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Electronic Structure and Covalent Bonding
Electronic Structure and Covalent Bonding

... -Aufbau principle: An electron goes into the available atomic orbital with the lowest energy. -Pauli exclusion principle: No more than two electrons can occupy each atomic orbital. -Hund’s rule: An electron goes into an empty degenerate orbital rather than pairing up. ...
Unit 2 Assignments Answers
Unit 2 Assignments Answers

... arrangement was brought on by the hydrogen bonding (a type of strong intermolecular force) water molecules have due to its V-shape structure with two sets of exposed lone-pairs, which makes water molecules very polar. As ice forms, the hexagonal structure takes up more space than its liquid counterp ...
this PDF file - Publications of the Serbian Chemical Society
this PDF file - Publications of the Serbian Chemical Society

... their cluster size distributions21 have been studied based on static crystalline properties and using ab initio potential respectively. Gupta proposed a semi-empirical potential to study the metallic fluids by molecular dynamics.22 Gupta potential function has been applied successfully by many resea ...
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Classical Thermodynamics I: Sublimation of Solid Iodine
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... about 1 atm to provide pressure broadening of the extremely sharp and intense absorption lines of the rotational fine structure (which can be individually resolved only by special techniques of laser spectroscopy). The reason lies in the logarithmic form of Eq. (34). Within the slit width or resolut ...
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18_Testbank - Lick Observatory

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In Situ Raman Spectroscopic Study of Gypsum (CaSO4·2H2O) and

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Chemistry - Chap 12 Homework Answers 2014

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AP Chemistry Chapter 11 Notes - Properties of Solutions In a , or

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299 Unit 9, Worksheet 1— Dalton`s Law of Partial Pressures

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Cold Fusion By Plasma Electrolysis of Water

... was formed from mass mF = 4,270602 ⋅10 −31 kg and flew away in the unknown direction; the second one – there were no conditions for the formation of the photons in the process being considered, and mass mF , which failed to be formed as a particle, “was dissolved” in the ether. Which variant is clos ...
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... d. Ice consists of water molecules in a hexagonal arrangement. 2. Compare a polar water molecule with a less-polar molecule, such as formaldehyde, CH2O. Both are liquids at room temperature and 1 atm pressure. a. Which liquid should have the higher boiling point? b. Which liquid is more volatile? c. ...
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Unit 1 review

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Degenerate matter

Degenerate matter in physics is a collection of free, non-interacting particles with a pressure and other physical characteristics determined by quantum mechanical effects. It is the analogue of an ideal gas in classical mechanics. The degenerate state of matter, in the sense of deviant from an ideal gas, arises at extraordinarily high density (in compact stars) or at extremely low temperatures in laboratories. It occurs for matter particles such as electrons, neutrons, protons, and fermions in general and is referred to as electron-degenerate matter, neutron-degenerate matter, etc. In a mixture of particles, such as ions and electrons in white dwarfs or metals, the electrons may be degenerate, while the ions are not.In a quantum mechanical description, free particles limited to a finite volume may take only a discrete set of energies, called quantum states. The Pauli exclusion principle prevents identical fermions from occupying the same quantum state. At lowest total energy (when the thermal energy of the particles is negligible), all the lowest energy quantum states are filled. This state is referred to as full degeneracy. The pressure (called degeneracy pressure or Fermi pressure) remains nonzero even near absolute zero temperature. Adding particles or reducing the volume forces the particles into higher-energy quantum states. This requires a compression force, and is made manifest as a resisting pressure. The key feature is that this degeneracy pressure does not depend on the temperature and only on the density of the fermions. It keeps dense stars in equilibrium independent of the thermal structure of the star.Degenerate matter is also called a Fermi gas or a degenerate gas. A degenerate state with velocities of the fermions close to the speed of light (particle energy larger than its rest mass energy) is called relativistic degenerate matter.Degenerate matter was first described for a mixture of ions and electrons in 1926 by Ralph H. Fowler, showing that at densities observed in white dwarfs the electrons (obeying Fermi–Dirac statistics, the term degenerate was not yet in use) have a pressure much higher than the partial pressure of the ions.
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