Catálogo de publicaciones - revistas

<jats:title>Abstract</jats:title> <jats:p>The properties of strange quark matter and the structures of (proto-)strange stars are studied within the framework of a baryon density-dependent quark mass model, where a novel quark mass scaling and self-consistent thermodynamic treatment are adopted. Our results indicate that the perturbative interaction has a significant impact on the properties of strange quark matter. It is determined that the energy per baryon increases with temperature, while the free energy decreases and eventually becomes negative. At fixed temperatures, the pressure at the minimum free energy per baryon is zero, suggesting that the thermodynamic self-consistency is preserved. Furthermore, the sound velocity <jats:italic>v</jats:italic> in quark matter approaches the extreme relativistic limit ( <jats:inline-formula> <jats:tex-math><?CDATA $ c/\sqrt{3} $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_5_055102_M2.jpg" xlink:type="simple" /> </jats:inline-formula>) as the density increases. By increasing the strengths of the confinement parameter <jats:italic>D</jats:italic> and perturbation parameter <jats:italic>C</jats:italic>, the tendency for <jats:italic>v</jats:italic> to approach the extreme relativistic limit at high density is slightly weakened. For (proto-)strange stars, the novel quark mass scaling can accommodate massive proto-strange stars with their maximum mass surpassing twice the solar mass by considering the isentropic stages along the star evolution line, where the entropy per baryon of the star matter is set to be 0.5 and 1 with the lepton fraction <jats:inline-formula> <jats:tex-math><?CDATA $ Y_{l} $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_5_055102_M6.jpg" xlink:type="simple" /> </jats:inline-formula> = 0.4. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>The measurement of gravitational waves produced by binary black-hole mergers at the Advanced LIGO has encouraged extensive studies on the stochastic gravitational wave background. Recent studies have focused on gravitational wave sources made of the same species, such as mergers from binary primordial black holes or those from binary astrophysical black holes. In this paper, we study a new possibility – the stochastic gravitational wave background produced by mergers of one primordial black hole and one astrophysical black hole. Such systems are necessarily present if primordial black holes exist. We study the isotropic gravitational wave background produced through the history of the universe. We find it is very challenging to detect such a signal. We also demonstrate that it is improper to treat the gravitational waves produced by such binaries in the Milky Way as a directional stochastic background due to a very low binary formation rate.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Understanding the thermodynamic phase transition of black holes can provide deep insights into the fundamental properties of black hole gravity and help to establish quantum gravity. In this work, we investigate the phase transition and its dynamics for the charged EPYM AdS black hole. Through reconstructing Maxwell's equal-area law, we find there exists a high-/low-potential black hole (HPBH/LPBL) phase transition, not only the pure large/small black hole phase transition. The Gibbs free energy landscape ( <jats:inline-formula> <jats:tex-math><?CDATA $ G_{\rm L} $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_5_055104_M1.jpg" xlink:type="simple" /> </jats:inline-formula>) is treated as a function of the black hole horizon, which is the order parameter of the phase transition due to thermal fluctuation. From the viewpoint of <jats:inline-formula> <jats:tex-math><?CDATA $ G_{\rm L} $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_5_055104_M2.jpg" xlink:type="simple" /> </jats:inline-formula>, the stable HPBH/LPBL states correspond to two wells of <jats:inline-formula> <jats:tex-math><?CDATA $ G_{\rm L} $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_5_055104_M3.jpg" xlink:type="simple" /> </jats:inline-formula>, which have the same depth. The unstable intermediate-potential black hole state corresponds to the local maximum of <jats:inline-formula> <jats:tex-math><?CDATA $ G_{\rm L} $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_5_055104_M4.jpg" xlink:type="simple" /> </jats:inline-formula>. Then we focus on the probability evolution governed by the Fokker–Planck equation. Through solving the Fokker–Planck equation with different reflection/absorption boundary conditions and initial conditions, the dynamics of switching between the coexistent HPBH and LPBL phases is probed within the first passage time. Furthermore, the effect of temperature on the dynamic properties of the phase transition is also investigated. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>The extensivity for the thermodynamics of general <jats:italic>D</jats:italic>-dimensional rotating black holes with or without a cosmological constant can be proved analytically, provided that the effective number of microscopic degrees of freedom and the chemical potential are given respectively as <jats:inline-formula> <jats:tex-math><?CDATA $ N = L^{D-2}/G,\; \mu = GTI_D/L^{D-2} $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_5_055105_M1.jpg" xlink:type="simple" /> </jats:inline-formula>, where <jats:italic>G</jats:italic> is the variable Newton constant, <jats:inline-formula> <jats:tex-math><?CDATA $ I_D $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_5_055105_M2.jpg" xlink:type="simple" /> </jats:inline-formula> is the Euclidean action, and <jats:italic>L</jats:italic> is a constant length scale. In the cases without a cosmological constant, i.e., the Myers-Perry black holes, the physical mass and the intensive variables can be expressed as explicit macro state functions in the extensive variables in a simple and compact form, which allows for an analytical calculation of the heat capacity. The results indicate that the Myers-Perry black holes with zero, one, and <jats:italic>k</jats:italic> equal rotation parameters are all thermodynamically unstable. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>The binding energies and proton separation energies of nuclides with $Z, N = 30-50$ \textcolor{blue}{are investigated,} based on the shell model with an uncertainty analysis through statistical methods. Several formulas are used to obtain the binding energies and proton separation energies according to the shell-model calculations. The non-parametric Bootstrap method is applied to establish an uncertainty decomposition and recomposition framework. Moreover, it \textcolor{blue}{is used to estimate the stability of proton(s) emission} for each nuclide. Two formulas for calculating the binding energies with a systematic uncertainty of $\sim0.3$ MeV are proposed, and a reliable extrapolation ability is examined. These binding energy formulas deduce similar forms of respective $S_{p}$ and $S_{2p}$ energies, which predict the extension of the nuclear boundary of this region. A nice description of the binding energies and proton separation energies is provided. \textcolor{blue}{The one- and two-proton separation energies and partial half-lives of proton emitting are predicted, thus showing a new dripline.} Besides, there are 30 unstable nuclides predicted to be bound against proton(s)-emission. These nuclear properties will be useful in nuclear astrophysics.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The collinearly-improved Balitsky-Kovchegov (ciBK) equation evolved unintegrated gluon distribution (UGD) is used, for the first time, to study the hadron productions in high energy proton-proton collisions in order to improve the predictive power of the Color Glass Condensate effective theory. We show that the ciBK equation evolved UGD provides a relatively better description of the LHC data on the transverse momentum and integrated multiplicity distributions of charged hadron and neutral pion productions for several collision energies, as compared to the running coupling Balitsky-Kovchegov (rcBK) equation evolved UGD, since the ciBK evolved UGD has a sharper transverse momentum distribution than the rcBK one. The impact of running coupling prescriptions on hadron productions are studied. It shows that the parent dipole and smallest dipole running coupling prescriptions give a similar depiction of the data. Moreover, the scale dependence of the fragmentation function is investigated by taking three typical values of scale. We find that the differences resulting from the scale dependence of the fragmentation function can be fully absorbed into the normalization factor which lumps higher order corrections.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The positive-parity signature partner bands in <jats:sup>103,105</jats:sup>Pd and <jats:sup>109</jats:sup>Cd nuclei are investigated by the semiclassical particle-rotor model. Based on the systematic study of neighbouring nuclei, the signature partner bands of <jats:sup>105</jats:sup>Pd are assigned to the π(g<jats:sub>9/2</jats:sub> <jats:sup>-4</jats:sup>)ν(g<jats:sub>7/2</jats:sub>h<jats:sub>11/2</jats:sub> <jats:sup>2</jats:sup>) configuration, and this assignment is also supported by the present calculations. Meanwhile the calculated B(E2) values of such bands of <jats:sup>105</jats:sup>Pd reproduce the experimental values well and exhibit decreasing behavior with increasing angular momentum, suggesting that these two bands may originate from antimagnetic rotation. Similar signature partner bands were also found in neighboring <jats:sup>103</jats:sup>Pd and <jats:sup>109</jats:sup>Cd nuclei. The properties of both bands show general agreement with the fingerprints of antimagnetic rotation, and thus the signature partner bands of <jats:sup>103</jats:sup>Pd and <jats:sup>109</jats:sup>Cd are suggested to be candidates for multiple antimagnetic rotational bands as that of <jats:sup>105</jats:sup>Pd. In addition, the evolution of the two-shears-like mechanism for possible multiple antimagnetic rotational bands in <jats:sup>103,105</jats:sup>Pd and <jats:sup>109</jats:sup>Cd nuclei is examined by investigating the orientation of the angular momenta.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The dependence of the black hole (BH) shadow and thermodynamics may be structured in the regular spacetime. Taking the regular Bardeen-AdS BH as an example, the relationship between the shadow radius and the event horizon radius is derived. It is found that these two radii display a positive correlation, implying that the BH temperature can be rewritten as a function of shadow radius in the regular spacetime. By analyzing the phase transition curves under the shadow context, we found that the shadow radius can replace the event horizon radius to present the BH phase transition process, and the phase transition grade can also be revealed by the shadow radius, indicating that the shadow radius may serve as a probe for the phase structure in the regular spacetime. Utilizing the temperature-shadow radius function, the thermal profile of the Bardeen-AdS BH is established. We obtained that the temperature shows an N-type change trend in $P&lt;P_{\rm c}$ situation. These results suggest that the phase transition process of the regular AdS BH can be completely presented in the thermal profile, and the relationship between the BH shadow and thermodynamics can also be established in the regular spacetime.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>One of the fundamental issues in cosmic ray physics is to explain the nature of cosmic ray acceleration and propagation mechanisms. Thanks to the precise cosmic ray data measured by recent space experiments, we are able to investigate the cosmic ray acceleration and propagation models more comprehensively and reliably. In this paper, we combine the secondary-to-primary ratios and the primary spectra measured by PAMELA, AMS02, ACE-CRIS and Voyager-1 to constrain the cosmic ray source and transport parameters. The study shows that the $Z&gt;2$ data yield a medium-energy diffusion slope $\delta_{2}\sim\left(0.42, 0.48\right)$ and a high-energy slope $\delta_{3}\sim\left(0.22, 0.34\right)$. The $Z\leq2$ species obtain a looser constraint on $\delta_{2}\sim\left(0.38, 0.47\right)$, but a tighter constraint on $\delta_{3}\sim\left(0.21, 0.30\right)$. The overlaps infer that the heavy and light particles can give compatible results at medium to high energies. Besides, both the light and heavy nuclei indicate a consistent diffusion slope variation $\Delta\delta_{H}$ around $200\sim300$~GV. At low energies, significant disagreements exist between the heavy and light elements. The B/C ratio requires a much larger diffusion slope shift $\Delta\delta_{L}$ around 4 GV or a stronger \textit{Alfv$\acute{e}$n velocity} $v_{A}$ than the low-mass data. This indicates that the heavy and light particles may suffer different low-energy transport behaviors in Galaxy. However, better understanding on the consistency/inconsistency between the heavy and light cosmic rays relies on more precise cross-sections, better constraints on correlations in systematic errors of data, more accurate estimation on Galaxy halo size and more robust description for Solar modulation during the reversal period of HMF.</jats:p>