Results 121 to 130 of about 3,880,015 (181)
Equation of State of Four- and Five-Dimensional Hard-Hypersphere Mixtures. [PDF]
Entropy (Basel), 2020 López de Haro M, Santos A, B Yuste S.
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Potential energy landscape of a flexible water model: Equation of state, configurational entropy, and Adam-Gibbs relationship. [PDF]
J Chem PhysEltareb A, Lopez GE, Giovambattista N.
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System size dependence of the non-monotonous pion freeze-out volume excitation function
Open Physics, 2012 Li Qingfeng +2 more
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Equations of State and Constitutive Equations
Journal of Rheology, 1986Equations-of state information in the otherwise undeformed state as a starting point for the development of constitutive equations is considered in addition to thermodynamics, free energy functions, and conceptual difficulties including the definition of reference states for strain.
Landel, Robert F., Peng, Steven T. J.
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Representation Of Continuous-time State Equations By Discrete-time State Equations
1977 11th Asilomar Conference on Circuits, Systems and Computers, 1977. Conference Record., 1978A method, based on multi-feedback and multi-feedforward control theory, is developed in the time domain for accurately representing continuous-time state equations by discrete-time state equations. A matrix continued fraction method is used as a basis for this work.
Shieh, Leang-San +2 more
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Physical Review B, 1988
The "universal" equation of state recently proposed by Vinet, Ferrante, Rose, and Smith is numerically equivalent, to leading order in finite strain, to several well-established two-parameter equations of state. Notably, it is in accord with the Birch-Murnaghan equation that is derived from Eulerian finite-strain theory, and hence is applicable to ...
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The "universal" equation of state recently proposed by Vinet, Ferrante, Rose, and Smith is numerically equivalent, to leading order in finite strain, to several well-established two-parameter equations of state. Notably, it is in accord with the Birch-Murnaghan equation that is derived from Eulerian finite-strain theory, and hence is applicable to ...
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2019
At the critical point one has \(\left( \partial p/\partial V_M\right) _T =0\) and \(\left( \partial ^2 p/\partial V_M^2\right) _T=0\). By calculating the derivative of the van der Waals equation with respect to \(V_M\), we find that the first condition reads \(p_c-a/V_{Mc}^2+2ab/V_{Mc}^3=0\).
Gregor Skačej, Primož Ziherl
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At the critical point one has \(\left( \partial p/\partial V_M\right) _T =0\) and \(\left( \partial ^2 p/\partial V_M^2\right) _T=0\). By calculating the derivative of the van der Waals equation with respect to \(V_M\), we find that the first condition reads \(p_c-a/V_{Mc}^2+2ab/V_{Mc}^3=0\).
Gregor Skačej, Primož Ziherl
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Proceedings of Latin American & Caribbean Petroleum Engineering Conference, 2007
Summary To predict the phase and volumetric behavior of hydrocarbon mixtures by using an Equation of State; e.g. the Peng and Robinson Equation of State "PREOS", the critical properties in terms of the critical pressure "pc" and critical temperature "Tc" as well as the acentric factor "ω" must be given for each component present in the ...
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Summary To predict the phase and volumetric behavior of hydrocarbon mixtures by using an Equation of State; e.g. the Peng and Robinson Equation of State "PREOS", the critical properties in terms of the critical pressure "pc" and critical temperature "Tc" as well as the acentric factor "ω" must be given for each component present in the ...
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2004
The equations of state appropriate to the interiors of most stars are simple in one major respect: they may be derived using the assumption that the radiation, gas, fluid, or even solid, is in a state of local thermodynamic equilibrium or LTE. By this we mean that at a particular position in the star complete thermodynamic equilibrium is as very nearly
Carl J. Hansen +2 more
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The equations of state appropriate to the interiors of most stars are simple in one major respect: they may be derived using the assumption that the radiation, gas, fluid, or even solid, is in a state of local thermodynamic equilibrium or LTE. By this we mean that at a particular position in the star complete thermodynamic equilibrium is as very nearly
Carl J. Hansen +2 more
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