Effective interactions and elementary excitations in nuclear matter

Pines, David; Quader, Khandker; Wambach, J.

doi:10.1016/0375-9474(88)90348-x

Cited by 37 publications

(26 citation statements)

References 26 publications

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“…The above expressions have been built such as M * /M = 1 in the limit for q → ∞ and M * = M * 0 for q → 0. Various nuclear structure studies [20,24,25] indicate that M * 0 /M =0.8, and this is the value we have used in our calculations.…”

Section: Resultsmentioning

confidence: 99%

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Effects of nuclear re-interactions in quasi-elastic neutrino–nucleus scattering

Bleve¹,

Có²,

Mitri³

et al. 2001

Astroparticle Physics

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Section: Resultsmentioning

confidence: 99%

“…It has been determined by using the expressions proposed in the polarization potential model of ref. [24]:…”

Section: Resultsmentioning

confidence: 99%

Effects of nuclear re-interactions in quasi-elastic neutrino–nucleus scattering

Bleve¹,

Có²,

Mitri³

et al. 2001

Astroparticle Physics

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“…(4.25), %0=120 MeV. Pines et al (1988) have carried out a comprehensive calculation using the polarization potential approach. If F& is assumed known (=0), and Fo is determined from the sum rule (4.18), the Pines calculation yields IC0=120 (see Brown, 1988b), so 120…”

Section: The Compression Modulus Komentioning

confidence: 99%

Supernova mechanisms

1990

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Supernovae of Type II occur at the end of the evolution of massive stars. The phenomenon begins when the iron core of the star exceeds a Chandrasekhar mass. The collapse of that core under gravity is well understood and takes a fraction of a second. To understand the phenomenon, a detailed knowledge of the equation of state at the relevant densities and temperatures is required. After collapse, the shock wave moves outward, but probably does not succeed in expelling the mass of the star. The most likely mechanisrn to do so is the absorption of neutrinos from the core by the material at medium distances. Observations and theory connected with SN 1987A are discussed, as are the conditions just before collapse and the emission of neutrinos by the collapsed core.

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“…We straightforwardly used the interaction as given in Ref. [54] and we obtained for the energy of the low-lying 3 − state the value of 6.65 MeV.…”

Section: Testing the Direct Knock-out Modelmentioning

confidence: 99%

Short-Range Correlations and Meson Exchange Currents in Photonucleon Emission

et al. 2002

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One-nucleon emission processes induced by photon absorption are studied by considering shortrange correlation effects. At energies above the giant resonance region the validity of the direct knockout model has been tested by comparison with continuum random phase approximation results. Nucleon re-scattering effects have been considered by using an optical potential. The role of the electromagnetic convection, magnetization, and meson exchange currents has been investigated as a function of both excitation energy and momentum transfer. The short-range correlation effects have been studied by using various correlation functions. We found that the nucleon photo-emission cross section is rather sensitive to the presence of short-range correlations at large values of nucleon emission angle. In this region, however, the effects of meson exchange currents are even larger than those produced by short-range correlations. C 2002 Elsevier Science (USA)

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Effective interactions and elementary excitations in nuclear matter

Cited by 37 publications

References 26 publications

Effects of nuclear re-interactions in quasi-elastic neutrino–nucleus scattering

Effects of nuclear re-interactions in quasi-elastic neutrino–nucleus scattering

Supernova mechanisms

Short-Range Correlations and Meson Exchange Currents in Photonucleon Emission

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