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arXiv 0812.3169astro-ph
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首次高精度太阳系外行星径向速度搜索

The First High-Precision Radial Velocity Search for Extra-Solar Planets

Gordon A. H. Walker

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23 pages, 7 figures
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摘要：

在1970年代末和1980年代初，固态信号发生探测器和吸收池的引入直接将波长基准施加在星光上，恒星径向速度（RV）测量的误差减少到多普勒搜索行星变得可行的程度。1980年，我们开始使用CFHT Coudé摄谱仪的氟化氢气体电池，并在12年的时间里监测了大约29颗太阳型恒星的RV。由于太阳系外行星的质量和轨道都与木星相似，我们每年只获得三到四次两晚的观测机会。1988年，我们强调了$γ$ Cep（K1 IV）的一个潜在行星伴星，1993年强调了$β$ Gem（K0 III）的一个伴星，1992年强调了$ε$ Eri（K2 V）的另一个伴星。这些行星都类似于木星系统，周期和质量分别为2.5年和1.4 $M_{J}$，1.6年和2.6 $M_{J}$，6.9年和0.9 $M_{J}$。所有这三个后来证实了更广泛的数据由得克萨斯州小组领导的科克伦和哈茨谁推导出目前接受的轨道要素。没有一个系统是简单的，有些人仍然质疑$ε$ Eri b。

英文摘要：

In the late 1970s and early 1980s, the introduction of solid-state, signal-generating detectors and absorption cells to impose wavelength fiducials directly on the starlight, the errors in stellar radial velocity (RV) measurements were reduced to the point where Doppler searches for planets became feasible. In 1980 we began to use a hydrogen fluoride gas cell with the CFHT coudé spectrograph and, for 12 years, monitored RVs of some 29 solar-type stars. Since extra-solar planets were expected to resemble Jupiter in both mass and orbit, we were awarded only three or four two-night observing runs each year. In 1988 we highlighted a potential planetary companion to $γ$ Cep (K1 IV), in 1993 one to $β$ Gem (K0 III), and another to $ε$ Eri (K2 V) in 1992. The putative planets all resembled Jovian systems with periods and masses of 2.5 yr and 1.4 $M_{J}$, 1.6 yr and 2.6 $M_{J}$, and 6.9 yr and 0.9 $M_{J}$, respectively. All three were subsequently confirmed from more extensive data by the Texas group led by Cochran and Hatzes who derived the currently accepted orbital elements. None of the systems is simple and some still question $ε$ Eri b.

机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。

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