Pulsating young brown dwarfs
Pulsating young brown dwarfs
复制标题
脉动的年轻褐矮星
DOI：
10.1051/0004-6361:200500020
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发表时间：
2005
影响因子：
6.5
通讯作者：
I. Baraffe
中科院分区：
文献类型：
--
作者：
F. Palla;I. Baraffe
我们提出了一个非绝热的，线性的稳定性分析模型的甚低质量恒星（VLMS）和棕矮星（BD）在中心的氘燃烧阶段的结果。我们发现不稳定的基本模式的周期变化之间的0.02 MBD的0.5hf或a0.1Mstar和0.1h。不稳定性的增长时间随着质量的减少而减少，并且在所考虑的质量范围内（0.1-0.02 M�）保持远低于氘燃烧时间尺度。这些结果对进化模型中相关输入物理的变化是鲁棒的。我们确定可能的候选人之间的脉动变化已知的VLMS和BD附近的星星形成的地区，其位置在HR图福尔斯内或接近边界的不稳定带。最后，我们讨论的可能性，观察到的变化在几个对象的周期为101小时，可以解释的脉动。
We present the results of a nonadiabatic, linear stability analysis of models of very low-mass stars (VLMSs) and brown dwarfs (BDs) during the deuterium burning phase in the center. We find unstable fundamental modes with periods varying between ∼ 5hf or a0 .1Mstar and ∼1 h for a 0.02 MBD. The growth time of the instability decreases with decreasing mass and remains well below the deuterium burning time scale in the mass range considered (0.1-0.02 M� ). These results are robust against variations of the relevant input physics in the evolutionary models. We identify possible candidates for pulsational variability among known VLMSs and BDs in nearby star forming regions whose location in the HR diagram falls within or close to the boundary of the instability strip. Finally, we discuss the possibility that the variability observed in a few objects with periods of ∼1 h can be interpreted in terms of pulsation.