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The HD 217107 planetary system: Twenty years of radial velocity measurements
Astronomische Nachrichten ( IF 0.9 ) Pub Date : 2020-10-11 , DOI: 10.1002/asna.202013830
Mark R. Giovinazzi 1 , Cullen H. Blake 1 , Jason D. Eastman 2 , Jason Wright 3 , Nate McCrady 4 , Rob Wittenmyer 5 , John A. Johnson 2 , Peter Plavchan 6 , David H. Sliski 1 , Maurice L. Wilson 2 , Samson A. Johnson 7 , Jonathan Horner 5 , Stephen R. Kane 8 , Audrey Houghton 4 , Juliana García‐Mejía 2 , Joseph P. Glaser 9
Affiliation  

The hot Jupiter HD 217107 b was one of the first exoplanets detected using the radial velocity (RV) method, originally reported in the literature in 1999. Today, precise RV measurements of this system span more than 20 years, and there is clear evidence for a longer-period companion, HD 217107 c. Interestingly, both the short-period planet ($P_\mathrm{b}\sim7.13$ d) and long-period planet ($P_\mathrm{c}\sim5059$ d) have significantly eccentric orbits ($e_\mathrm{b}\sim0.13$ and $e_\mathrm{c}\sim0.40$). We present 42 additional RV measurements of this system obtained with the MINERVA telescope array and carry out a joint analysis with previously published RV measurements from four different facilities. We confirm and refine the previously reported orbit of the long-period companion. HD 217107 b is one of a relatively small number of hot Jupiters with an eccentric orbit, opening up the possibility of detecting precession of the planetary orbit due to General Relativistic effects and perturbations from other planets in the system. In this case, the argument of periastron, $\omega$, is predicted to change at the level of $\sim$0.8$^\circ$ century$^{-1}$. Despite the long time baseline of our observations and the high quality of the RV measurements, we are only able to constrain the precession to be $\dot{\omega}<65.9^\circ$ century$^{-1}$. We discuss the limitations of detecting the subtle effects of precession in exoplanet orbits using RV data.

中文翻译:

HD 217107 行星系统:二十年的径向速度测量

热木星 HD 217107 b 是最早使用径向速度 (RV) 方法探测到的系外行星之一,最初在 1999 年的文献中报道。今天,对该系统的精确 RV 测量跨越了 20 多年,并且有明确的证据表明一个长期伴侣,HD 217107 c。有趣的是,短周期行星($P_\mathrm{b}\sim7.13$ d)和长周期行星($P_\mathrm{c}\sim5059$ d)都有明显的偏心轨道($e_\mathrm {b}\sim0.13$ 和 $e_\mathrm{c}\sim0.40$)。我们展示了使用 MINERVA 望远镜阵列获得的该系统的 42 个额外 RV 测量值,并与先前发布的来自四个不同设施的 RV 测量值进行了联合分析。我们确认并改进了先前报告的长周期伴星轨道。HD 217107 b 是少数具有偏心轨道的热木星之一,这开辟了检测由于广义相对论效应和系统中其他行星的扰动而导致的行星轨道进动的可能性。在这种情况下,periastron 的参数 $\omega$ 预计会在 $\sim$0.8$^\circ$ Century$^{-1}$ 的水平上发生变化。尽管我们观测的基线时间很长,RV 测量的质量很高,但我们只能将岁差限制为 $\dot{\omega}<65.9^\circ$ Century$^{-1}$。我们讨论了使用 RV 数据检测系外行星轨道中进动的微妙影响的局限性。在这种情况下,periastron 的参数 $\omega$ 预计会在 $\sim$0.8$^\circ$ Century$^{-1}$ 的水平上发生变化。尽管我们观测的基线时间很长,RV 测量的质量很高,但我们只能将岁差限制为 $\dot{\omega}<65.9^\circ$ Century$^{-1}$。我们讨论了使用 RV 数据检测系外行星轨道中进动的微妙影响的局限性。在这种情况下,periastron 的参数 $\omega$ 预计会在 $\sim$0.8$^\circ$ Century$^{-1}$ 的水平上发生变化。尽管我们观测的基线时间很长,RV 测量的质量很高,但我们只能将岁差限制为 $\dot{\omega}<65.9^\circ$ Century$^{-1}$。我们讨论了使用 RV 数据检测系外行星轨道中进动的微妙影响的局限性。
更新日期:2020-10-11
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