A Search for Transit Effects in Spectra of 51 Pegasi and HD 209458
A Search for Transit Effects in Spectra of 51 Pegasi and HD 209458
复制标题
51 Pegasi 和 HD 209458 光谱中凌日效应的搜索
DOI：
10.1086/317706
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发表时间：
2000
影响因子：
3.5
通讯作者：
G. Marcy
中科院分区：
文献类型：
--
作者：
K. Bundy;G. Marcy
我们使用高分辨率光谱来寻找围绕 HD 209458 和 51 Pegasi 运行的行星的明显吸收线或发射线。对于每颗恒星，在下合期间获得了两个光谱，从而能够检测来自行星大气的吸收线。还在全范围的轨道相位上检查了光谱。搜索涉及从运输过程中获取的参考光谱中减去运输过程中的光谱。我们发现 HD 209458 和 51 Peg 在任何轨道相位的光谱都没有显着变化，典型的检测阈值为几个百分点。 HD 209458 的速度测量值在中凌日后 40 分钟进行，比开普勒拟合低约 20 m s−1，大概是由于行星移除了旋转恒星表面后退半球的通量。这与行星的轨道与恒星自转方向相同，与 D. Queloz 及其同事最近的研究结果一致。
We have used high‐resolution optical spectra to search for obvious absorption or emission lines from the planets orbiting HD 209458 and 51 Pegasi. For each star, two spectra were obtained during inferior conjunction, enabling the detection of absorption lines from the planetary atmosphere. Spectra were also examined at a full range of orbital phases. The search involved subtracting spectra during transit from reference spectra taken out of transit. We found no significant variations in the spectra of HD 209458 and 51 Peg at any orbital phase, with typical detection thresholds of several percent. Velocity measurements of HD 209458 taken 40 minutes after midtransit fall ∼20 m s−1 below the Keplerian fit, presumably due to the planet removing flux from the receding hemisphere of the rotating stellar surface. This is consistent with the planet orbiting in the same direction as the star spins, in agreement with recent work by D. Queloz and coworkers.