Photometric observations of an eclipsing binary system, YY Eridani were done in blue (B) and yellow (V) wavelength bands and, finally, the light curve in each wavelength band was constructed. Orbital elements and phys...Photometric observations of an eclipsing binary system, YY Eridani were done in blue (B) and yellow (V) wavelength bands and, finally, the light curve in each wavelength band was constructed. Orbital elements and physical properties of YY Eridani have been calculated using observational data of Binnendijk (1965) and authors have developed Wilson Devinney technique in analyzing the best solution of this eclipsing binary system. More physical parameters eg: orbital inclination, gravity darkening exponent, effective temperature, gravitational potential etc. of each component were calculated in this research for the best solution of YY Eridani. Synthetic light curves which were constructed from the best solution are in good correspondence with observational light curves of Binnendijk. When comparing with observational light curves obtained from this research, it was found that there exist the phase shift of 0 1. It is possible that physical properties of YY Eridani have been changed due to the rotation of its major axis or mass transfer mechanism of the system.展开更多
The motion of a test particle within the context of the restricted four-body problem(R4BP)driven by a new kind of potential,called the generalized Manev potential,with perturbations in the Coriolis and centrifugal for...The motion of a test particle within the context of the restricted four-body problem(R4BP)driven by a new kind of potential,called the generalized Manev potential,with perturbations in the Coriolis and centrifugal forces is considered in this study.The system possesses eight libration points which were distributed on its plane of motion in different manner from those of the usual Newtonian potential.Unlike the case of the perturbed R4BP under Newtonian potential,where two of these librations are stable,all of them are unstable in linear sense under Manev potential.We found that a gradual perturbation in the centrifugal force causes the trajectories of motion to drift inward but the Coriolis force was proven to have no effect on the location of the libration points of the system.Using first order Lyapunov characteristic exponents,the dynamical behavior of the system is found irregular.We experimented with a high velocity stellar system(82 G.Eridani)to establish the applicability of the model in astrophysics.展开更多
Taking into account the helium and metal diffusion, we explore the possible evolutionary status with a seismic analysis, of the MOST （Microvariability and Oscillations of STars） target： the star e Eri. We adopt dif...Taking into account the helium and metal diffusion, we explore the possible evolutionary status with a seismic analysis, of the MOST （Microvariability and Oscillations of STars） target： the star e Eri. We adopt different input parameters to construct models to fit the available observational constraints in, e.g., Teff, L, R and [Fe/H]. From the computation we obtain the average large spacings of e Eri to be about 194 ± 1μHz. The age of the diffused models was found to be about 1 Gyr, which is younger than the age determined previously by models without diffusion. We found that the effect of pure helium diffusion on the internal structure of the young low-mass star is slight, but that of metal diffusion is obvious. The metal diffusion leads the models to have much higher temperature in the radiative interior, and, correspondingly a higher sound speed there, hence a larger frequency and spacings.展开更多
文摘Photometric observations of an eclipsing binary system, YY Eridani were done in blue (B) and yellow (V) wavelength bands and, finally, the light curve in each wavelength band was constructed. Orbital elements and physical properties of YY Eridani have been calculated using observational data of Binnendijk (1965) and authors have developed Wilson Devinney technique in analyzing the best solution of this eclipsing binary system. More physical parameters eg: orbital inclination, gravity darkening exponent, effective temperature, gravitational potential etc. of each component were calculated in this research for the best solution of YY Eridani. Synthetic light curves which were constructed from the best solution are in good correspondence with observational light curves of Binnendijk. When comparing with observational light curves obtained from this research, it was found that there exist the phase shift of 0 1. It is possible that physical properties of YY Eridani have been changed due to the rotation of its major axis or mass transfer mechanism of the system.
文摘The motion of a test particle within the context of the restricted four-body problem(R4BP)driven by a new kind of potential,called the generalized Manev potential,with perturbations in the Coriolis and centrifugal forces is considered in this study.The system possesses eight libration points which were distributed on its plane of motion in different manner from those of the usual Newtonian potential.Unlike the case of the perturbed R4BP under Newtonian potential,where two of these librations are stable,all of them are unstable in linear sense under Manev potential.We found that a gradual perturbation in the centrifugal force causes the trajectories of motion to drift inward but the Coriolis force was proven to have no effect on the location of the libration points of the system.Using first order Lyapunov characteristic exponents,the dynamical behavior of the system is found irregular.We experimented with a high velocity stellar system(82 G.Eridani)to establish the applicability of the model in astrophysics.
基金the National Natural Science Foundation of China
文摘Taking into account the helium and metal diffusion, we explore the possible evolutionary status with a seismic analysis, of the MOST （Microvariability and Oscillations of STars） target： the star e Eri. We adopt different input parameters to construct models to fit the available observational constraints in, e.g., Teff, L, R and [Fe/H]. From the computation we obtain the average large spacings of e Eri to be about 194 ± 1μHz. The age of the diffused models was found to be about 1 Gyr, which is younger than the age determined previously by models without diffusion. We found that the effect of pure helium diffusion on the internal structure of the young low-mass star is slight, but that of metal diffusion is obvious. The metal diffusion leads the models to have much higher temperature in the radiative interior, and, correspondingly a higher sound speed there, hence a larger frequency and spacings.
