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Pulsating red giant stars in eccentric binary systems discovered from Kepler space-based photometry. A sample study and the analysis of KIC 5006817

机译:从开普勒基于空间的光度法发现的偏心双星系统中的红色巨星。 KIC 5006817的样本研究和分析

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摘要

The unparalleled photometric data obtained by NASA's Kepler space telescope led to an improved understanding of red giant stars and binary stars. Seismology allows us to constrain the properties of red giants. In addition to eclipsing binaries, eccentric non-eclipsing binaries, exhibiting ellipsoidal modulations, have been detected with Kepler. We aim to study the properties of eccentric binary systems containing a red giant star and derive the parameters of the primary giant component. We apply asteroseismic techniques to determine masses and radii of the primary component of each system. For a selected target, light and radial velocity curve modelling techniques are applied to extract the parameters of the system. The effects of stellar on the binary system are studied. The paper presents the asteroseismic analysis of 18 pulsating red giants in eccentric binary systems, for which masses and radii were constrained. The orbital periods of these systems range from 20 to 440days. From radial velocity measurements we find eccentricities between e=0.2 to 0.76. As a case study we present a detailed analysis of KIC5006817. From seismology we constrain the rotational period of the envelope to be at least 165 d, roughly twice the orbital period. The stellar core rotates 13 times faster than the surface. From the spectrum and radial velocities we expect that the Doppler beaming signal should have a maximum amplitude of 300ppm in the light curve. Through binary modelling, we determine the mass of the secondary component to be 0.29±0.03,M⊙. For KIC5006817 we exclude pseudo-synchronous rotation of the red giant with the orbit. The comparison of the results from seismology and modelling of the light curve shows a possible alignment of the rotational and orbital axis at the 2σ level. Red giant eccentric systems could be progenitors of cataclysmic variables and hot subdwarf B stars.
机译:NASA开普勒太空望远镜获得的无与伦比的光度数据使人们对红色巨星和双星有了更好的理解。地震学使我们能够限制红色巨人的属性。除偏光二进制文件外,开普勒还发现了显示椭圆体调制的偏心非偏光二进制文件。我们旨在研究包含红色巨星的偏心双星系统的性质,并推导初级巨星分量的参数。我们应用星震技术来确定每个系统主要部分的质量和半径。对于选定的目标,可以应用光速和径向速度曲线建模技术来提取系统的参数。研究了恒星对二元系统的影响。本文对质量和半径受约束的偏心二元系统中的18个脉动红巨星进行了星震分析。这些系统的轨道周期从20天到440天不等。通过径向速度测量,我们发现e = 0.2到0.76之间的偏心率。作为案例研究,我们对KIC5006817进行了详细分析。根据地震学,我们将包络线的旋转周期限制为至少165 d,大约是轨道周期的两倍。恒星芯旋转的速度比表面快13倍。从频谱和径向速度,我们预计多普勒波束信号在光曲线中的最大振幅应为300ppm。通过二元建模,我们确定次要成分的质量为0.29±0.03 ,M⊙。对于KIC5006817,我们排除了红色巨人与轨道的伪同步旋转。地震学结果和光曲线建模结果的比较表明,旋转轴和轨道轴可能在2σ水平对准。红色巨型偏心系统可能是灾难变星和炽热的矮矮B星的祖先。

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