Catálogo de publicaciones - revistas

<jats:title>Abstract</jats:title> <jats:p>Experimental elastic scattering angular distributions of <jats:sup>11</jats:sup>B, <jats:sup>12</jats:sup>C, and <jats:sup>16</jats:sup>O + heavy-ions are used to study the Woods-Saxon potential parameters. Best fitted values of the diffuseness parameters are found for each system, and a linear relationship is expressed between the diffuseness parameters and <jats:inline-formula> <jats:tex-math><?CDATA $A_1^{1/3}+A_2^{1/3}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054105_M1.jpg" xlink:type="simple" /> </jats:inline-formula> . The correlation of the potential depth and radius parameters with <jats:inline-formula> <jats:tex-math><?CDATA $A_1^{1/3}+A_2^{1/3}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054105_M2.jpg" xlink:type="simple" /> </jats:inline-formula> is also revealed within the limitations of the diffuseness parameter formula. Because the incident energies of most of the analyzed reactions are below or around the Coulomb barrier, the energy dispersion relation between the real and imaginary potentials is considered in order to investigate the ratio between the imaginary and real potential well depths, resulting in an expression of <jats:inline-formula> <jats:tex-math><?CDATA $W/V$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054105_M3.jpg" xlink:type="simple" /> </jats:inline-formula> . Within the limitation of the volume integrals calculated with the S <jats:inline-formula> <jats:tex-math><?CDATA $\tilde{a}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054105_M4.jpg" xlink:type="simple" /> </jats:inline-formula>o Paulo potential, parameterized formulas for the depth and radius parameters are obtained. The systematic Woods-Saxon potential parameters derived in the present work can reproduce not only the experimental data of elastic scattering angular distributions induced by <jats:sup>11</jats:sup>B, <jats:sup>12</jats:sup>C, and <jats:sup>16</jats:sup>O but also some elastic scattering induced by other heavy-ions. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>Several different transport processes, such as heat, momentum, and charge transports, may occur simultaneously in a thermal plasma system. The corresponding transport coefficients are heat conductivity, shear viscosity, and electric conductivity. In the present study, we investigate the color-electric conductivity of the quark-gluon plasma (QGP) in the presence of shear viscosity, focusing on the connection between the charge transport and momentum transport. To achieve this goal, we solve the viscous chromohydrodynamic equations obtained from the QGP kinetic theory associated with the distribution function modified by shear viscosity. According to the solved color fluctuations of hydrodynamic quantities, we obtain the induced color current through which the color-electric conductivity is derived. Numerical analysis shows that the conductivity properties of the QGP are mainly demonstrated by the longitudinal part of the color-electric conductivity. Shear viscosity has an appreciable impact on real and imaginary parts of the color-electric conductivity in some frequency regions.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Proton-halo breakup behavior in the <jats:inline-formula> <jats:tex-math><?CDATA $ \varepsilon_0\to 0 $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054107_M1.jpg" xlink:type="simple" /> </jats:inline-formula> limit (where <jats:inline-formula> <jats:tex-math><?CDATA $ \varepsilon_0 $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054107_M2.jpg" xlink:type="simple" /> </jats:inline-formula> is the ground-state binding energy) is studied around the Coulomb barrier in the <jats:inline-formula> <jats:tex-math><?CDATA $ ^8{\rm{B}}+{}^{58}{\rm{Ni}} $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054107_M3.jpg" xlink:type="simple" /> </jats:inline-formula> reaction for the first time. For practical purposes, apart from the experimental <jats:inline-formula> <jats:tex-math><?CDATA $ ^8{\rm{B}} $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054107_M4.jpg" xlink:type="simple" /> </jats:inline-formula> binding energy of 137 keV, three more arbitrarily chosen values (1, 0.1, 0.01 keV) are considered. It is first shown that the Coulomb barrier between the core and the proton prevents the <jats:inline-formula> <jats:tex-math><?CDATA $ ^7{\rm{Be}}+p $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054107_M5.jpg" xlink:type="simple" /> </jats:inline-formula> system from reaching the state of an open proton-halo system, which, among other factors, would require the ground-state wave function to extend to infinity in the asymptotic region, as <jats:inline-formula> <jats:tex-math><?CDATA $ \varepsilon_0\to 0 $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054107_M6.jpg" xlink:type="simple" /> </jats:inline-formula>. The elastic scattering cross section, which depends on the density of the ground-state wave function, is found to have a negligible dependence on the binding energy in this limit. The total, Coulomb and nuclear breakup cross sections are all reported to increase significantly from <jats:inline-formula> <jats:tex-math><?CDATA $ \varepsilon_0 = 137 $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054107_M7.jpg" xlink:type="simple" /> </jats:inline-formula> to 1.0 keV, and converge to their maximum values as <jats:inline-formula> <jats:tex-math><?CDATA $ \varepsilon_0\to 0 $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054107_M8.jpg" xlink:type="simple" /> </jats:inline-formula>. This increase is mainly understood as coming from a longer tail of the ground-state wave function for <jats:inline-formula> <jats:tex-math><?CDATA $ \varepsilon_0\leqslant 1.0 $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054107_M9.jpg" xlink:type="simple" /> </jats:inline-formula> keV, compared to that for <jats:inline-formula> <jats:tex-math><?CDATA $ \varepsilon_0 = 137 $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054107_M10.jpg" xlink:type="simple" /> </jats:inline-formula> keV. It is also found that the effect of the continuum-continuum couplings is to slightly delay the convergence of the breakup cross section. The analysis of the reaction cross section indicates a convergence of all the breakup observables as <jats:inline-formula> <jats:tex-math><?CDATA $ \varepsilon_0\to 0 $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_054107_M11.jpg" xlink:type="simple" /> </jats:inline-formula>. These results provide a better sense of the dependence of the breakup process on the breakup threshold. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>The effects of pre-equilibrium emission and secondary decay on the determination of the freeze-out volume are investigated using the isospin-dependent quantum molecular dynamics model accompanied by the statistical decay model GEMINI. Small-mass projectiles and large-mass targets with central collisions are studied at intermediate energies. It is revealed that the proton yields of pre-equilibrium emission are smaller than those of secondary decay. However, the determination of the freeze-out volume from the proton yields is more easily affected by pre-equilibrium emission. Moreover, the percentage of proton yields in the freeze-out stage is found to be approximately 50%.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Fission properties of the actinide nuclei are deduced from theoretical analysis. We investigate potential energy surfaces and fission barriers and predict the fission fragment mass yields of actinide isotopes. The results are compared with experimental data where available. The calculations were performed in the macroscopic-microscopic approximation with the Lublin-Strasbourg Drop (LSD) for the macroscopic part, and the microscopic energy corrections were evaluated in the Yukawa-folded potential. The Fourier nuclear shape parametrization is used to describe the nuclear shape, including the non-axial degree of freedom. The fission fragment mass yields of the nuclei considered are evaluated within a 3D collective model using the Born-Oppenheimer approximation.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The establishment of a possible connection between neutrino emission and gravitational-wave (GW) bursts is important to our understanding of the physical processes that occur when black holes or neutron stars merge. In the Daya Bay experiment, using the data collected from December 2011 to August 2017, a search was performed for electron-antineutrino signals that coincided with detected GW events, including GW150914, GW151012, GW151226, GW170104, GW170608, GW170814, and GW170817. We used three time windows of ±10, ±500, and ±1000 s relative to the occurrence of the GW events and a neutrino energy range of 1.8 to 100 MeV to search for correlated neutrino candidates. The detected electron-antineutrino candidates were consistent with the expected background rates for all the three time windows. Assuming monochromatic spectra, we found upper limits (90% confidence level) of the electron-antineutrino fluence of (1.13 − 2.44)×10<jats:sup>11</jats:sup> cm<jats:sup>−2</jats:sup> at 5 MeV to 8.0×10<jats:sup>7</jats:sup> cm<jats:sup>−2</jats:sup> at 100 MeV for the three time windows. Under the assumption of a Fermi-Dirac spectrum, the upper limits were found to be (5.4 − 7.0)×10<jats:sup>9</jats:sup> cm<jats:sup>−2</jats:sup> for the three time windows. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>Based on the Melnikov method, we investigate chaotic behaviors in the extended thermodynamic phase space for a slowly rotating Kerr-AdS black hole under temporal and spatial perturbations. Our results show that the temporal perturbation coming from a thermal quench of the spinodal region in the phase diagram may cause temporal chaos only when the perturbation amplitude is above a critical value, which involves the angular momentum <jats:italic>J</jats:italic>. Under the spatial perturbation, however, it is found that spatial chaos always occurs, independent of the perturbation amplitude. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>The collisional Penrose process of massive spinning particles in a rotational Einstein-Gauss-Bonnet (EGB) black hole background is studied. By numerically solving the equations of motion for spinning particles, we find that the energy extraction efficiency increases monotonically with the decrease of the EGB coupling parameter <jats:inline-formula> <jats:tex-math><?CDATA $ \alpha$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_055102_M1.jpg" xlink:type="simple" /> </jats:inline-formula>. Moreover, the efficiency <jats:inline-formula> <jats:tex-math><?CDATA $ \eta$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_055102_M2.jpg" xlink:type="simple" /> </jats:inline-formula> increases as the particle spin <jats:italic>s</jats:italic> grows. We also find that the energy extraction efficiency increases with the decrease of the EGB coupling parameter <jats:inline-formula> <jats:tex-math><?CDATA $ \alpha$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_055102_M3.jpg" xlink:type="simple" /> </jats:inline-formula>. When the EGB coupling constant <jats:inline-formula> <jats:tex-math><?CDATA $ \alpha=0$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_055102_M4.jpg" xlink:type="simple" /> </jats:inline-formula>, our results reduce to the Kerr case, which has been investigated previously. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>We derive an exact solution for a spherically symmetric Bardeen black hole surrounded by perfect fluid dark matter (PFDM). By treating the magnetic charge <jats:italic>g</jats:italic> and dark matter parameter <jats:inline-formula> <jats:tex-math><?CDATA $\alpha$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_055103_M1.jpg" xlink:type="simple" /> </jats:inline-formula> as thermodynamic variables, we find that the first law of thermodynamics and the corresponding Smarr formula are satisfied. The thermodynamic stability of the black hole is also studied. The results show that there exists a critical radius <jats:inline-formula> <jats:tex-math><?CDATA $r_{+}^{C}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_055103_M2.jpg" xlink:type="simple" /> </jats:inline-formula> where the heat capacity diverges, suggesting that the black hole is thermodynamically stable in the range <jats:inline-formula> <jats:tex-math><?CDATA $0\lt r_{+}\lt r_{+}^{C}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_055103_M3.jpg" xlink:type="simple" /> </jats:inline-formula>. In addition, the critical radius <jats:inline-formula> <jats:tex-math><?CDATA $r_{+}^{C}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_055103_M4.jpg" xlink:type="simple" /> </jats:inline-formula> increases with the magnetic charge <jats:italic>g</jats:italic> and decreases with the dark matter parameter <jats:inline-formula> <jats:tex-math><?CDATA $\alpha$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_055103_M5.jpg" xlink:type="simple" /> </jats:inline-formula>. Applying the Newman-Janis algorithm, we generalize the spherically symmetric solution to the corresponding rotating black hole. With the metric at hand, the horizons and ergospheres are studied. It turns out that for a fixed dark matter parameter <jats:inline-formula> <jats:tex-math><?CDATA $\alpha$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_055103_M6.jpg" xlink:type="simple" /> </jats:inline-formula>, in a certain range, with the increase of the rotation parameter <jats:italic>a</jats:italic> and magnetic charge <jats:italic>g</jats:italic>, the Cauchy horizon radius increases while the event horizon radius decreases. Finally, we investigate the energy extraction by the Penrose process in a rotating Bardeen black hole surrounded by PFDM. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>The phase state of dense matter in the intermediate density range ( <jats:inline-formula> <jats:tex-math><?CDATA $\sim$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_055104_M1.jpg" xlink:type="simple" /> </jats:inline-formula>1-10 times the nuclear saturation density) is both intriguing and unclear and can have important observable effects in the present gravitational wave era of neutron stars. As matter density increases in compact stars, the sound velocity is expected to approach the conformal limit ( <jats:inline-formula> <jats:tex-math><?CDATA $c_s/c=1/\sqrt{3}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_055104_M2.jpg" xlink:type="simple" /> </jats:inline-formula>) at high densities and should also fulfill the causality limit ( <jats:inline-formula> <jats:tex-math><?CDATA $c_s/c&lt;1$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_45_5_055104_M3.jpg" xlink:type="simple" /> </jats:inline-formula>). However, its detailed behavior remains a prominent topic of debate. It was suggested that the sound velocity of dense matter could be an important indicator of a deconfinement phase transition, where a particular shape might be expected for its density dependence. In this work, we explore the general properties of the sound velocity and the adiabatic index of dense matter in hybrid stars as well as in neutron stars and quark stars. Various conditions are employed for the hadron-quark phase transition with varying interface tension. We find that the expected behavior of the sound velocity can also be achieved by the nonperturbative properties of the quark phase, in addition to a deconfinement phase transition. Moreover, it leads to a more compact star with a similar mass. We then propose a new class of quark star equation of states, which can be tested by future high-precision radius measurements of pulsar-like objects. </jats:p>