| The variety of stellar luminosity will reveal the properties of stars.There are many factors contributing to the photometric changes of stars,such as external factors,e.g.binary eclipsing or planetary transiting,as well as internal factors such as star spots,magnetic field activity or stellar vibration.With the launch of space telescopes such as CoRoT,Kepler and TESS,more and more time-domain observations will be released,which will help researchers better study the properties and internal structures of stars.Binary system is one of the important observation sources in astronomy.It is a natural laboratory for the verification of Newton's law,general relativity and stellar evolution theory.When two stars eclipsed with each other,the total observed brightness of the system decreases alternately.Different eclipsing contours reflect different orbital configurations and relative sizes of the binary components.However eclipsing phe-nomenon between two stars only provide relative parameters,as long as combined with asteroseismology for one star's absolute parameters,such as mass and radius,coupled with Kepler's third law,can be convenient to determine the parameters of the binary system.Combined with the motion information of binary,the orbit configuration can be restricted.And then the orbital dynamic evolution process and the evolution process of stars in binary can be studied.This thesis focuses on the study of astroseismology for the eclipsing binary system in Kepler time-domain observation data.The first chapter of this thesis briefly reviews the research progress and observation progress of asteroseismology and binary systems,including oscillating characteristics of stars in different evolution stages,the classification and the orbital evolution of binary stars,and so on.The research is based on the observation of Kepler space telescope,so this chapter also brie:fly introduces the Kepler space telescope,including observation mode,data structure and noise sources.The long continuous,uninterrupted,and high precision observational data extremely valuable in stellar seismology research field.In the second chapter,the widely accepted theory of stellar oscillation is reviewed.Through the peirturbation proce,ssing of,stellar oscillation equations,we introduce the p mode oscillation produced by pressure disturbance and g mode oscillation produced by gravity disturbance.And the propagate area also discussed.The excitation of os-cillatioTn needs by other forms of energy into the oscillation energy.We classify the oscillation caused by random turbulent motion on the stellar surface as random excita-tion mechanism.Accordingly,we classify the?echanism and the ? mechanism as continuous excitation mechanism.The random and continuous excitation mechanism will be studied in the nest section respectively.The third chapter studies the solar like oscillation stars.By cross-matching the solar like oscillation sources and eclipsing binaries in Kepler's field of vision,92 os-cillation eclipsing binaries were obtained.Through the solution of light curve,and solving binary orbital configuration,and then use one of the members of the oscilla-tion star's asteroseismology scale relation,we deduced the other star's mass and radius.The parameters are obtained independently by the method of asteroseismology,which can be compared with other methods of stellar spectral observation or radial velocity observation.On the contrary,it is also possible to modify the solution methods such as asteroseismology method or spectral method by exact stellar parameters.In chapter four we studied the c)Scuti variable stars.The pulsation of a single star has been extensively studied.However,we focused on the ? Scuti star in an eclipsing binary system.The intrinsic pressure modes of a ? Scuti star have been altered by its companion's tidal forces.U,sing high precision photometry data from K2 mission,we present a short-period eclipsing binary EPIC 202843107.By subtracting the binary model we obtained 13 high signal to noise ratio stellar independent pulsations to set limits to the asteroseismic analysis,and obtained an optimal model.The model shows that EPIC 202843107A is a typical ? Scuti star in the post-main sequence phase,and the stellar outer layer is concentrated with low-frequency P mode oscillations.Due to the star distortions caused by its companion's gravity,the l=0.1 modes are dampened and the l= 2 mode is enhanced;all splitting frequencies are exhibited in the l= 2 modes because of stellar rotation.The companion's powerful gravity deforms EPIC 202843107A,which could easily lead to an incorrectly recognized frequency pattern.So the binary parameters are required to perform a more accurate asteroseismic analysis.Finally,the summarizes and prospects of the research are persent in chapter five.Asteroseismology can get to know the physical state of host star,to accurately deter-mine the stellar evolution stage and exoplanets system parameter,also can make us a better understanding of the surrounding environment,such as the exoplanet's habitable zone.It is believed that in the near future,human will hear other sounds from a new world through the study of astroseismology-Listening to the stars and searching for new worlds!... |
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