期刊
ASTROPHYSICAL JOURNAL
卷 710, 期 2, 页码 1596-1609出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/710/2/1596
关键词
methods: data analysis; stars: fundamental parameters; stars: interiors; stars: oscillations
资金
- International Space Science Institute (ISSI)
- European Helio- and Asteroseismology Network (HELAS)
- European Commission
- UK Science and Technology Facilities Council (STFC)
- Science and Technology Facilities Council [ST/F002041/1] Funding Source: researchfish
- STFC [ST/F002041/1] Funding Source: UKRI
The NASA Kepler mission is designed to find planets through transits. Accurate and precise radii of the detected planets depend on knowing the radius of the host star accurately, which is difficult unless the temperature and luminosity of the star are known precisely. Kepler, however, has an asteroseismology program that will provide seismic variables that can characterize stellar radii easily, accurately, and extremely precisely. In this paper, we describe the Yale-Birmingham (YB) method to determine stellar radii using a combination of seismic and conventional variables and analyze the effect of these variables on the result. We find that for main-sequence stars, a knowledge of the parallax is not important to get accurate radii using the YB method: we can get results to an accuracy and precision of better than a few percent if we know the effective temperature and the seismic parameters for these stars. Metallicity does not make much difference either. However, good estimates of the effective temperature and metallicity, along with those of the seismic parameters, are essential to determine radii of subgiants properly. On the other hand, for red giants we find that determining radii properly is not possible without a good estimate of the parallax. We find that the so-called surface term in the seismic data has minimal effect on the inferred radii. Uncertainties in the convective mixing length can matter under some circumstances and can cause a systematic shift in the inferred radii. Blind tests with data simulated to match those expected from the asteroseismic survey phase of Kepler show that it will be possible to infer stellar radii successfully using our method.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据