Collective dynamics of nuclear fusion: deformation changes and heating during the fusion

Mikhailov, I.N.; Mikhailova, T. I.; Toro, M. Di; Baran, V.; Briançon, Ch.

doi:10.1016/0375-9474(96)00166-2

Cited by 7 publications

(2 citation statements)

References 39 publications

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“…The estimates of the total kinetic energy for each component are compatible with the experimental data [9] as well as with recent dynamical calculations [20]. As an alternate dynamical approach, the virial-theorem-based approach, developped and initially applied to heavy-ion collisions by I. N. Mikhailov and collaborators [44], can also be applied to fission. This work is underway for the symmetric fission of the 258 Fm isotope with microscopically calculated ingredients, namely the potential-energy surface obtained in the present study and the inertia parameters calculated in the HFBCS framework as in Ref.…”

Section: Discussionsupporting

confidence: 49%

Fission modes ofFm256andFm258in a microscopic app

Bonneau

2006

Phys. Rev. C

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A static microscopic study of potential-energy surfaces within the Skyrme-Hartree-Fock-plus-BCS model is carried out for the 256 Fm and 258 Fm isotopes with the goal of deducing some properties of spontaneous fission. The calculated fission modes are found to be in agreement with the experimentaly observed asymmetric-to-symmetric transition in the fragment-mass distributions and with the high-and low-total-kinetic-energy modes experimentally observed in 258 Fm. Most of the results are similar to those obtained in macroscopic-microscopic models as well as in recent Hartree-FockBogolyubov calculations with the Gogny interaction, with a few differences in their interpretations. In particular an alternative explanation is proposed for the low-energy fission mode of 258 Fm.

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Section: Discussionsupporting

confidence: 49%

Fission modes ofFm256andFm258in a microscopic app

Bonneau

2006

Phys. Rev. C

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“…More precisely, the rate of energy dissipation by viscosity is described by the Newtonian law for viscous stresses [21,40]. Besides, the fingerprints of viscoelastic behaviour of macroscopic nuclear matter has also been disclosed in the dynamics of nuclear fusion [41,42] and fission [43] (see also [39]). At the same time, it must be stressed that the physics beyond the elastodynamics of nuclear resonant response is different from that for nuclear fission.…”

Section: Introductionmentioning

confidence: 99%

On the stability of global non-radial pulsations of neutron stars

Баструков

Weber²,

Podgainy

1999

J. Phys. G: Nucl. Part. Phys.

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A neutron star is the cosmic nuclear object in which the energy of gravitational pull is brought to equilibrium by elastic energy stored in the neutron Fermi-continuum. Evidence for the viscoelastic behaviour of a stellar nuclear matter provides a seismological model of pulsar glitches interpreted as a sudden release of the elastic energy. In laboratory nuclear physics, the signatures of viscoelasticity of nuclear matter are found in the current investigations on the collective nuclear dynamics, in which a heavy nucleus is modelled by a spherical piece of viscoelastic Fermicontinuum compressed to the normal nuclear density. It is plausible to expect, therefore, that the motions of self-gravitating nuclear matter constituting the interior of neutron stars should be governed by the equations of an elastic solid, rather than by hydrodynamic equations describing the behaviour of gaseous plasma inside the main sequence stars. In this paper, we present arguments that elastodynamic equations, originally introduced in the context of nuclear collective dynamics, can provide a proper account of elasticity in the large scale motions of neutron matter under its own gravity. Emphasis is placed on mathematical physics underlying the constructive description of the continuum mechanics and the rheology of macroscopic nuclear matter. The capability of the elastodynamic approach is examined by analysis of oscillatory dynamics of a neutron star in the standard homogenous model, operating with a spherical mass of self-gravitating degenerate neutron matter whose viscoelastic behaviour is described in terms of the spheroidal and torsional gravitational-elastic eigenmodes, inherenly related to viscoelasticy. The energy variational principle is utilized to compute the frequencies of viscoelastic gravitational pulsations and their relaxation time. The method is demonstrated for both the idealized homogeneous model and the neutron star models constructed on realistic equations of state. Finally, we derive analytic conditions for the stability of a neutron star to linear elastic deformations accompanying the nonradial pulsations, and discuss the fingerprints of these pulsations in the electromagnetic activity of radiopulsars.

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Collective energy dissipated in nucleus–nucleus collisions

Mikhailov¹,

Mikhailova

2004

Nuclear Physics A

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Collective dynamics of nuclear fusion: deformation changes and heating during the fusion

Cited by 7 publications

References 39 publications

Fission modes ofFm256andFm258in a microscopic app

Fission modes ofFm256andFm258in a microscopic app

On the stability of global non-radial pulsations of neutron stars

Collective energy dissipated in nucleus–nucleus collisions

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