Mass–Radius Relationship for M Dwarf Exoplanets: Comparing Nonparametric and Parametric Methods
Mass–Radius Relationship for M Dwarf Exoplanets: Comparing Nonparametric and Parametric Methods
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M 矮系外行星的质量-半径关系：比较非参数方法和参数方法
DOI：
10.3847/1538-4357/ab334c
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发表时间：
2019
期刊：
影响因子：
--
通讯作者：
S. Mahadevan
中科院分区：
文献类型：
--
作者：
S. Kanodia;A. Wolfgang;G. Stefansson;Bo;S. Mahadevan
虽然它们是银河系中最丰富的恒星，但M矮星只形成了已知恒星中的一小部分，这些恒星拥有测量半径和质量的系外行星。本文利用对24颗系外行星的质量-半径（M-R）测量，分析了M矮星周围行星的质量-半径（M-R）关系。特别是，我们应用参数和非参数模型并比较两种不同的拟合方法。我们还用这些方法对M矮星的M-R关系与开普勒样品的结果进行了比较。使用非参数方法，我们发现M矮星周围最小和最大行星的预测质量小于开普勒数据的类似拟合，但3颗R矮星行星的质量分布在两个数据集之间没有实质性差异。随着未来凌日系外行星调查卫星和可居住区行星探测器等仪器对M矮M-R关系的补充，我们将能够更详细地描述这些差异。我们发布了一个公开的Python代码MRExo（https：//github.com/shbhuk/mrexo），它使用Ning等人介绍的非参数算法来拟合M-R关系。这样的非参数拟合不假设对测量的潜在幂律拟合，因此可以用于拟合比幂律更少偏差的M-R关系。此外，MRExo提供了一种工具来预测质量从半径后方，反之亦然。
Though they are the most abundant stars in the Galaxy, M dwarfs form only a small subset of known stars hosting exoplanets with measured radii and masses. In this paper, we analyze the mass–radius (M-R) relationship of planets around M dwarfs using M-R measurements for 24 exoplanets. In particular, we apply both parametric and nonparametric models and compare the two different fitting methods. We also use these methods to compare the results of the M dwarf M-R relationship with that from the Kepler sample. Using the nonparametric method, we find that the predicted masses for the smallest and largest planets around M dwarfs are smaller than similar fits to the Kepler data, but that the distribution of masses for 3 R⊕ planets does not substantially differ between the two data sets. With future additions to the M dwarf M-R relation from the Transiting Exoplanet Survey Satellite and instruments like the Habitable Zone Planet Finder, we will be able to characterize these differences in more detail. We release a publicly available Python code called MRExo (https://github.com/shbhuk/mrexo) that uses the nonparametric algorithm introduced by Ning et al. to fit the M-R relationship. Such a nonparametric fit does not assume an underlying power-law fit to the measurements and hence can be used to fit an M-R relationship that is less biased than a power law. In addition, MRExo offers a tool to predict mass from radius posteriors, and vice versa.
DOI：
10.3847/1538-4357/aada83
发表时间：
2018-05
期刊：
The Astrophysical Journal
影响因子：
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作者：
T. Berger;D. Huber;E. Gaidos;J. V. van Saders
通讯作者：
T. Berger;D. Huber;E. Gaidos;J. V. van Saders
凌日系统GJ1214：高精度散焦凌日观测并寻找凌日时间变化的证据
影响因子：
6.5
作者：
Harpsøe K
通讯作者：
Harpsøe K
影响因子：
4.8
作者：
Awiphan, S.;Kerins, E.;Haislip, J. B.
通讯作者：
Haislip, J. B.