Catálogo de publicaciones - revistas

<jats:title>Abstract</jats:title> <jats:p>The tension between the Hubble constant values obtained from local measurements and cosmic microwave background (CMB) measurements has motivated us to consider the cosmological model beyond ΛCDM. We investigate the cosmology in the large scale Lorentz violation model with a non-vanishing spatial curvature. The degeneracy among spatial curvature, cosmological constant, and cosmological contortion distribution makes the model viable in describing the known observational data. We obtain some constraints on the spatial curvature by comparing the relationship between measured distance modulus and red-shift with the predicted one, the evolution of matter density over time, and the evolution of effective cosmological constant. The implications of the large scale Lorentz violation model with the non-vanishing spatial curvature under these constrains are discussed.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>In this study, we investigate the shadow and photon sphere of the black bole in clouds of strings and quintessence with static and infalling spherical accretions. We obtain the geodesics of the photons near a black hole with different impact parameters <jats:italic>b</jats:italic> to investigate how the string cloud model and quintessence influence the specific intensity by altering the geodesic and the average radial position of photons. In addition, the range of the string cloud parameter <jats:italic>a</jats:italic> is constrained to ensure that a shadow can be observed. Moreover, the light sources in the accretion follow a normal distribution with an attenuation factor <jats:italic>γ</jats:italic>, and we adopt a model of the photon emissivity <jats:inline-formula> <jats:tex-math><?CDATA $ j(\nu_e) $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_6_065102_M1.jpg" xlink:type="simple" /> </jats:inline-formula> to obtain the specific intensities. Furthermore, the shadow with static spherical accretion is plotted, which demonstrates that the apparent shape of the shadow is a perfect circle, and the value of <jats:italic>γ</jats:italic> influences the brightness of the photon sphere. Subsequently, we investigate the profile and specific intensity of the shadows with static and infalling spherical accretions, respectively. The interior of the shadows with an infalling spherical accretion will be darker than that with the static spherical accretion, and the specific intensity with both static and infalling spherical accretions gradually converges. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>In this work, we study the optical properties of a class of magnetically charged rotating black hole spacetimes. The black holes in question are assumed to be immersed in the quintessence field, and subsequently, the resulting black hole shadows are expected to be modified by the presence of dark energy. We investigate the photon region and the black hole shadow, especially their dependence on the relevant physical conditions, such as the quintessence state parameter, angular momentum, and magnetic charge magnitude. The photon regions depend sensitively on the horizon structure and possess intricate features. Moreover, from the viewpoint of a static observer, we explore a few observables, especially those associated with the distortion of the observed black hole shadows.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>In this study, we determine the influence of the nucleon-nucleon short range correlation (SRC) on static spherically symmetric neutron stars (NSs) from the perspectives of radial and nonradial oscillations for the first time. We revise the equation of state and coupling parameters in the relativistic mean field theory after considering the SRC effect, and select the hyperon coupling parameters as the <jats:italic>SU</jats:italic>(3) model. For the non-radial oscillations, the SRC effect decreases the <jats:inline-formula> <jats:tex-math><?CDATA $ f $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_6_065104_M1.jpg" xlink:type="simple" /> </jats:inline-formula>-mode frequency by <jats:inline-formula> <jats:tex-math><?CDATA $ 0.2\sim0.3 $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_6_065104_M2.jpg" xlink:type="simple" /> </jats:inline-formula> kHz. For the radial oscillations, it decreases the fundamental radial frequency <jats:inline-formula> <jats:tex-math><?CDATA $ f_{1} $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_6_065104_M3.jpg" xlink:type="simple" /> </jats:inline-formula> by 0.75 ~ 0.85 kHz. Additionally, we refit the linear relationship between the average density and <jats:inline-formula> <jats:tex-math><?CDATA $ f $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_6_065104_M4.jpg" xlink:type="simple" /> </jats:inline-formula>-mode frequency for SRC. Combining the characteristics of the radial and non-radial frequencies, we provide a view of inferring the maximum mass of NSs. Owing to the characteristics of the SRC influence on the radial frequency, we expect that the SRC can be tested by future observation and can also be used as a probe for the structure inside NSs. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>New physics could be explored through loop effects by the precision measurements at the Circular Electron Positron Collider due to its clean collision environment and high luminosity. In this work, we focus on two dark matter models that involve additional electroweak fermionic multiplets. We calculate their one-loop corrections to five processes, i.e. $e^+e^- \to \mu^+\mu^-, ~Zh, ~ZZ, ~W^+W^-$, and $Z\gamma$, and investigate the corresponding signatures at CEPC with the projected sensitivity. We find that the detectable parameter regions of these processes are complementary. The combined analysis shows that the mass of dark matter $m_{\chi^0_1}$ in these two models can be probed up to $ \sim 150~\mathrm{GeV}$ and $\sim 450$ GeV at a 95\% confidence level, respectively. Content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Article funded by SCOAP3 and published under licence by Chinese Physical Society and the Institute of High Energy Physics of the Chinese Academy of Science and the Institute of Modern Physics of the Chinese Academy of Sciences and IOP Publishing Ltd.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>In this work, we construct a non-commutative gauge theory of the modified structure of the gravitational field using the Seiberg-Witten map and the general tetrad fields of Schwarzschild space-time, to show that the non-commutative geometry removes the singularity in the origin of the black hole, thus obtaining a non-singular Schwarzschild black hole. The geodetic structure of this black hole presents new types of motion next to the event horizon within stable orbits that are not allowed by the ordinary Schwarzschild spacetime. The noncommutative periastron advance of Mercury orbit are obtained, and with the available experimental data, we find a parameter of non-commutativity of order of 10−25 s.kg−1. This result shows that the new fundamental length √~ is of order 10−31 m.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>In this work, we have modified a scenario, originally proposed by Grimus and Lavoura, in order to obtain maximal values for atmospheric mixing angle and $CP$ violating Dirac phase of the lepton sector. To achieve this, we have employed $CP$ and some discrete symmetries in a type II seesaw model. In order to make predictions about neutrino mass ordering and the smallness of the reactor angle, we have obtained some conditions on the elements of the neutrino mass matrix of our model. Finally, within the framework of our model, we have studied quark masses and mixing pattern. Content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Article funded by SCOAP3 and published under licence by Chinese Physical Society and the Institute of High Energy Physics of the Chinese Academy of Science and the Institute of Modern Physics of the Chinese Academy of Sciences and IOP Publishing Ltd.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The properties of proto neutron star (PNS) PSR J0737-3039A is studied by using relativistic mean field theory. Five sets of nucleon coupling constants (DD-MEI, GL85, GL97, GM1 and NL2) are used. Using these five sets of nucleon coupling constants, the radius of the PNS PSR J0737-3039A is $R$=15.693-18.846 km, the central baryon density is $\rho_{c}$=0.247-0.359 fm$^{-3}$, the central energy density is $\varepsilon_{c}$=4.30$\times$10$^{14}$-6.49$\times$10$^{14}$ g.cm$^{-3}$, and the central pressure is $p_{c}$=3.79$\times$10$^{34}$-5.85$\times$10$^{34}$ dyne.cm$^{-2}$. For DD-MEI, GL85, GL97 and GM1, baryons octet all appear in the PNS PSR J0737-3039A. By NL2, only baryons n, p, $\Lambda$, $\Sigma^{0}$, $\Sigma^{-}$, $\Xi^{0}$ and $\Xi^{-}$ are present. Corresponding to the same baryon density, the relative densities of the same baryon in the PNS PSR J0737-3039A calculated from different nucleon coupling constants differ greatly. The central relative baryon densities of the PNS PSR J0737-3039A calculated by different nucleon coupling constants also differ greatly.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The energy dependence of the spectral fluctuations in the interacting boson model (IBM) and its connections to the mean-field structures have been analyzed through adopting two statistical measures, the nearest neighbor level spacing distribution $P(S)$ measuring the chaoticity (regularity) in energy spectra and the $\Delta_3(L)$ statistics of Dyson and Metha measuring the spectral rigidity. Specifically, the statistical results as functions of the energy cutoff have been worked out for different dynamical situations including the U(5)-SU(3) and SU(3)-O(6) transitions as well as those near the AW arc of regularity. It is found that most of the changes in spectral fluctuations are triggered near the stationary points of the classical potential especially for the cases in the deformed region of the IBM phase diagram. The results thus justify the stationary point effects from the point of view of statistics. In addition, the approximate degeneracies in the $2^+$ spectrum on the AW arc is also revealed from the statistical calculations.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We study the properties of the gravitational wave (GW) signals produced by first-order phase transitions during the inflation era. We show that the power spectrum of the GW oscillates with its wave number. This signal can be observed directly by future terrestrial and spatial gravitational wave detectors and through the B-mode spectrum in CMB. This oscillatory feature of GW is generic for any approximately instantaneous sources occurring during inflation and is distinct from the GW from phase transitions after the inflation. The details of the GW spectrum contain information about the scale of the phase transition and the later evolution of the universe.</jats:p>