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<jats:title>Abstract</jats:title> <jats:p>We discuss the <jats:inline-formula> <jats:tex-math><?CDATA $P-V$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_6_065105_M1.jpg" xlink:type="simple" /> </jats:inline-formula> criticality and the Joule-Thomson expansion of charged AdS black holes in the Rastall gravity. We find that although the equation-of-state of a charged AdS black hole in the Rastall gravity is related to the Rastall parameter <jats:inline-formula> <jats:tex-math><?CDATA $\lambda$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_6_065105_M2.jpg" xlink:type="simple" /> </jats:inline-formula>, its reduced equation-of-state at the critical point is independent of the Rastall parameter <jats:inline-formula> <jats:tex-math><?CDATA $\lambda$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_6_065105_M3.jpg" xlink:type="simple" /> </jats:inline-formula>, as is the case in the Einstein gravity where <jats:inline-formula> <jats:tex-math><?CDATA $\lambda=0$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_6_065105_M4.jpg" xlink:type="simple" /> </jats:inline-formula>. This is the reason why the critical exponents are not related to the Rastall parameter <jats:inline-formula> <jats:tex-math><?CDATA $\lambda$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_6_065105_M5.jpg" xlink:type="simple" /> </jats:inline-formula>. We also find that the inversion temperature <jats:inline-formula> <jats:tex-math><?CDATA ${T_{i}}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_6_065105_M6.jpg" xlink:type="simple" /> </jats:inline-formula> is related to the Rastall parameter <jats:inline-formula> <jats:tex-math><?CDATA $\lambda$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_6_065105_M7.jpg" xlink:type="simple" /> </jats:inline-formula>, but that the minimum inversion temperature <jats:inline-formula> <jats:tex-math><?CDATA ${T_{i}}^{\rm min}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_6_065105_M8.jpg" xlink:type="simple" /> </jats:inline-formula> and the ratio <jats:inline-formula> <jats:tex-math><?CDATA $\varepsilon$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_6_065105_M9.jpg" xlink:type="simple" /> </jats:inline-formula> between the minimum inversion temperature and the critical temperature are both independent of the Rastall parameter <jats:inline-formula> <jats:tex-math><?CDATA $\lambda$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_6_065105_M10.jpg" xlink:type="simple" /> </jats:inline-formula>. At the critical point, the thermodynamic evolution of a charged AdS black hole in the Rastall gravity behaves as in the van der Waals fluid and charged AdS black hole in the Einstein gravity. We show the inversion curves and isenthalpic curves in the <jats:inline-formula> <jats:tex-math><?CDATA $T-P$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_6_065105_M11.jpg" xlink:type="simple" /> </jats:inline-formula> plane and analyze the effect of the Rastall constant <jats:inline-formula> <jats:tex-math><?CDATA $\lambda$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_6_065105_M12.jpg" xlink:type="simple" /> </jats:inline-formula> on the inversion curves of a charged AdS black hole during the Joule-Thomson expansion. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>We study matter accretion onto Einstein-aether black holes by adopting the Hamiltonian approach. The general solution of accretion is discussed using the isothermal equation of state. Different types of fluids are considered, including ultra-relativistic, ultra-stiff, sub-relativistic, and radiation fluids, and the accretion process onto Einstein-aether black holes is analyzed. The behavior of the fluid flow and the existence of critical points is investigated for Einstein-aether black holes. We further discuss the general expression and behavior of polytropic fluid onto Einstein-aether black holes. The most important feature of this work is the investigation of the mass accretion rate of the above-mentioned fluids and the comparison of our findings with the Schwarzschild black hole, which generates particular signatures. Moreover, the maximum mass accretion rate occurs near the Killing and universal horizons, and the minimum accretion rate lies between them.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present a model for tail wavelets, a phenomenon known as “echo” in the literature. The tail wavelet may appear in signal reconnaissances in the merger of binary compact objects, including black holes and neutron stars. We show that the dark matter surrounding the compact objects lead to a speculated tail wavelet following the main gravitational wave (GW). We demonstrate that the radiation pressure of the main wave is fully capable of pushing away the surrounding matter to some altitude, and splashing down of the matter excites the tail wavelet after ringing down of the main wave. We illustrate this concept in a simplified model, where numerical estimations are conducted on the specific distribution of dark matter outside the black hole horizon and the threshold values in accordance with observations. We study the full back reaction of the surrounding dark matter to the metric and find that the effect on to the tail wavelets is insignificant. We reveal the fine difference between the tail wavelets of a dressed and a bare black hole. We demonstrate that the tail wavelet can appear as a natural phenomenon in the frame of general relativity, without invoking modified gravities or quantum effects.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Pion-mass-dependent nucleon-nucleon (<jats:italic>NN</jats:italic>) potentials are obtained in terms of the one-pion exchange and contact terms from the latest lattice QCD simulations of the two-nucleon system. They assume the forms of the leading order (LO) <jats:italic>NN</jats:italic> potential from the chiral effective field theory and thus are referred to as the LO chiral potential in this study. We extract the coefficients of contact terms and cut-off momenta in these potentials, for the first time, by fitting the phase shifts of <jats:inline-formula> <jats:tex-math><?CDATA $^1S_0$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_071002_M1.jpg" xlink:type="simple" /> </jats:inline-formula> and <jats:inline-formula> <jats:tex-math><?CDATA $^3S_1$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_071002_M2.jpg" xlink:type="simple" /> </jats:inline-formula> channels obtained from the HALQCD collaboration with various pion masses from 468.6 to 1170.9 MeV. The low-energy constants in the <jats:inline-formula> <jats:tex-math><?CDATA $^1S_0$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_071002_M3.jpg" xlink:type="simple" /> </jats:inline-formula> and <jats:inline-formula> <jats:tex-math><?CDATA $^3S_1$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_071002_M4.jpg" xlink:type="simple" /> </jats:inline-formula> channels become weaker and approach each other for larger pion masses. These LO chiral potentials are applied to symmetric nuclear and pure neutron matter within the Brueckner-Hartree-Fock method. Presently, however, we do not yet have the information of the <jats:italic>P</jats:italic>-wave <jats:italic>NN</jats:italic> interaction to be provided by the lattice QCD simulations for a complete description of nuclear matter. Our results enhance understanding of the development of nuclear structure and nuclear matter by controlling the contribution of the pionic effect and elucidate the role of chiral symmetry of the strong interaction in complex systems. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>In light of the recently obtained LHC Higgs data, we examine the parameter space of the type II two-Higgs-doublet model, in which the 125 GeV Higgs bosons exhibit wrong sign Yukawa couplings. Combining the relevant theoretical and experimental limits, we find that the LHC Higgs data exclude most of the parameter space of the wrong sign Yukawa coupling. For <jats:inline-formula> <jats:tex-math><?CDATA $m_H=$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073101_M1.jpg" xlink:type="simple" /> </jats:inline-formula> 600 GeV, the allowed samples are mainly distributed across several corners and narrow bands of <jats:inline-formula> <jats:tex-math><?CDATA $m_A \lt 20$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073101_M2.jpg" xlink:type="simple" /> </jats:inline-formula> GeV, 30 <jats:inline-formula> <jats:tex-math><?CDATA $ \lt m_A \lt 120$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073101_M3.jpg" xlink:type="simple" /> </jats:inline-formula> GeV, 240 GeV <jats:inline-formula> <jats:tex-math><?CDATA $ \lt m_A \lt 300$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073101_M4.jpg" xlink:type="simple" /> </jats:inline-formula> GeV, 380 GeV <jats:inline-formula> <jats:tex-math><?CDATA $ \lt m_A \lt 430$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073101_M5.jpg" xlink:type="simple" /> </jats:inline-formula> GeV, and 480 GeV <jats:inline-formula> <jats:tex-math><?CDATA $ \lt m_A \lt 550$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073101_M6.jpg" xlink:type="simple" /> </jats:inline-formula> GeV. For <jats:inline-formula> <jats:tex-math><?CDATA $m_A=$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073101_M7.jpg" xlink:type="simple" /> </jats:inline-formula> 600 GeV, <jats:inline-formula> <jats:tex-math><?CDATA $m_H$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073101_M8.jpg" xlink:type="simple" /> </jats:inline-formula> is required to be lower than 470 GeV. The light pseudo-scalar with a mass of 20 GeV is still permitted in the case of the wrong sign Yukawa coupling of 125 GeV Higgs bosons. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>We study the quasi-two-body decays <jats:inline-formula> <jats:tex-math><?CDATA $B_{(s)} \to \psi [K^*(892), K^*(1410),$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073102_M1.jpg" xlink:type="simple" /> </jats:inline-formula> <jats:inline-formula> <jats:tex-math><?CDATA $K^*(1680)] \to \psi K\pi$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073102_M2.jpg" xlink:type="simple" /> </jats:inline-formula> by employing the perturbative QCD (PQCD) factorization approach, where the charmonia <jats:inline-formula> <jats:tex-math><?CDATA $\psi$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073102_M3.jpg" xlink:type="simple" /> </jats:inline-formula> represents <jats:inline-formula> <jats:tex-math><?CDATA $J/\psi$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073102_M4.jpg" xlink:type="simple" /> </jats:inline-formula> and <jats:inline-formula> <jats:tex-math><?CDATA $\psi(2S)$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073102_M5.jpg" xlink:type="simple" /> </jats:inline-formula>. The corresponding decay channels are studied by constructing the kaon-pion distribution amplitude (DA) <jats:inline-formula> <jats:tex-math><?CDATA $\Phi_{K \pi}^{\rm{P}}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073102_M6.jpg" xlink:type="simple" /> </jats:inline-formula>, which comprises important final state interactions between the kaon and pion in the resonant region. Relativistic Breit-Wigner formulas are adopted to parameterize the time-like form factor <jats:inline-formula> <jats:tex-math><?CDATA $F_{K\pi}$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073102_M7.jpg" xlink:type="simple" /> </jats:inline-formula> appearing in the kaon-pion DAs. The <jats:italic>SU</jats:italic>(3) flavor symmetry breaking effect resulting from the mass difference between the kaon and pion is taken into account, which makes significant contributions to the longitudinal polarizations. The observed branching ratios and the polarization fractions of <jats:inline-formula> <jats:tex-math><?CDATA $B_{(s)} \to \psi K^*(892) \to \psi K\pi$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073102_M8.jpg" xlink:type="simple" /> </jats:inline-formula> are accommodated by tuning hadronic parameters for the kaon-pion DAs. The PQCD predictions for <jats:inline-formula> <jats:tex-math><?CDATA $B_{(s)} \to \psi [K^*(1410), K^*(1680)] \to \psi K\pi$?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073102_M9.jpg" xlink:type="simple" /> </jats:inline-formula> modes from the same set of parameters can be tested by precise data obtained in the future from LHCb and Belle II experiments. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present an improved calculation of the strong coupling constants <jats:inline-formula> <jats:tex-math><?CDATA $ g_{D^*D\rho} $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073103_M3.jpg" xlink:type="simple" /> </jats:inline-formula> and <jats:inline-formula> <jats:tex-math><?CDATA $ g_{B^*B\rho} $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073103_M4.jpg" xlink:type="simple" /> </jats:inline-formula> in light-cone sum rules, including one-loop QCD corrections of leading power with <jats:inline-formula> <jats:tex-math><?CDATA $ \rho $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073103_M5.jpg" xlink:type="simple" /> </jats:inline-formula> meson distribution amplitudes. We further compute subleading-power corrections from two-particle and three-particle higher-twist contributions at leading order up to twist-4 accuracy. The next-to-leading order corrections to the leading power contribution numerically offset the subleading-power corrections to a certain extent, and our numerical results are consistent with those of previous studies on sum rules. A comparison between our results and existing model-dependent estimations is also made. </jats:p>

<jats:title>Abstract</jats:title> <jats:p>We construct holographic Janus solutions, which describe a conformal interface in the theory of M2-branes, in four-dimensional gauged supergravities using a perturbative method. In particular, we study three Einstein-scalar systems and their BPS equations, which are derived by Bobev, Pilch, and Warner (2014). The actions of our interest are all consistent truncations of <jats:inline-formula> <jats:tex-math><?CDATA $ D = 11 $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073104_M1.jpg" xlink:type="simple" /> </jats:inline-formula> supergravity, chosen to be invariant under <jats:inline-formula> <jats:tex-math><?CDATA $ SO(4)\times SO(4) $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073104_M2.jpg" xlink:type="simple" /> </jats:inline-formula>, <jats:inline-formula> <jats:tex-math><?CDATA $ SU(3)\times U(1)\times U(1) $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073104_M3.jpg" xlink:type="simple" /> </jats:inline-formula>, and <jats:inline-formula> <jats:tex-math><?CDATA $ G_2 $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073104_M4.jpg" xlink:type="simple" /> </jats:inline-formula> symmetry subgroups of <jats:inline-formula> <jats:tex-math><?CDATA $ SO(8) $?></jats:tex-math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="cpc_44_7_073104_M5.jpg" xlink:type="simple" /> </jats:inline-formula>. The utility of our semi-analytic result is illustrated by the calculation of minimal area surface and the associated holographic entanglement entropy. </jats:p>