The TESS light curve of the eccentric eclipsing binary 1SWASP J011351.29+314909.7 - no evidence for a very hot M-dwarf companion
The TESS light curve of the eccentric eclipsing binary 1SWASP J011351.29+314909.7 - no evidence for a very hot M-dwarf companion
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偏心食双星 1SWASP J011351.29 314909.7 的 TESS 光变曲线 - 没有证据表明存在非常热的 M 矮星伴星
DOI：
10.1093/mnrasl/slaa122
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发表时间：
2020
期刊：
影响因子：
--
通讯作者：
Swayne M
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文献类型：
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作者：
Swayne M
2014 年对食双星 1SWASPJ011351.29+314909.7 (J0113+31) 的一项研究报告称，0.95-M⊙主星的 M 矮星伴星的有效温度出乎意料地高。从次日食深度推断出的有效温度比恒星模型预测的值高约 600 K。这样的异常结果质疑了我们对低质量恒星的理解，并可能表明在推断围绕它们运行的系外行星的特性时存在很大的不确定性。我们试图利用凌日系外行星勘测卫星（TESS）最近观测到的 J0113+31 的光变曲线来测量 M 矮星伴星的有效温度。我们使用 pycheops 建模软件将凌日和日食组合模型拟合到 TESS 光曲线。为了计算次级有效温度，我们将最拟合的日食深度与理论恒星模型预测的日食深度进行比较。我们确定 M 矮星的有效温度为 Teff,2= 3208 ± 43 K，假设 logg2= 5，[Fe/H]= -0.4，并且没有 α 元素增强。改变这些假设会使 Teff,2 变化不到 100 K。这些结果并不支持观测到的低质量恒星温度与理论上的低质量恒星温度之间存在大的异常。
A 2014 study of the eclipsing binary star 1SWASPJ011351.29+314909.7 (J0113+31) reported an unexpectedly high effective temperature for the M-dwarf companion to the 0.95-M⊙primary star. The effective temperature inferred from the secondary eclipse depth was ∼600 K higher than the value predicted from stellar models. Such an anomalous result questions our understanding of low-mass stars and might indicate a significant uncertainty when inferring properties of exoplanets orbiting them. We seek to measure the effective temperature of the M-dwarf companion using the light curve of J0113+31 recently observed by theTransiting Exoplanet Survey Satellite(TESS). We use the pycheops modelling software to fit a combined transit and eclipse model to theTESSlight curve. To calculate the secondary effective temperature, we compare the best-fitting eclipse depth to the predicted eclipse depths from theoretical stellar models. We determined the effective temperature of the M dwarf to beTeff,2= 3208 ± 43 K, assuming logg2= 5, [Fe/H] = −0.4, and no alpha-element enhancement. Varying these assumptions changesTeff,2by less than 100 K. These results do not support a large anomaly between observed and theoretical low-mass star temperatures.