Current quests in nucleosynthesis: present and future neutron-induced reaction measurements

Praena, J.; Pignatari, M.; Mastinu, P.; Martín-Hernández, Guido; Prete, G.; Quesada, J. M.; Sabaté-Gilarte, M.

doi:10.1051/epjconf/20146607022

Cited by 3 publications

(1 citation statement)

References 34 publications

(47 reference statements)

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“…The behavior of particles inside compact stars like white dwarfs, formed by matter with density lower than the nuclear density, can be experimentally reproduced in some cases by means of nuclear accelerators [1,2]. In adittion, complementary theoretical models that help describing the interactions in the interior of compact stars, even for low energy interactions, the dynamics can be explored as well through general relativity or non relativistic effective theories [3,4].…”

Section: Introductionmentioning

confidence: 99%

A model for low mass compact objects

Estevez-Delgado

Paulin-Fuentes

et al. 2019

Rev. Mex. Fís.

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A model for low mass compact objects with compactness ratio $u\leq 0.06092997016$ is presented here. Density, pressure and sound speed are regular and monotonic decreasing functions. The change between the central density $\rho_c$ and the density on the surface $\rho_b$ is lower than $3.94\%$ and the maximum change occurs for the biggest compactness, i.e. $\rho_c=1.039350237\rho_b$. This allows us to apply this model for the case of compact stars in which the density variation is very small. In particular, we can use this model for PSR B0943 + 10, a quark star candidate, with radius $R=2.6{\rm Km}$ and mass $M=0.2 M_\odot$. According to our model it comes out that the density on the surface is $\rho_b=5.388074 \times 10^{17} Kg/m^3$ and its central density $\rho_c=1.007150 \rho_b$ is slightly bigger than the surface density and larger than the nuclear density.

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Section: Introductionmentioning

confidence: 99%

A model for low mass compact objects

Estevez-Delgado

Paulin-Fuentes

et al. 2019

Rev. Mex. Fís.

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Production and measurement of a stellar neutron spectrum at 30 keV

Praena,

Verdera,

López

et al. 2024

Eur. Phys. J. A

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A few years ago, we theoretically studied the production of a stellar neutron spectrum at kT = 30 keV using a shaped proton beam impinging on a thick lithium target. Here, we first measure the proton distribution to better control the produced neutron spectrum. Then, we measure the forward-emitted angle-integrated neutron spectrum of the 7Li(p,n)7Be reaction via time-of-flight neutron spectrometry with such proton distribution. The result resembles a stellar neutron spectrum at kT = 30 keV. This method avoids in activation experiments the need for spectrum correction. In the case of spherical samples, no knowledge of the cross-section of the isotope being measured by activation would be necessary. Therefore, the present method is of interest for isotopes with unknown or poorly known cross-sections, such as branching points in astrophysics. The key point of our method is the experimental control of the proton distribution that impinges on the lithium target.

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An interior solution with perfect fluid

et al. 2020

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Starting from the construction of a solution for Einstein’s equations with a perfect fluid for a static spherically symmetric spacetime, we present a model for stars with a compactness rate of [Formula: see text]. The model is physically acceptable, that is to say, its geometry is non-singular and does not have an event horizon, pressure and speed of sound are bounded functions, positive and monotonically decreasing as function of the radial coordinate, also the speed of sound is lower than the speed of light. While it is shown that the adiabatic index [Formula: see text], which guarantees the stability of the solution. In a complementary manner, numerical data are presented considering the star PSR J0737-3039A with observational mass of [Formula: see text], for the value of compactness [Formula: see text], which implies the radius [Formula: see text] and the range of the density [Formula: see text] [Formula: see text], where [Formula: see text] and [Formula: see text] are the central density and the surface density, respectively. This range is consistent with the expected values; as such, the model presented allows to describe this type of stars.

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Current quests in nucleosynthesis: present and future neutron-induced reaction measurements

Cited by 3 publications

References 34 publications

A model for low mass compact objects

A model for low mass compact objects

Production and measurement of a stellar neutron spectrum at 30 keV

An interior solution with perfect fluid

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