Catálogo de publicaciones - revistas

<jats:title>Abstract</jats:title> <jats:p>We studied the chiral magnetic effect in AuAu, RuRu, and ZrZr collisions at <jats:inline-formula> <jats:tex-math><?CDATA $\sqrt{s_{{NN}}}=200\;{\rm{GeV}}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094103_M1.jpg" xlink:type="simple" /> </jats:inline-formula>. The axial charge evolution was modeled with stochastic hydrodynamics, and geometrical quantities were calculated with the Monte Carlo Glauber model. By adjusting the relaxation time of the magnetic field, we found our results are in good agreement with background subtracted data for AuAu collisions at the same energy. We also made predictions for RuRu and ZrZr collisions. We found a weak centrality dependence on initial chiral imbalance, which implies that the centrality dependence of chiral magnetic effect signals results mainly from the effects of the magnetic field and volume factor. Furthermore, our results show an unexpected dependence on system size. While the AuAu system has larger chiral imbalance and magnetic field, it was observed to have a smaller signal for the chiral magnetic effect due to the larger volume suppression factor. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>The main purpose of this study is to interpret the possibilities of hybrid star configurations under different phase transition paths and provide a general description of the conditions and features of the different configurations. We assume that there are two possible phase transition paths, i.e., from a nuclear phase to a 2flavor(2f)/3flavor(3f) quark phase directly, or first from a nuclear phase to a 2f quark phase, and then from that phase to a 3f quark phase sequentially. In addition, we consider Maxwell and Gibbs constructions based on the assumption of a first-order transition, which yields multiple configurations of hybrid stars: N-2f, N-3f, and N-2f-3f for a Maxwell construction, and N-2fmix-2f, N-3fmix-3f, N-2f3fmix, and N-2fmix-3f for a Gibbs construction. From the radii analysis of different hybrid star configurations with the same mass of <jats:inline-formula> <jats:tex-math><?CDATA $1.95M_\odot$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094104_M1.jpg" xlink:type="simple" /> </jats:inline-formula>, the appearance of the quark matter (from nuclear to 2f or 3f quark matter) causes a radius difference of 0.5km~2km and provides the possibility of detection by NICER in the future. However, the sequential transition from 2f to 3f quark matter is difficult to detect because the transition does not lead to too high of a change in radius (far smaller than <jats:inline-formula> <jats:tex-math><?CDATA $0.5\; {\rm{km}}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094104_M3.jpg" xlink:type="simple" /> </jats:inline-formula>). The dependence solely on the measurements of the stellar radii to probe the equation of state of dense matter in neutron stars causes difficulties. Multi-messenger observations can help us to infer the interior of a neutron star in the future. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>Neutron–proton momentum correlation functions are constructed from a three-body photodisintegration channel, i.e., core+n+p, and used to explore the spatial-time information of the non-clustering Woods–Saxon spherical structure as well as the <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_44_9_094105_M2.jpg" xlink:type="simple" /> </jats:inline-formula>-clustering structures of <jats:inline-formula> <jats:tex-math><?CDATA $^{12}{\rm{C}}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094105_M3.jpg" xlink:type="simple" /> </jats:inline-formula> or <jats:inline-formula> <jats:tex-math><?CDATA $^{16}{\rm{O}}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094105_M4.jpg" xlink:type="simple" /> </jats:inline-formula> based on an extended quantum molecular dynamics model. The emission time sequence of neutrons and protons is indicated by the ratio of velocity-gated neutron–proton correlation functions, demonstrating its sensitivity to <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_44_9_094105_M5.jpg" xlink:type="simple" /> </jats:inline-formula>-clustering structures. This work sheds light on a new probe for <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_44_9_094105_M6.jpg" xlink:type="simple" /> </jats:inline-formula>-clustering structures. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>In this study, we systematically investigate the <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_44_9_094106_M4.jpg" xlink:type="simple" /> </jats:inline-formula> decay preformation factors, <jats:inline-formula> <jats:tex-math><?CDATA $P_{\alpha}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094106_M5.jpg" xlink:type="simple" /> </jats:inline-formula>, and the <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_44_9_094106_M6.jpg" xlink:type="simple" /> </jats:inline-formula> decay half-lives of 152 nuclei around <jats:italic>Z</jats:italic> = 82, <jats:italic>N</jats:italic> = 126 closed shells based on the generalized liquid drop model (GLDM) with <jats:inline-formula> <jats:tex-math><?CDATA $P_{\alpha}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094106_M7.jpg" xlink:type="simple" /> </jats:inline-formula> being extracted from the ratio of the calculated <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_44_9_094106_M8.jpg" xlink:type="simple" /> </jats:inline-formula> decay half-life to the experimental one. The results show that there is a remarkable linear relationship between <jats:inline-formula> <jats:tex-math><?CDATA $P_{\alpha}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094106_M9.jpg" xlink:type="simple" /> </jats:inline-formula> and the product of valance protons (holes) <jats:inline-formula> <jats:tex-math><?CDATA $N_p$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094106_M10.jpg" xlink:type="simple" /> </jats:inline-formula> and valance neutrons (holes) <jats:inline-formula> <jats:tex-math><?CDATA $N_n$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094106_M11.jpg" xlink:type="simple" /> </jats:inline-formula>. At the same time, we extract the <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_44_9_094106_M12.jpg" xlink:type="simple" /> </jats:inline-formula> decay preformation factor values of the even–even nuclei around the <jats:italic>Z</jats:italic> = 82, <jats:italic>N</jats:italic> = 126 closed shells from the study of Sun <jats:inline-formula> <jats:tex-math><?CDATA ${et\ al.}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094106_M13.jpg" xlink:type="simple" /> </jats:inline-formula> [J. Phys. G: Nucl. Part. Phys., <jats:bold>45</jats:bold>: 075106 (2018)], in which the <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_44_9_094106_M14.jpg" xlink:type="simple" /> </jats:inline-formula> decay was calculated by two different microscopic formulas. We find that the <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_44_9_094106_M15.jpg" xlink:type="simple" /> </jats:inline-formula> decay preformation factors are also related to <jats:inline-formula> <jats:tex-math><?CDATA $N_pN_n$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094106_M16.jpg" xlink:type="simple" /> </jats:inline-formula>. Combining with our previous studies [Sun <jats:inline-formula> <jats:tex-math><?CDATA ${et\ al.}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094106_M17.jpg" xlink:type="simple" /> </jats:inline-formula>, Phys. Rev. C, <jats:bold>94</jats:bold>: 024338 (2016); Deng <jats:inline-formula> <jats:tex-math><?CDATA ${et\ al.}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094106_M18.jpg" xlink:type="simple" /> </jats:inline-formula>, ibid. <jats:bold>96</jats:bold>: 024318 (2017); Deng <jats:inline-formula> <jats:tex-math><?CDATA ${et\ al.}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094106_M19.jpg" xlink:type="simple" /> </jats:inline-formula>, ibid. <jats:bold>97</jats:bold>: 044322 (2018)] and that of Seif <jats:inline-formula> <jats:tex-math><?CDATA ${et\ al.,}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_9_094106_M20.jpg" xlink:type="simple" /> </jats:inline-formula> [Phys. Rev. C, <jats:bold>84</jats:bold>: 064608 (2011)], we suspect that this phenomenon of linear relationship for the nuclei around the above closed shells is model-independent. This may be caused by the effect of the valence protons (holes) and valence neutrons (holes) around the shell closures. Finally, using the formula obtained by fitting the <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_44_9_094106_M21.jpg" xlink:type="simple" /> </jats:inline-formula> decay preformation factor data calculated by the GLDM, we calculate the <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_44_9_094106_M22.jpg" xlink:type="simple" /> </jats:inline-formula> decay half-lives of these nuclei. The calculated results agree with the experimental data well. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>Inspired by the availability of recent experimental as well as theoretical data on the energy levels of odd-mass <jats:sup>151-161</jats:sup>Pm and odd-odd <jats:sup>154,156</jats:sup>Pm, we applied the theoretical framework of the projected shell model to further understand the nuclear structure of these nuclei. The calculations closely reproduced the experimental data reported for the yrast bands of these isotopes by assuming an axial (prolate) deformation of ~0.3. Other properties along the yrast line, such as transition energies and transition probabilities, have also been discussed. Band diagrams are plotted to understand their intrinsic multi-quasiparticle structure, which turn out to be dominated by 1-quasiparticle bands for the odd-mass Pm isotopes and 2-quasiparticle bands for the doubly-odd Pm isotopes under study. The present study not only confirms the recently reported experimental/theoretical data, but also extends the already available information on the energy levels and adds new information regarding the reduced transition probabilities. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>In this work, we have performed Skyrme density functional theory (DFT) calculations of nuclei around <jats:sup>132</jats:sup>Sn to study whether the abnormal odd-even staggering (OES) behavior of binding energies around <jats:italic>N</jats:italic> = 82 can be reproduced. With the Skyrme forces SLy4 and SkM*, we tested the volume- and surface-type pairing forces and also the intermediate between these two pairing forces, in the Hartree-Fock-Bogoliubov (HFB) approximation with or without the Lipkin-Nogami (LN) approximation or particle number projection after the convergence of HFBLN (PLN). The Universal Nuclear Energy Density Function (UNEDF) parameter sets are also used. The trend of the neutron OES against the neutron number or proton number does not change significantly by tuning the density dependence of the pairing force. Moreover, for the pairing force that is favored more at the nuclear surface, a larger mass OES is obtained, and vice versa. It appears that the combination of volume and surface pairing can give better agreement with the data. In the studies of the OES, a larger ratio of surface to volume pairing might be favored. Additionally, in most cases, the OES given by the HFBLN approximation agrees more closely with the experimental data. We found that both the Skyrme and pairing forces can influence the OES behavior. The mass OES calculated by the UNEDF DFT is explicitly smaller than the experimental one. The UNEDF1 and UNEDF2 forces can reproduce the experimental trend of the abnormal OES around <jats:sup>132</jats:sup>Sn. The neutron OES of the tin isotopes given by the SkM* force agrees more closely with the experimental one than that given by the SLy4 force in most cases. Both SLy4 and SkM* DFT have difficulties in reproducing the abnormal OES around <jats:sup>132</jats:sup>Sn. Using the PLN method, the systematics of OES are improved for several combinations of Skyrme and pairing forces. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>In this study, the scenario of a two-component warm tachyon inflation is considered, where the tachyon field plays the role of the inflaton by driving the inflation. During inflation, the tachyon scalar field interacts with the other component of the Universe, which is assumed to be photon gas, i.e., radiation. The interacting term contains a dissipation coefficient, and the study is modeled based on two different and familiar choices of the coefficient that were studied in the literature. By employing the latest observational data, the acceptable ranges for the free parameters of the model are obtained. For any choice within the estimated ranges, there is an acceptable concordance between the theoretical predictions and observations. Although the model is established based on several assumptions, it is crucial to verify their validity for the obtained values of the free parameters of the model. It is found that the model is not self-consistent for all values of the ranges, and for some cases, the assumptions are violated. Therefore, to achieve both self-consistency and agreement with the data, the parameters of the model must be constrained. Subsequently, we consider the recently proposed swampland conjecture, which imposes two conditions on the inflationary models. These criteria rule out some inflationary models; however, warm inflation is among those that successfully satisfy the swampland criteria. We conduct a precise investigation, which indicates that the proposed warm tachyon inflation cannot satisfy the swampland criteria for some cases. In fact, for the first case of the dissipation coefficient, in which, there is dependency only on the scalar field, the model agrees with observational data. However, it is in direct tension with the swampland criteria. Nevertheless, for the second case, wherein the dissipation coefficient has a dependency on both the scalar field and temperature, the model exhibits acceptable agreement with observational data, and suitably satisfies the swampland criteria.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Quasinormal modes (QNMs) for massless and massive Dirac perturbations of Born-Infeld black holes (BHs) in higher dimensions are investigated. Solving the corresponding master equation in accordance with hypergeometric functions and the QNMs are evaluated. We discuss the relationships between QNM frequencies and spacetime dimensions. Meanwhile, we also discuss the stability of the Born-Infeld BH by calculating the temporal evolution of the perturbation field. Both the perturbation frequencies and the decay rate increase with increasing dimension of spacetime <jats:italic>n</jats:italic>. This shows that the Born-Infeld BHs become more and more unstable at higher dimensions. Furthermore, the traditional finite difference method is improved, so that it can be used to calculate the massive Dirac field. We also elucidate the dynamic evolution of Born-Infeld BHs in a massive Dirac field. Because the number of extra dimensions is related to the string scale, there is a relationship between the spacetime dimension <jats:italic>n</jats:italic> and the properties of Born-Infeld BHs that might be advantageous for the development of extra-dimensional brane worlds and string theory. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>Banerjee-Ghosh's work shows that the singularity problem can be naturally avoided by the fact that black hole evaporation stops when the remnant mass is greater than the critical mass when including the generalized uncertainty principle (GUP) effects with first- and second-order corrections. In this paper, we first follow their steps to reexamine Banerjee-Ghosh's work, but we find an interesting result: the remnant mass is always equal to the critical mass at the final stage of black hole evaporation with the inclusion of the GUP effects. Then, we use Hossenfelder's GUP, i.e., another GUP model with higher-order corrections, to restudy the final evolution behavior of the black hole evaporation, and we confirm the intrinsic self-consistency between the black hole remnant and critical masses once more. In both cases, we also find that the thermodynamic quantities are not singular at the final stage of black hole evaporation.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We study adiabatic regularization of a coupling massless scalar field in general spatially flat Robertson-Walker (RW) spacetimes. For the conformal coupling, the 2nd-order regularized power spectrum and 4th-order regularized stress tensor are zero, and no trace anomaly exists in general RW spacetimes. This is a new result that exceeds those found in de Sitter space. For the minimal coupling, the regularized spectra are also zero in the radiation-dominant and matter-dominant stages, as well as in de Sitter space. The vanishing of these adiabatically regularized spectra is further confirmed by direct regularization of the Green's function. For a general coupling and general RW spacetimes, the regularized spectra can be negative under the conventional prescription. At a higher order of regularization, the spectra will generally become positive, but will also acquire IR divergence, which is inevitable for a massless field. To avoid the IR divergence, the inside-horizon regularization is applied. Through these procedures, nonnegative UV- and IR-convergent power spectrum and spectral energy density will eventually be achieved.</jats:p>