TESTING THE ASTEROSEISMIC SCALING RELATIONS FOR RED GIANTS WITH ECLIPSING BINARIES OBSERVED BY KEPLER
TESTING THE ASTEROSEISMIC SCALING RELATIONS FOR RED GIANTS WITH ECLIPSING BINARIES OBSERVED BY KEPLER
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DOI：
10.3847/0004-637x/832/2/121
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发表时间：
2016-09
期刊：
影响因子：
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通讯作者：
P. Gaulme;J. McKeever;J. Jackiewicz;M. Rawls;E. Corsaro;B. Mosser;J. Southworth;S. Mahadevan
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文献类型：
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作者：
P. Gaulme;J. McKeever;J. Jackiewicz;M. Rawls;E. Corsaro;B. Mosser;J. Southworth;S. Mahadevan
鉴于集合星震学在了解大量恒星的基本性质方面的潜力，确定这些测量所依据的标度关系的准确性至关重要。从几个强大的验证技术，到目前为止，所有的迹象表明，恒星半径的估计，从小行星地震的比例关系是准确的，在百分之几。拥有至少一颗星星并具有可探测到的类太阳振荡的双星系统是验证小行星地震半径和质量推断的理想测试对象。通过结合视向速度（RV）测量和食的光度时间序列，有可能确定双线分光双星每个组成部分的质量和半径。我们报告的结果进行了为期四年的RV调查与天体物理研究联合会的3.5米望远镜和APOGEE光谱仪在阿帕奇点天文台的埃歇尔光谱仪。我们比较的质量和半径的10个红巨星（RG）通过结合径向速度和日食测光的估计从星震标度关系。我们发现，asterosseismic标度关系高估RG半径平均约5%，质量约15%的恒星在不同阶段的RG演变。系统性地高估质量会导致低估恒星年龄，这可能对用于银河系研究的系综星震学有重要影响。作为第二个目标的一部分，其中asteroseismology是用于了解二进制系统，我们确认，振荡的RG在密切的二进制可以被抑制到无法检测到，在以前的工作中提出的假设。
Given the potential of ensemble asteroseismology for understanding fundamental properties of large numbers of stars, it is critical to determine the accuracy of the scaling relations on which these measurements are based. From several powerful validation techniques, all indications so far show that stellar radius estimates from the asteroseismic scaling relations are accurate to within a few percent. Eclipsing binary systems hosting at least one star with detectable solar-like oscillations constitute the ideal test objects for validating asteroseismic radius and mass inferences. By combining radial velocity (RV) measurements and photometric time series of eclipses, it is possible to determine the masses and radii of each component of a double-lined spectroscopic binary. We report the results of a four-year RV survey performed with the échelle spectrometer of the Astrophysical Research Consortium’s 3.5 m telescope and the APOGEE spectrometer at Apache Point Observatory. We compare the masses and radii of 10 red giants (RGs) obtained by combining radial velocities and eclipse photometry with the estimates from the asteroseismic scaling relations. We find that the asteroseismic scaling relations overestimate RG radii by about 5% on average and masses by about 15% for stars at various stages of RG evolution. Systematic overestimation of mass leads to underestimation of stellar age, which can have important implications for ensemble asteroseismology used for Galactic studies. As part of a second objective, where asteroseismology is used for understanding binary systems, we confirm that oscillations of RGs in close binaries can be suppressed enough to be undetectable, a hypothesis that was proposed in a previous work.