, but in the <ins style="font-weight: bold; text-decoration: none;">[http://en.wikipedia.org/wiki/Shock_wave </ins>shockwaves<ins style="font-weight: bold; text-decoration: none;">] </ins>from their explosive supernova, create elements heavier than iron, such as silver (Ag), gold (Au), and platinum (Pt).</div></td></tr>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Every living thing is made of bits of Big Bang (H), chemicals fused in stars (O) (C), and bits of Supernova remnants (Cu) ! Every living thing has stardust in it.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div><ins style="font-weight: bold; text-decoration: none;">[http://youtu.be/m5TwT69i1lU </ins>Every living thing<ins style="font-weight: bold; text-decoration: none;">] </ins>is made of bits of Big Bang (H), chemicals fused in stars (O) (C), and bits of Supernova remnants (Cu) ! Every living thing has stardust in it.</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Origins of Chemical Compounds ==</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>== Origins of Chemical Compounds ==</div></td></tr>
</table>WikiSysophttps://prancer.physics.louisville.edu/astrowiki/index.php?title=Periodic_Table_of_the_Elements&diff=800&oldid=prevWikiSysop: /* Origins of Elements */2012-02-20T09:47:36Z<p><span dir="auto"><span class="autocomment">Origins of Elements</span></span></p>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>At the time of the Big Bang, pressure and temperatures were such that subatomic particles could form. As conditions changed so did the types of particles that formed. Electrons, quarks, protons and neutrons, all happened in a fraction of a second. Helium ions, 2 protons and 2 neutrons in one nucleus, were present after 3 minutes. Not until 300,000 years later was the universe cool enough to allow protons, helium and other nuclei to capture electrons to create atoms of hydrogen, and helium, and traces of lithium and beryllium.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>At the time of the <ins style="font-weight: bold; text-decoration: none;">'''</ins>Big Bang<ins style="font-weight: bold; text-decoration: none;">'''</ins>, <ins style="font-weight: bold; text-decoration: none;">'''</ins>pressure<ins style="font-weight: bold; text-decoration: none;">''' </ins>and <ins style="font-weight: bold; text-decoration: none;">'''</ins>temperatures<ins style="font-weight: bold; text-decoration: none;">''' </ins>were such that subatomic particles could form. As conditions changed so did the types of particles that formed. Electrons, quarks, protons and neutrons, all happened in a fraction of a second. Helium ions, 2 protons and 2 neutrons in one nucleus, were present after 3 minutes. Not until 300,000 years later was the universe cool enough to allow protons, helium and other nuclei to capture electrons to create atoms of hydrogen, and helium, and traces of lithium and beryllium.</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>To this day the most abundant element in the universe is still hydrogen. It shows up as a magenta color in many star forming nebulae, such as the Horsehead Nebula where hydrogen is reacting with starlight. The dark absorbing cloud that forms the familiar shape and blocks our view of stars behind the nebula, is dust, mostly made of carbon.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>To this day the most abundant element in the universe is still hydrogen. It shows up as a magenta color in many star forming nebulae, such as the Horsehead Nebula where hydrogen is reacting with starlight. The dark absorbing cloud that forms the familiar shape and blocks our view of stars behind the nebula, is dust, mostly made of carbon.</div></td></tr>
</table>WikiSysophttps://prancer.physics.louisville.edu/astrowiki/index.php?title=Periodic_Table_of_the_Elements&diff=799&oldid=prevWikiSysop: /* Elements */2012-02-20T09:46:13Z<p><span dir="auto"><span class="autocomment">Elements</span></span></p>
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<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The '''atomic mass''' is roughly the number of protons + neutrons (plus a little more for the electrons and the fact that a neutron is slightly more massive than a proton). Most light atoms have the same number of neutrons as protons. So the atomic mass of He is (2 protons + 2 neutrons) roughly 4 (plus a little more). The '''exceptions''' are (1) Hydrogen, which is found most often as a proton with an electron and no neutron, and (2) the heaviest elements, which need more neutrons to glue the atom together keeping the protons from repelling each other. For example, copper has an atomic number of 29 (29 protons) but an atomic mass, not of 58 but of 63 meaning it has 34 neutrons. (Specifically one atomic mass unit equals 1/12th the mass of a carbon atom, but it is easiest just to look up the atomic mass on the Periodic Table.)</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>The '''atomic mass''' is roughly the number of protons + neutrons (plus a little more for the electrons and the fact that a neutron is slightly more massive than a proton). Most light atoms have the same number of neutrons as protons. So the atomic mass of He is (2 protons + 2 neutrons) roughly 4 (plus a little more). The '''exceptions''' are (1) Hydrogen, which is found most often as a proton with an electron and no neutron, and (2) the heaviest elements, which need more neutrons to glue the atom together keeping the protons from repelling each other. For example, copper has an atomic number of 29 (29 protons) but an atomic mass, not of 58 but of 63 meaning it has 34 neutrons. (Specifically one atomic mass unit equals 1/12th the mass of a carbon atom, but it is easiest just to look up the atomic mass on the Periodic Table.)</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker" data-marker="−"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #ffe49c; vertical-align: top; white-space: pre-wrap;"><div>Atoms are normally '''neutral''', that is there are the same number of protons (positive charges) in an atom, as there are electrons (negative charges). If an atom has too many or too few electrons, it is called an '''ion'''. If there are too many electrons it is a negative ion (since electrons have a negative charge.) If it has too few electrons it is a positive ion. Dissolve table salt in water and the NaCl molecule becomes Na<sup>+</sup>and Cl<sup>-</sup in solution. In the Earth's atmosphere, N<sub>2 </sub> (nitrogen molecule) and O<sub>2</sub> (oxygen molecule) may lose an electron when struck by a cosmic ray and become the ions N<sub>2</sub><sup>+</sup> and O<sub>2</sub><sup>+</sup>. Sunlight and starlight can ionize elements and compounds. In interstellar gas, neutral H atoms may become H+, a bare proton with no electron.</div></td><td class="diff-marker" data-marker="+"></td><td style="color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #a3d3ff; vertical-align: top; white-space: pre-wrap;"><div>Atoms are normally '''neutral''', that is there are the same number of protons (positive charges) in an atom, as there are electrons (negative charges). If an atom has too many or too few electrons, it is called an '''ion'''. If there are too many electrons it is a negative ion (since electrons have a negative charge.) If it has too few electrons it is a positive ion. Dissolve table salt in water and the NaCl molecule becomes Na<sup>+</sup>and Cl<sup>-</sup<ins style="font-weight: bold; text-decoration: none;">> </ins>in solution. In the Earth's atmosphere, N<sub>2 </sub> (nitrogen molecule) and O<sub>2</sub> (oxygen molecule) may lose an electron when struck by a cosmic ray and become the ions N<sub>2</sub><sup>+</sup> and O<sub>2</sub><sup>+</sup>. Sunlight and starlight can ionize elements and compounds. In interstellar gas, neutral H atoms may become H<ins style="font-weight: bold; text-decoration: none;"><sup></ins>+<ins style="font-weight: bold; text-decoration: none;"></sup></ins>, a bare proton with no electron.</div></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><br/></td></tr>
<tr><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>If positive ions and negative ions are adjacent, and the environment is right, they will naturally [http://www.youtube.com/watch?v=xTx_DWboEVs&NR=1 combine]. Another way elements can combine to form compounds is by [http://www.youtube.com/watch?v=1wpDicW_MQQ covalent bonding], sharing electrons.</div></td><td class="diff-marker"></td><td style="background-color: #f8f9fa; color: #202122; font-size: 88%; border-style: solid; border-width: 1px 1px 1px 4px; border-radius: 0.33em; border-color: #eaecf0; vertical-align: top; white-space: pre-wrap;"><div>If positive ions and negative ions are adjacent, and the environment is right, they will naturally [http://www.youtube.com/watch?v=xTx_DWboEVs&NR=1 combine]. Another way elements can combine to form compounds is by [http://www.youtube.com/watch?v=1wpDicW_MQQ covalent bonding], sharing electrons.</div></td></tr>
</table>WikiSysop