Lecture_5_Molecules - 1 1 http://www. privatehand...

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Unformatted text preview: 1 1 http://www. privatehand .com/fash/element s.html 2 Where weve been H, He formed in Big Bang Heavier elements formed By fusion and neutron absorption in stars By neutron bombardment in supernovae 2 3 4 Where were going What happens when remnants of supernovae explosion cool down? Molecules form (which ones?) Some material exists as dust, ice, gas How does a planetary system (like the solar system) form? 3 5 6 Stellar nursuries In regions dense with matter, large stars will form Large stars which are capable of forming Fe (30X solar mass) burn for about 60 million years before ending in supernovae These large stars also emit streams of energetic particles which cause chemical (and some nuclear) changes in interstellar material Eventually all thats left are the longer burning smaller stars and their planetary systems made up of original gasses and the remnants of these explosions 4 7 Stars High temperatures Electrons are not bound to nucleus (plasma) Nuclear changes (physics) Interstellar clouds Low temperatures Electrons are bound to nucleus Electron sharing creates molecules (chemistry) 8 5 9 The mass of the atom is mostly in the nucleus (protons and neutrons) The size of the atom is determined by the electron cloud 10 Periodic Table of the Elements Review: What are the numbers in each box? 6 11 Electron shells and atomic structure First shell: 2 electrons Shell: energy level of electron Orbital: likely location of electron Each orbital can hold two electrons (different spins) 12 Second Shell: 8 electrons p-orbitals Two Electrons Six Electrons Second shell holds eight electrons (2s, 6p) 7 13 Third shell: 18 electrons p-orbitals Two Electrons Six Electrons d-orbitals...
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This note was uploaded on 02/08/2011 for the course EAS 1601 taught by Professor Lynch during the Spring '08 term at Georgia Institute of Technology.

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Lecture_5_Molecules - 1 1 http://www. privatehand...

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