A substellar component orbiting the F-star 30 Arietis B
A substellar component orbiting the F-star 30 Arietis B
复制标题
绕 F 星 30 Arietis B 运行的亚恒星组件
DOI：
10.1051/0004-6361/200912112
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发表时间：
2009
影响因子：
6.5
通讯作者：
D. Gandolfi
中科院分区：
文献类型：
--
作者：
E. Guenther;M. Hartmann;M. Esposito;A. Hatzes;F. Cusano;D. Gandolfi
上下文目前大多数径向速度行星搜索计划都集中在一个太阳质量的恒星上。因此，我们对大质量恒星的巨行星和褐矮星伴星的频率的了解相当有限。在类太阳恒星的情况下，短周期褐矮星伴星和超大质量行星的频率似乎很低。目标。在这里，我们提出了一个亚恒星的伴星30阿里B，一个F星的1.16 ± 0.04 $M_\odot$，是一个层次的三重系统的成员的证据。方法.这颗伴星是通过使用2米阿尔弗雷德-詹士望远镜及其阶梯光栅摄谱仪进行精确的径向速度测量而探测到的。碘吸收池为精确的恒星径向速度测量提供了波长参考。结果通过对径向速度测量结果的分析，导出了伴星的轨道周期为P = 335.1 ± 2.5天，偏心率e = 0.289 ± 0.092，质量函数f（m）=（6.1 ± 1.7）× 10 - 7 M_（odot）。结论.我们得出结论：30 Ari B的径向速度变化是由于一颗质量为9.88 ± 0.94 $M_{\mathrm{Jup}}$的大质量行星或棕矮星伴星引起的。因此，该天体属于罕见的大质量行星和褐矮星类，它们围绕主序星运行。
Context. Most current radial velocity planet search programs have concentrated on stars of one solar mass. Our knowledge on the frequency of giant planets and brown dwarf companions to more massive stars is thus rather limited. In the case of solar-like stars, the frequency of short-period brown dwarf companions and very massive planets seems to be low. Aims. Here we present evidence for a substellar companion to 30 Ari B, an F-star of 1.16 ± 0.04 $M_\odot$ that is a member of a hierarchical triple system. Methods. The companion was detected by means of precise radial velocity measurements using the 2-m Alfred-Jensch telescope and its echelle spectrograph. An iodine absorption cell provided the wavelength reference for precise stellar radial velocity measurements. Results. We analyzed our radial velocity measurements and derived an orbit to the companion with period, P = 335.1 ± 2.5 days, eccentricity e = 0.289 ± 0.092, and mass function $f(m)$ = (6.1 ± 1.7)$\times$10 -7 $M_\odot$. Conclusions. We conclude that the radial velocity variations of 30 Ari B are due to a companion with m sin i of 9.88 ± 0.94 $M_{\mathrm{Jup}}$ that is either a massive planet or a brown dwarf. The object thus belongs to the rare class of massive planets and brown dwarfs orbiting main- sequence stars.