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<jats:title>Abstract</jats:title> <jats:p>We investigate the effects of higher-order deformations <jats:inline-formula> <jats:tex-math><?CDATA $\beta_\lambda$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_2_024107_M1.jpg" xlink:type="simple" /> </jats:inline-formula> ( <jats:inline-formula> <jats:tex-math><?CDATA $\lambda=4,6,8,$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_2_024107_M2.jpg" xlink:type="simple" /> </jats:inline-formula> and 10) on the ground state properties of superheavy nuclei (SHN) near the doubly magic deformed nucleus <jats:inline-formula> <jats:tex-math><?CDATA $^{270}{\rm{Hs}}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_2_024107_M3.jpg" xlink:type="simple" /> </jats:inline-formula> using the multidimensionally-constrained relativistic mean-field (MDC-RMF) model with five effective interactions: PC-PK1, PK1, NL3<jats:sup>*</jats:sup>, DD-ME2, and PKDD. The doubly magic properties of <jats:inline-formula> <jats:tex-math><?CDATA $^{270}{\rm{Hs}}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_2_024107_M4.jpg" xlink:type="simple" /> </jats:inline-formula> include large energy gaps at <jats:inline-formula> <jats:tex-math><?CDATA $N=162$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_2_024107_M5.jpg" xlink:type="simple" /> </jats:inline-formula> and <jats:inline-formula> <jats:tex-math><?CDATA $Z=108$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_2_024107_M6.jpg" xlink:type="simple" /> </jats:inline-formula> in the single-particle spectra. By investigating the binding energies and single-particle levels of <jats:inline-formula> <jats:tex-math><?CDATA $^{270}{\rm{Hs}}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_2_024107_M7.jpg" xlink:type="simple" /> </jats:inline-formula> in the multidimensional deformation space, we find that, among these higher-order deformations, the deformation <jats:inline-formula> <jats:tex-math><?CDATA $\beta_6$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_2_024107_M8.jpg" xlink:type="simple" /> </jats:inline-formula> has the greatest impact on the binding energy and influences the shell gaps considerably. Similar conclusions hold for other SHN near <jats:inline-formula> <jats:tex-math><?CDATA $^{270}{\rm{Hs}}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_2_024107_M9.jpg" xlink:type="simple" /> </jats:inline-formula>. Our calculations demonstrate that the deformation <jats:inline-formula> <jats:tex-math><?CDATA $\beta_6$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_2_024107_M10.jpg" xlink:type="simple" /> </jats:inline-formula> must be considered when studying SHN using MDC-RMF. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>We investigate quantum kinetic theory for a massive fermion system under a rotational field. From the Dirac equation in rotating frame we derive the complete set of kinetic equations for the spin components of the 8- and 7-dimensional Wigner functions. While the particles are no longer on a mass shell in the general case due to the rotation–spin coupling, there are always only two independent components, which can be taken as the number and spin densities. With help from the off-shell constraint we obtain the closed transport equations for the two independent components in the classical limit and at the quantum level. The classical rotation–orbital coupling controls the dynamical evolution of the number density, but the quantum rotation–spin coupling explicitly changes the spin density.</jats:p>

<jats:title>Abstract</jats:title> <jats:p> <jats:inline-formula> <jats:tex-math><?CDATA $\eta N$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_2_024109_M1.jpg" xlink:type="simple" /> </jats:inline-formula> interactions are investigated in hot magnetized asymmetric nuclear matter using the chiral <jats:italic>SU</jats:italic>(3) model and chiral perturbation theory (ChPT). In the chiral model, the in-medium properties of <jats:italic>η</jats:italic>-mesons are calculated using medium modified scalar densities under the influence of an external magnetic field. Further, in a combined chiral model and ChPT approach, off-shell contributions of the <jats:inline-formula> <jats:tex-math><?CDATA $\eta N$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_2_024109_M2.jpg" xlink:type="simple" /> </jats:inline-formula> interactions are evaluated from the ChPT effective <jats:inline-formula> <jats:tex-math><?CDATA $\eta N$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_46_2_024109_M3.jpg" xlink:type="simple" /> </jats:inline-formula> Lagrangian, and the in-medium effect of scalar densities are incorporated from the chiral <jats:italic>SU</jats:italic>(3) model. We find that the magnetic field has a significant effect on the in-medium mass and optical potential of <jats:italic>η</jats:italic> mesons, and we observe a deeper mass-shift in the combined chiral model and ChPT approach than in the solo chiral <jats:italic>SU</jats:italic>(3) model. In both approaches, no additional mass-shift is observed due to the uncharged nature of <jats:italic>η</jats:italic> mesons in the presence of a magnetic field. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>In this study, we investigate the possibilities of generating baryon number asymmetry under thermal equilibrium within the frameworks of teleparallel and symmetric teleparallel gravities. Through the derivative couplings of the torsion scalar and the non-metricity scalar to baryons, baryon number asymmetry is produced in the radiation dominated epoch. For gravitational baryogenesis mechanisms in these two frameworks, the produced baryon-to-entropy ratio is too small to be consistent with observations. However, the gravitational leptogenesis models within both frameworks have the potential to explain the observed baryon-antibaryon asymmetry.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We develop the regular black hole solutions by incorporating the 1-loop quantum correction to the Newton potential and a time delay between an observer at the regular center and one at infinity. We define the maximal time delay between the center and the infinity by scanning the mass of black holes such that the sub-Planckian feature of the Kretschmann scalar curvature is preserved during the process of evaporation. We also compare the distinct behavior of the Kretschmann curvature for black holes with asymptotically Minkowski cores and those with asymptotically de-Sitter cores, including Bardeen and Hayward black holes. We expect that such regular black holes may provide more information about the construction of effective metrics for Planck stars.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The Large High Altitude Air Shower Observatory (LHAASO) (Fig. 1) is located at Mt. Haizi (4410 m a.s.l., 600 g/cm<jats:sup>2</jats:sup>, 29° 21’ 27.56” N, 100° 08’ 19.66” E) in Daocheng, Sichuan province, P.R. China. LHAASO consists of 1.3 km<jats:sup>2</jats:sup> array (KM2A) of electromagnetic particle detectors (ED) and muon detectors (MD), a water Cherenkov detector array (WCDA) with a total active area of 78,000 m<jats:sup>2</jats:sup>, 18 wide field-of-view air Cherenkov telescopes (WFCTA) and a newly proposed electron-neutron detector array (ENDA) covering 10,000 m<jats:sup>2</jats:sup>. Each detector is synchronized with all the other through a clock synchronization network based on the White Rabbit protocol. The observatory includes an IT center which comprises the data acquisition system and trigger system, the data analysis facility. In this Chapter, all the above-mentioned components of LHAASO as well as infrastructure are described. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>In the <jats:italic>γ</jats:italic>-ray sky, the highest fluxes come from Galactic sources: supernova remnants (SNRs), pulsars and pulsar wind nebulae, star forming regions, binaries and micro-quasars, giant molecular clouds, Galactic center, and the large extended area around the Galactic plane. The radiation mechanisms of <jats:italic>γ</jats:italic>-ray emission and the physics of the emitting particles, such as the origin, acceleration, and propagation, are of very high astrophysical significance. A variety of theoretical models have been suggested for the relevant physics, and emission with energies <jats:italic>E</jats:italic>≥10<jats:sup>14</jats:sup> eV are expected to be crucial in testing them. In particular, this energy band is a direct window to test at which maximum energy a particle can be accelerated in the Galactic sources and whether the most probable source candidates such as Galactic center and SNRs are “PeVatrons”. Designed aiming at the very high energy (VHE, &gt;100 GeV) observation, LHAASO will be a very powerful instrument in these astrophysical studies. Over the past decade, great advances have been made in the VHE <jats:italic>γ</jats:italic>-ray astronomy. More than 170 VHE <jats:italic>γ</jats:italic>-ray sources have been observed, and among them, 42 Galactic sources fall in the LHAASO field-of-view. With a sensitivity of 10 milli-Crab, LHAASO can not only provide accurate spectra for the known <jats:italic>γ</jats:italic>-ray sources, but also search for new TeV-PeV <jats:italic>γ</jats:italic>-ray sources. In the following sub-sections, the observation of all the Galactic sources with LHAASO will be discussed in details. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>Extra-galactic gamma-ray sources, such as gamma-ray bursts, active galactic nuclei, starburst galaxies, are interesting and important targets for LHAASO observations. In this chapter, the prospects of detecting these sources with LHAASO and their physical implications are studied. The upgrade plan for the Water Cherenkov Detector Array (WCDA), which aims to enhance the detectability of relatively lower energy photons, is also presented. In addition, a study on constraining the extragalactic background light with LHAASO observation of blazars is presented.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>In the first part of this Chapter the present state of knowledge from the observations of cosmic rays between 10<jats:sup>13</jats:sup> and 10<jats:sup>20</jats:sup> eV is summarized. This is not intended to be a complete review, but rather a broad overview of the relevant processes involving cosmic rays, including the astrophysical environments in which they take place. This overview mainly concerns experimental results and phenomenological aspects of their interpretation, therefore experiments’ description is not given but references to the vast bibliography are provided in the text. Some attempt is made to address the most popular explanations offered by theoretical models. The second part is devoted to the description of the LHAASO performance and of its capability to provide a response to several open questions, still unanswered, concerning cosmic rays above 10<jats:sup>13</jats:sup> eV, highlighting which major steps forward in this field could be taken from LHAASO observations. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>In order to reveal the nature of dark matter, it is crucial to detect its non-gravitational interactions with the standard model particles. The traditional dark matter searches focused on the so-called weakly interacting massive particles. However, this paradigm is strongly constrained by the null results of current experiments with high precision. Therefore there is a renewed interest of searches for heavy dark matter particles above TeV scale. The Large High Altitude Air Shower Observatory (LHAASO) with large effective area and strong background rejection power is very suitable to investigate the gamma-ray signals induced by dark matter annihilation or decay above TeV scale. In this document, we review the theoretical motivations and background of heavy dark matter. We review the prospects of searching for the gamma-ray signals resulted from dark matter in the dwarf spheroidal satellites and Galactic halo for LHAASO, and present the projected sensitivities. We also review the prospects of searching for the axion-like particles, which are a kind of well motivated light pseudo-scalars, through the LHAASO measurement of the very high energy gamma-ray spectra of astrophysical sources.</jats:p>