Non-Abelian density functional theory

Vlasov, George V.

doi:10.1103/physrevc.58.2581

Cited by 2 publications

(7 citation statements)

References 19 publications

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“…Nevertheless, it is highly desirable to find the neutron star parameters with exact EOS and reveal the essence of correlation energy. The recent exact accounts of the correlation energy [11] were performed for the σ model with the Lagrangian…”

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confidence: 99%

“…in addition to the exchange terms (10)- (11). The total energy density of the system ε is determined by Eqs.…”

mentioning

confidence: 99%

“…(12)-(19) yield high accurate solution after a series of iterations. In our previous simulation [11] we requested saturation at k F = 1.36 fm −1 , that yielded the binding energy E B = −12.8 MeV per nucleon and the compression modulus K = 314 MeV. Now we have adjusted the coupling constant g = 13.96 in order to get the empirical saturation value of E B = −15.75 MeV.…”

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confidence: 99%

“…Our Lagrangian (8) corresponds to an intermediate situation (K = 285 MeV and M * = 1.64M ). However, the main advantage of (8) concerns the possibility of development in terms of response-functions and the possibility to evaluate the correlation energy (20) [11][12][13]. It is wellknown from solid-state physics that the correlation energy softens the EOS [17], now it is proved in the direct nuclear matter calculation.…”

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confidence: 99%

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Correlation energy of nuclear matter and neutron star masses

Trojan¹,

Vlasov

2010

Phys. Rev. C

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We consider nuclear matter in the frames of the sigma model and find the role of correlation energy in the determination of the parameters of neutron stars. The response-function formalism is used for calculations within the Hartree-Fock approach and beyond. When electrons and muons are present in the neutron-rich matter, the maximal mass of the star is M * = 1.64 (in the unit of the solar mass M ). The correlation energy becomes very important for the stars with M * ∼ 0.7 ÷ 1.5M and its effect is estimated as 0.3 ÷ 0.4M extracted from the relevant values obtained in the frames of the Hartree-Fock approximation. On the whole, the nuclear equation of state is definitely "softened."

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confidence: 99%

“…in addition to the exchange terms (10)- (11). The total energy density of the system ε is determined by Eqs.…”

mentioning

confidence: 99%

mentioning

confidence: 99%

mentioning

confidence: 99%

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Correlation energy of nuclear matter and neutron star masses

Trojan¹,

Vlasov

2010

Phys. Rev. C

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“…Both PN and AS EOS are no more than limiting theoretical possibilities, while the real nuclear matter includes strong interaction and its EOS is stiffer than PN EOS but softer than AS EOS. For a reliable example we consider the neutron-rich matter in the nonlinear sigma model (NSM) [10,11]. This NSM EOS was calculated at a high accuracy, including the effect of correlation energy, and its EOS stands between PN and AS -by these three alternatives we manage to embrace the whole range of possible envelope materials.…”

Section: Tachyon Core In Non-tachyonic Envelopementioning

confidence: 99%

Tachyon stars

Trojan

2011

Preprint

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We consider a self-gravitating body composed of ideal Fermi gas of tachyons at zero temperature. The Oppenheimer-Volkoff equation is solved for various central densities and various tachyon mass parameter m. Although a pure tachyon star has finite mass, it cannot occur in nature because the equilibrium condition P = 0 and the causality condition cannot be satisfied simultaneously. A stable configuration with tachyon content must be covered with a non-tachyon envelope. The boundary between the tachyon core and the envelope is determined by the critical pressure P T , which depends on the tachyon mass m. The tachyon core is dominant and its mass can exceed many times the solar mass M when m is much smaller than the nucleon mass m p , while at large m compared with m p , the main contribution to the total stellar mass is due to the envelope whose material determines the parameters of the whole star. However, the parameters of the tachyon core do not depend on the envelope material. When the tachyon core appears, its mass M T and radius r T grow up with increasing central density until maximum values are reached, after which the mass and radius slowly decrease. The redshift at the surface of the tachyon core does not depend on m and never exceeds z max 0.3. The maximum mass of tachyon core and its maximum radius are achieved at certain central density and obey universal formulas M T max /M = 0.52m 2 p /m 2 and r T max [km] = 4.07 m 2 p /m 2 that allow to estimate arbitrary supermassive tachyonic bodies at the cosmological scale.

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Non-Abelian density functional theory

Cited by 2 publications

References 19 publications

Correlation energy of nuclear matter and neutron star masses

Correlation energy of nuclear matter and neutron star masses

Tachyon stars

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