First photometric investigation of the near-contact binary LM And     

《New Astronomy》2022

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A photometric study of V608 Cam: apparent period changes as a result of surface activity     

《New Astronomy》2022

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First photometric and orbital period investigations of the total-eclipse contact binary V0339 Com     

《New Astronomy》2022

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The two roles of the SPH Kernel and dissipation on accretion disc modelling in semi-detached Low-Mass Close Binaries     

《New Astronomy》2024

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First photometric study of two eclipsing binary star systems: V523 And and V543 And     

《New Astronomy》2022

Detailed photometric analysis of V523 And and V543 And from the Wide Angle Search for Planets survey is presented for the first time. It was found that while V523 And is a detached binary, V543 And is a semi-detached binary star system. The adopted masses and radii for the primary and secondary components are $M_1=0.77\pm 0.08$ M${}_{\odot }$, $R_1=0.87\pm 0.08$ R${}_{\odot }$ and $M_2=0.50\pm 0.12$ M${}_{\odot }$, $R_2=0.77\pm 0.17$ R${}_{\odot }$ for V523 And; and $M_1=1.59\pm 0.16$ M${}_{\odot }$, $R_1=1.46\pm 0.09$ R${}_{\odot }$ and $M_2=0.58\pm 0.17$ M${}_{\odot }$, $R_2=1.66\pm 0.22$ R${}_{\odot }$ for V543 And. Orbital period variations of the systems were analyzed using the O-C method. The O-C change of V523 And is discussed in terms of the magnetic activity cycle of one or both components and light travel time effect (LTTE) due to a third body in the system. Among these mechanisms, LTTE seems to be the most appropriate mechanism to explain the O-C variation of the system since the quadrupole moments of the primary and secondary components ($\Delta Q$) were found to be in the order of $10^{49}$ g cm${}^2$. The O-C diagram of V543 And shows a downward parabolic trend, which suggests a secular period decrease with a rate of $0.080\pm 0.012$ s/year. The parabolic O-C variation of V543 And was interpreted in terms of the non-conservative mass transfer mechanism. According to this scenario, the range of possible values of the mass gain rate (${\dot{M}}_1$) of the primary component of V543 And as well as the mass-loss rate ($\dot{M}$) of the system were found to be $10^{-5}$–$10^{-11}$ M${}_{\odot }$/year and $10^{-6}$–$10^{-8}$ M${}_{\odot }$/year, respectively.  相似文献   

Study on the variation of orbital period,quasi-periodic oscillations and negative superhumps in V729 Sgr     

《New Astronomy》2022

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Orbital period changes in IO Cep,IM Cep and TX Ari: Path to masses of distant components     

《New Astronomy》2022

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The first photometric analysis study of the GW Psc binary system     

《New Astronomy》2022

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Study of the Astrophysical Origins of Chemical Elements in Two Apparently-single CEMP-s Stars     

《Chinese Astronomy and Astrophysics》2022,46(1):49-62

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First TESS light curve solution and orbital period analysis of V567 And     

《New Astronomy》2022

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