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- https://phys.libretexts.org/Bookshelves/Quantum_Mechanics/Quantum_Mechanics_(Walet)/06%3A_Scattering_from_Potential_Steps_and_Square_Barriers
- https://phys.libretexts.org/Bookshelves/Optics/Geometric_Optics_(Tatum)/zz%3A_Back_Matter
- https://phys.libretexts.org/Bookshelves/Quantum_Mechanics/Quantum_Mechanics_(Walet)/03%3A_The_Schrodinger_Equation/3.03%3A_Analysis_of_the_wave_equationOne of the important aspects of the Schrödinger equation(s) is its linearity. For the time independent Schrödinger equation, which is usually called an eigenvalue problem.
- https://phys.libretexts.org/Bookshelves/University_Physics/Radically_Modern_Introductory_Physics_Text_II_(Raymond)/zz%3A_Back_Matter/11%3A_Glossaryextremely high frequency electromagnetic radiation emitted by the nucleus of an atom, either from natural nuclear decay or induced nuclear processes in nuclear reactors and weapons; the lower end of t...extremely high frequency electromagnetic radiation emitted by the nucleus of an atom, either from natural nuclear decay or induced nuclear processes in nuclear reactors and weapons; the lower end of the \(\displaystyle γ\) -ray frequency range overlaps the upper end of the X-ray range, but \(\displaystyle γ\) rays can have the highest frequency of any electromagnetic radiation
- https://phys.libretexts.org/Bookshelves/Quantum_Mechanics/Quantum_Mechanics_(Walet)/05%3A_Innite_Wells/5.01%3A_Zero_of_Energy_is_ArbitraryThat is a very workable definition, except in one case: if we take a square well and make it deeper and deeper, the energy of the lowest state decreases with the bottom of the well. As the well depth g...That is a very workable definition, except in one case: if we take a square well and make it deeper and deeper, the energy of the lowest state decreases with the bottom of the well. As the well depth goes to infinity, the energy of the lowest bound state reaches −∞, and so does the second, third etc. It makes much more physical sense to define the bottom of the well to have zero energy, and the potential outside to have value V 0, which goes to infinity.
- https://phys.libretexts.org/Bookshelves/Nuclear_and_Particle_Physics/Nuclear_and_Particle_Physics_(Walet)/04%3A_Nuclear_Models/4.01%3A_Nuclear_Shell_ModelThe simplest of the single particle models is the nuclear shell model. It is based on the observation that the nuclear mass formula, which describes the nuclear masses quite well on average, fails for...The simplest of the single particle models is the nuclear shell model. It is based on the observation that the nuclear mass formula, which describes the nuclear masses quite well on average, fails for certain “magic numbers”, i.e., for neutron number N=20, 28, 50, 82, 126 and proton number Z=20, 28, 50, 82.
- https://phys.libretexts.org/Bookshelves/Quantum_Mechanics/Quantum_Mechanics_(Walet)/13%3A_Miscellaneous_Quantum_Mechanics_Topics/13.01%3A_Bell's_TheoremA derivation of the theorem and a discussion of the consequences. A somewhat subtle topic, but here it is treated in a non-technical fashion. It assumes knowledge of wave-particle duality such as can ...A derivation of the theorem and a discussion of the consequences. A somewhat subtle topic, but here it is treated in a non-technical fashion. It assumes knowledge of wave-particle duality such as can be found in the Double Slit or the Wave-Particle Duality documents; also assumed is considerable knowledge of the Stern-Gerlach Experiment.
- https://phys.libretexts.org/Bookshelves/Astronomy__Cosmology/Supplemental_Modules_(Astronomy_and_Cosmology)/Cosmology/Astrophysics_(Richmond)/07%3A_Astronomical_Spectra%2C_Filters_and_MagnitudesThe u and v passbands, for example, lie just to the left and to the right of the strong break in the stellar spectrum (the "Balmer jump"); the ratio of the light gathered through these two passbands i...The u and v passbands, for example, lie just to the left and to the right of the strong break in the stellar spectrum (the "Balmer jump"); the ratio of the light gathered through these two passbands is a good diagnostic of stellar temperature. Note that the peak of the convolved spectrum lies to the blue of the filter transmission curve, because the stellar spectrum is "tilted" towards the blue.
- https://phys.libretexts.org/Bookshelves/Astronomy__Cosmology/Supplemental_Modules_(Astronomy_and_Cosmology)/Cosmology/Astrophysics_(Richmond)/19%3A_Digression_-_the_Lagrange_Points_in_the_3-Body_ProblemAlong the line joining the two masses Two bodies, no rotation. One body, with rotation. Two bodies, with rotation. Zoom in closer, two bodies with rotation. Lagrange points in action The SOHO satellit...Along the line joining the two masses Two bodies, no rotation. One body, with rotation. Two bodies, with rotation. Zoom in closer, two bodies with rotation. Lagrange points in action The SOHO satellite is close to the Earth-Sun L1 point. A discussion of the Lagrange Points from SOHO's web site. Technical derivation and analysis of the Lagrange Points, again by Neil Cornish. John Baez's page on the Lagrange Points (John is a mathematical physicist at UC Riverside)
- https://phys.libretexts.org/Bookshelves/Astronomy__Cosmology/Supplemental_Modules_(Astronomy_and_Cosmology)/Cosmology/Astrophysics_(Richmond)/22%3A_The_Boltzmann_EquationWhen an atom absorbs a photon, it jumps up to a higher level; the difference in energy of the two levels must be equal to the energy of the photon. "H-alpha" refers to the n=2 to n=3 transition, "H-be...When an atom absorbs a photon, it jumps up to a higher level; the difference in energy of the two levels must be equal to the energy of the photon. "H-alpha" refers to the n=2 to n=3 transition, "H-beta" to the n=2 to n=4 transition, "H-gamma" to the n=2 to n=5 transition, and so on. The second factor on the right-hand side depends on two quantities: the difference in energy between the two states, and the temperature T of the gas within which the atom sits.
- https://phys.libretexts.org/Bookshelves/Astronomy__Cosmology/Supplemental_Modules_(Astronomy_and_Cosmology)/Cosmology/Astrophysics_(Richmond)/06%3A_Blackbody_RadiationAt the turn of the twentieth century, German physicist Max Planck figured out a mathematical expression for the spectrum of radiation emitted from a blackbody, a (fictional) object which absorbs all i...At the turn of the twentieth century, German physicist Max Planck figured out a mathematical expression for the spectrum of radiation emitted from a blackbody, a (fictional) object which absorbs all incident radiation.
