Contact binary systems,including massive,middle-mass and low-mass systems,have been observed.It is necessary to construct the evolutionary model for contact binary systems with all different masses.The model introduce...Contact binary systems,including massive,middle-mass and low-mass systems,have been observed.It is necessary to construct the evolutionary model for contact binary systems with all different masses.The model introduced by Huang,Song and Bi indicates some special and unique understandings of the physical processes occurring in the contact binaries.It is necessary to test whether this model can be applied to the early-type contact binaries.The best way to test a theoretical model is to know whether this model can explain the observational phenomena of such binaries.For this aim,a comparison is performed for the relations of mass-luminosity,mass-radius,and the distribution in the HR diagram obtained from the model introduced by Huang et al.and those from the astronomical observations.A good result is obtained by the comparison.This means the model can be used in calculating the evolution of early-type contact binaries,and can explain the observational phenomena of such binaries.展开更多
In this work, predictions of the spectral energy distribution from populations of single and binary stars are incorporated into a galactic chemical and color evolution model to explore the significance of the effects ...In this work, predictions of the spectral energy distribution from populations of single and binary stars are incorporated into a galactic chemical and color evolution model to explore the significance of the effects of the binary interactions on the color evolution of M33. We first constructed a model without binary interactions, and the model is able to reproduce most of the available observational constraints on the distribution of stellar parameters. We then run simulations with the same set of model parameters but with binary interactions considered. By comparing the results for the populations with and without binary interactions, we find that the inclusion of binary interactions makes the surface brightness greater (~0.1 mag arcsec 2) in FUV-band but smaller (~0.7 mag arcsec 2) in K-band, while it results in the FUV K color bluer (~0.8 mag). To reproduce the observations, a model that considers the binary interactions should make more gas fall onto the disk in the early time of the galaxy evolution, or increase the total stellar mass, or both.展开更多
基金supported by the National Natural Science Foundation of China (Grant No.10933002)
文摘Contact binary systems,including massive,middle-mass and low-mass systems,have been observed.It is necessary to construct the evolutionary model for contact binary systems with all different masses.The model introduced by Huang,Song and Bi indicates some special and unique understandings of the physical processes occurring in the contact binaries.It is necessary to test whether this model can be applied to the early-type contact binaries.The best way to test a theoretical model is to know whether this model can explain the observational phenomena of such binaries.For this aim,a comparison is performed for the relations of mass-luminosity,mass-radius,and the distribution in the HR diagram obtained from the model introduced by Huang et al.and those from the astronomical observations.A good result is obtained by the comparison.This means the model can be used in calculating the evolution of early-type contact binaries,and can explain the observational phenomena of such binaries.
基金supported by the National Natural Science Foundation of China (Grant Nos. 11033008 and 10821061)the Chinese Academy of Sciences (Grant No. KJCX2-YW-T24)
文摘In this work, predictions of the spectral energy distribution from populations of single and binary stars are incorporated into a galactic chemical and color evolution model to explore the significance of the effects of the binary interactions on the color evolution of M33. We first constructed a model without binary interactions, and the model is able to reproduce most of the available observational constraints on the distribution of stellar parameters. We then run simulations with the same set of model parameters but with binary interactions considered. By comparing the results for the populations with and without binary interactions, we find that the inclusion of binary interactions makes the surface brightness greater (~0.1 mag arcsec 2) in FUV-band but smaller (~0.7 mag arcsec 2) in K-band, while it results in the FUV K color bluer (~0.8 mag). To reproduce the observations, a model that considers the binary interactions should make more gas fall onto the disk in the early time of the galaxy evolution, or increase the total stellar mass, or both.
