Quasi-Free Scattering and Nuclear Structure

Jacob, Gerhard; Maris, Th.A.J.

doi:10.1103/revmodphys.38.121

Cited by 384 publications

(177 citation statements)

References 66 publications

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“…The QF reaction is well described in the the impulse approximation (IA) formalism [34][35][36][37][38][39][40][41][42][43][44][45], provided that (i) the momentum in the initial channel is sufficiently high or the associated wavelength is smaller than the nuclear radius of the Trojan horse nucleus a and the incident nucleus A can interact only with the fragment x, leaving the second fragment s as a spectator; (ii) the incident center-of-mass (c.m.) energy is higher than the binding energy of the clusters x and s in a.…”

Section: A Quasi-free Mechanism and Impulse Approximationmentioning

confidence: 99%

See 1 more Smart Citation

AstrophysicalS(E)factor of theN15(
Cognata
¹
,
Romano
²
,
Spitaleri
³

et al. 2007
Phys. Rev. C

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The low-energy bare-nucleus cross section for 15 N(p, α) 12 C is extracted by means of the Trojan horse method applied to the 2 H( 15 N,α 12 C)n reaction at E beam = 60 MeV. For the first time we applied the modified half-offenergy-shell resonant R-matrix method that takes into account off-energy-shell effects and initial-and final-state interactions. In particular it has been shown that inclusion of Coulomb 15 N-d scattering and off-shell effects do not affect the determination of the astrophysical factor. Also the simple plane-wave approximation used in previous analyses is justified. The results extracted via the Trojan horse method are compared to direct data in the same energy region and show very good agreement in the energy interval 70-312 keV. These results confirm the extrapolations of the S factor reported in literature.

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Section: A Quasi-free Mechanism and Impulse Approximationmentioning

confidence: 99%

“…As desired, the cross section of the TH reaction (3) can be factorized into two terms corresponding to Fig. 1(a) [36][37][38][40][41][42]45] by…”

Section: A Quasi-free Mechanism and Impulse Approximationmentioning

confidence: 99%

AstrophysicalS(E)factor of theN15(
Cognata
¹
,
Romano
²
,
Spitaleri
³

et al. 2007
Phys. Rev. C

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“…Theoretical analyses of the (p, pN) reactions with stable nuclei have been commonly done using the distorted-wave impulse approximation (DWIA) [6]. Roughly speaking, the impulse approximation (IA) means that the binding potential of the removed particle can be neglected in comparison with the projectile-target kinetic energy (see, e.g., Ref.…”

Section: Introductionmentioning

confidence: 99%

Three-body model for the analysis of quasifree scattering reactions in inverse kinematics

Moro

2015

Phys. Rev. C

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A new method to calculate cross sections for (p,pn) and (p,2p) reactions measured under inverse kinematics conditions is proposed. The method uses the prior form of the scattering transition amplitude and replaces the exact three-body wave function appearing in this expression with an expansion in terms of p-n or p-p states, covering the physically relevant excitation energies and partial waves. A procedure of discretization, similar to that used in continuum-discretized coupled-channels calculations, is applied to make this expansion finite and numerically tractable. The proposed formalism is nonrelativistic, but several relativistic kinematical corrections are applied to extend its applicability to energies of current interest. The underlying optical potentials for the entrance and exit channels are generated microscopically by folding an effective density-dependent G matrix with the density of the composite nucleus. Numerical calculations for 12 C(p,2p), 12 C(p,pn), and 23 O(p,pn) at ∼400 MeV/nucleon are presented to illustrate the method. The role of final-state interactions and Pauli principle between the outgoing nucleons is also discussed.

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“…The TH nucleus A breaks up into x and s which are called the participant and the spectator of the binary a(x, c)C reaction, respectively. Jacob et al 1966): The introduction of the penetration factor through the Coulomb barrier, described in terms of the regular and irregular Coulomb functions, and the normalization of the high-energy direct measurements make the extraction of the bare-nucleus S(E) factor possible (Equation (1)). The THM cross section represents the bare-nucleus cross section, as extensively discussed by Spitaleri et al (2004Spitaleri et al ( , 2011.…”

Section: The Trojan Horse Methodsmentioning

confidence: 99%

AN UPDATED⁶Li(p, α)³He REACTION RATE AT ASTROPHYSICAL ENERGIES WITH THE TROJAN HORSE METHOD

Lamia

Spitaleri

Pizzone

et al. 2013

ApJ

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The lithium problem influencing primordial and stellar nucleosynthesis is one of the most interesting unsolved issues in astrophysics. 6 Li is the most fragile of lithium's stable isotopes and is largely destroyed in most stars during the pre-main-sequence (PMS) phase. For these stars, the convective envelope easily reaches, at least at its bottom, the relatively low 6 Li ignition temperature. Thus, gaining an understanding of 6 Li depletion also gives hints about the extent of convective regions. For this reason, charged-particle-induced reactions in lithium have been the subject of several studies. Low-energy extrapolations of these studies provide information about both the zero-energy astrophysical S(E) factor and the electron screening potential, U e . Thanks to recent direct measurements, new estimates of the 6 Li(p, α) 3 He bare-nucleus S(E) factor and the corresponding U e value have been obtained by applying the Trojan Horse method to the 2 H( 6 Li, α 3 He)n reaction in quasi-free kinematics. The calculated reaction rate covers the temperature window 0.01 to 2T 9 and its impact on the surface lithium depletion in PMS models with different masses and metallicities has been evaluated in detail by adopting an updated version of the FRANEC evolutionary code.

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Quasi-Free Scattering and Nuclear Structure

Cited by 384 publications

References 66 publications

AstrophysicalS(E)factor of theN15(
Cognata
¹
,
Romano
²
,
Spitaleri
³

et al. 2007
Phys. Rev. C

AstrophysicalS(E)factor of theN15(
Cognata
¹
,
Romano
²
,
Spitaleri
³

et al. 2007
Phys. Rev. C

Three-body model for the analysis of quasifree scattering reactions in inverse kinematics

AN UPDATED⁶Li(p, α)³He REACTION RATE AT ASTROPHYSICAL ENERGIES WITH THE TROJAN HORSE METHOD

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Quasi-Free Scattering and Nuclear Structure

Cited by 384 publications

References 66 publications

AstrophysicalS(E)factor of theN15(Cognata1, Romano2, Spitaleri3 et al. 2007Phys. Rev. C

AstrophysicalS(E)factor of theN15(Cognata1, Romano2, Spitaleri3 et al. 2007Phys. Rev. C

Three-body model for the analysis of quasifree scattering reactions in inverse kinematics

AN UPDATED6Li(p, α)3He REACTION RATE AT ASTROPHYSICAL ENERGIES WITH THE TROJAN HORSE METHOD

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Product

Resources

About

AstrophysicalS(E)factor of theN15(
Cognata
¹
,
Romano
²
,
Spitaleri
³

et al. 2007
Phys. Rev. C

AstrophysicalS(E)factor of theN15(
Cognata
¹
,
Romano
²
,
Spitaleri
³

et al. 2007
Phys. Rev. C

AN UPDATED⁶Li(p, α)³He REACTION RATE AT ASTROPHYSICAL ENERGIES WITH THE TROJAN HORSE METHOD