An analysis of the transit times of tres-1b
An analysis of the transit times of tres-1b
复制标题
tres-1b 的渡越时间分析
DOI：
10.1111/j.1745-3933.2005.00113.x
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发表时间：
2005
影响因子：
--
通讯作者：
E. Agol
中科院分区：
文献类型：
--
作者：
J. Steffen;E. Agol
已知凌日行星系统中第二颗行星的存在将导致凌日之间的时间发生变化。这些变化可以用来限制轨道要素和扰动行星的质量。我们分析了Charbonneau等人给出的TrES-1系统的过境时间。我们从这些数据中没有发现第二颗行星的令人信服的证据。通过进一步的分析，我们约束的质量，扰动行星可以作为一个函数的两个行星的半长轴比和偏心率的扰动行星。在低阶平均运动共振附近（分数偏差在0.1%以内），我们发现二级行星通常必须具有与地球质量相当或小于地球质量的质量，这表明这些数据是第一个对地球质量以下的行星敏感的数据。我们比较了这种技术的灵敏度与未来的扰动行星的质量，高精度的径向速度测量。Ke yw ords：eclipses-stars：individual：GSC 02652 − 01324-planetary systems.
The presence of a second planet in a known, transiting-planet system will cause the time between transits to vary. These variations can be used to constrain the orbital elements and mass of the perturbing planet. We analyse the set of transit times of the TrES-1 system given in Charbonneau et al. We find no convincing evidence for a second planet in the TrES-1 system from those data. By further analysis, we constrain the mass that a perturbing planet could have as a function of the semi-major axis ratio of the two planets and the eccentricity of the perturbing planet. Near low-order, mean-motion resonances (within ∼1 per cent fractional deviation), we find that a secondary planet must generally have a mass comparable to or less than the mass of the Earth ‐ showing that these data are the first to have sensitivity to subEarth-mass planets. We compare the sensitivity of this technique to the mass of the perturbing planet with future, high-precision radial velocity measurements. Ke yw ords: eclipses ‐ stars: individual: GSC 02652 − 01324 ‐ planetary systems.