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Explore the physics of highly compressed matter, including the equation of state under high pressure conditions. Learn about bulk modulus, Fermi pressure, and ionization effects on the state of matter. Delve into experiments, planetary physics, and atomic models in hot, dense plasmas. This study covers a wide range of temperatures and densities, offering insights into the behavior of matter under extreme conditions.
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More’s QEOS • The pressure is equal to zero at the solid density and the experimental bulk modulus is reproduced. • The cold pressure at the density less than the solid density should be negative (tensile force). • The Fermi pressure of electron is reproduced to be a dominant term at high density in the limit of eF >> Te, wheneFis the Fermi energy of electron. • The ideal gas EOS should be reproduced at high temperature Te >> eF . • The effective charge Z* is determined not only by the thermal ionization, but also by the pressure ionization.
Formula of Equation of State Applicable to Wide Range of T and n Total Free Energy Thermodynamic Consistency
Ion Equation of State (Cowan Model by More) • 0 < Ti < D (low-temperature solid phase) • D< Ti < Tm (high-temperature solid phase) • Tm < Ti (fluid phase)
Melting Temperature (eV)
Electron Equation of State based on Thomas-Fermi Model
Thomas Fermi Model Takabe-Takami model,
varies from Ge= 2/3 for x >> 1 to Ge = 2/3 g (= 0.821) for x << 1.
Bonding Correction where Pb0 = eb0brs/3, rs the solid density, R/Rs = (rs / r)1/3. The parameters eb0 and b are determined so that the total pressure is equal to zero at r = rs and Te = 0 and the bulk modulus defined by
Image of Atoms in Hot-Dense Plasmas(Pressure Ionization) 10.2 Atomic Physics of Hot Dense Plasam
Average Atom Model Screened Hydrogen Model rn =a0n2 / Zn
photo excitation cross-section sm,m' ∫fm,m'ndn = 1 xn = Pn / gn
