ON THE AGE OF GLIESE 86
ON THE AGE OF GLIESE 86
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格利斯 86 岁
DOI：
10.1088/0004-637x/785/1/68
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发表时间：
2014
期刊：
影响因子：
--
通讯作者：
F. Pozo Nuñez
中科院分区：
文献类型：
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作者：
K. Fuhrmann;R. Chini;L. Buda;F. Pozo Nuñez
格利泽86是一颗邻近的行星，拥有一颗目视双星，由一颗K型主星Gl 86 A和一颗白色矮星Gl 86 B组成。在这项工作中，我们提出了一个模型大气分析的MA = 0.83 M的主，其化学毫不含糊地确定它作为一个10 Gyr老磁盘星星。对于第二颗，这产生了一个祖先质量Mprog = 1.11 ± 0.05 M，并且--通过与它的本地兄弟o 2 Eri-1的推论--一个白色矮星质量MB = 0.49 ± 0.02 M。与Gl 86 A的2-3 Gyr色球年龄的差异，如Rocha-Pinto，Castilho和Maciel首先指出的，因此最有可能是来自遥远简并的质量和角动量的先前吸积的结果。因此，这也意味着对于短周期的系统，如天狼星或南河三，当它们演化到行星状星云阶段时，人们必须期待显著的风吸积，这样系统的年龄就不能从它们目前明亮的原色中可靠地确定。
Gliese 86 is a nearby planet hosting a visual binary consisting of a K-type primary, Gl 86 A, and a white dwarf secondary, Gl 86 B. In this work, we present a model atmosphere analysis of the MA = 0.83 M☉ primary, whose chemistry unambiguously identifies it as a 10 Gyr old disk star. For the secondary, this gives rise to a progenitor mass Mprog = 1.11 ± 0.05 M☉, and—by inference with its local sibling o2 Eri—a white dwarf mass MB = 0.49 ± 0.02 M☉. The discrepancy with the 2–3 Gyr chromospheric age of Gl 86 A, as first noted by Rocha-Pinto, Castilho & Maciel, is thus most plausibly the result of a former accretion of mass and angular momentum from the distant degenerate. In consequence, this also implies that with respect to shorter-period systems, like Sirius or Procyon, one must expect significant wind accretion when they evolve through the planetary nebula phase, such that the system ages cannot be reliably determined from their currently bright primaries.