THE CALIFORNIA PLANET SURVEY. I. FOUR NEW GIANT EXOPLANETS
THE CALIFORNIA PLANET SURVEY. I. FOUR NEW GIANT EXOPLANETS
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DOI：
10.1088/0004-637x/721/2/1467
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发表时间：
2010-03
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通讯作者：
Andrew W. Howard;John A. Johnson;Geoffrey W. Marcy;Debra A. Fischer;Jason T. Wright;David Bernat;Gregory W. Henry;Kathryn M. G. Peek;H. Isaacson;K. Apps;M. Endl;William D. Cochran;Jeff A. Valenti;Jay Anderson;Nikolai E. Piskunov
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作者：
Andrew W. Howard;John A. Johnson;Geoffrey W. Marcy;Debra A. Fischer;Jason T. Wright;David Bernat;Gregory W. Henry;Kathryn M. G. Peek;H. Isaacson;K. Apps;M. Endl;William D. Cochran;Jeff A. Valenti;Jay Anderson;Nikolai E. Piskunov
我们给出了过去十年由加州行星调查局(CPS)在凯克天文台获得的四颗恒星的精确多普勒测量结果。这些恒星，即HD 34445、HD 126614、HD 13931和Gl 179，都证明有一颗行星处于开普勒式运动中。我们还给出了两颗恒星HD 34445和Gl179的霍比-埃伯利望远镜的多普勒测量结果，证实了凯克的探测结果，并显著改进了轨道参数。这些行星增加了围绕冰线附近或之外运行的巨行星的统计特性，值得通过天体测量、成像和星载光谱进行后续研究。它们的轨道参数涵盖了行星最小质量(Msin i=0.38-1.9MJup)、轨道周期(P=2.87-11.5yr)、半长轴(a=2.1-5.2AU)和偏心率(e=0.02-0.41)的广泛范围。HD 34445 b(P=2.87年，M sin i=0.79MJ，e=0.27)是一颗围绕一颗古老的G型恒星运行的大质量行星。我们宣布了一颗行星HD 126614 AB和一颗M矮星HD 126614 B，它围绕着富含金属的恒星HD 126614(我们现在称为HD 126614 A)运行。这颗行星的最小质量为Msin i=0.38MJup，围绕主星运行，周期P=3.41年，轨道间距a=2.3AU。微弱的M矮星伴星HD 126614 B与恒星主星相距489ms(33AU)，是通过自适应光学和Palomar天文台的法罗相机直接观测发现的。这个新系统中的主星HD 126614 A是已知所有行星恒星中金属丰度最高的([Fe/H]=+0.56)。HD 13931 b(P=11.5yr，Msin i=1.88MJup，e=0.02)是一颗绕着一颗近太阳双胞胎运行的类似木星的天体。GL179b(P=6.3yr，Msin i=0.82MJup，e=0.21)是一颗绕弱M矮星运行的大质量行星。正如Johnson&Apps最近记录的那样，Gl 179的高金属丰度与M矮星之间的行星金属丰度关联是一致的。
We present precise Doppler measurements of four stars obtained during the past decade at Keck Observatory by the California Planet Survey (CPS). These stars, namely, HD 34445, HD 126614, HD 13931, and Gl 179, all show evidence for a single planet in Keplerian motion. We also present Doppler measurements from the Hobby-Eberly Telescope (HET) for two of the stars, HD 34445 and Gl 179, that confirm the Keck detections and significantly refine the orbital parameters. These planets add to the statistical properties of giant planets orbiting near or beyond the ice line, and merit follow-up by astrometry, imaging, and space-borne spectroscopy. Their orbital parameters span wide ranges of planetary minimum mass (M sin i = 0.38–1.9 MJup), orbital period (P = 2.87–11.5 yr), semimajor axis (a = 2.1–5.2 AU), and eccentricity (e = 0.02–0.41). HD 34445 b (P = 2.87 yr, M sin i = 0.79 MJup, e = 0.27) is a massive planet orbiting an old, G-type star. We announce a planet, HD 126614 Ab, and an M dwarf, HD 126614 B, orbiting the metal-rich star HD 126614 (which we now refer to as HD 126614 A). The planet, HD 126614 Ab, has minimum mass M sin i = 0.38 MJup and orbits the stellar primary with period P = 3.41 yr and orbital separation a = 2.3 AU. The faint M dwarf companion, HD 126614 B, is separated from the stellar primary by 489 mas (33 AU) and was discovered with direct observations using adaptive optics and the PHARO camera at Palomar Observatory. The stellar primary in this new system, HD 126614 A, has the highest measured metallicity ([Fe/H] = +0.56) of any known planet-bearing star. HD 13931 b (P = 11.5 yr, M sin i = 1.88 MJup, e = 0.02) is a Jupiter analog orbiting a near solar twin. Gl 179 b (P = 6.3 yr, M sin i = 0.82 MJup, e = 0.21) is a massive planet orbiting a faint M dwarf. The high metallicity of Gl 179 is consistent with the planet–metallicity correlation among M dwarfs, as documented recently by Johnson & Apps.