Alkali Line Profiles for Brown Dwarfs and their Application
Alkali Line Profiles for Brown Dwarfs and their Application
复制标题
褐矮星碱线剖面及其应用
DOI：
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发表时间：
2006
期刊：
影响因子：
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通讯作者：
P. Hauschildt
中科院分区：
文献类型：
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作者：
C. Johnas;N. Allard;D. Homeier;P. Hauschildt
自1995年以来，在寻找棕矮星和太阳系外巨行星方面取得了巨大的进展和极其令人兴奋的结果。在它们的光谱形成过程中，碱共振线的远翼，特别是NaI和KI，起着非常重要的作用。为了计算合成光谱和颜色并得出这些物体的可靠参数和大气化学成分，模型大气是必要的。利用碱共振线轮廓[1]和[2]，将概述合成光谱与先前结果[3]、[4]的差异。此外，还将讨论与有效温度和大气中的化学物质有关的谱线形成过程。对于合成光谱，使用了通用的恒星大气程序PHONIX[5]。
Since 1995, there have been great advances and extremely exciting results in the search for brown dwarfs and extrasolar giant planets. In the formation of their spectra, the far wings of the alkali resonance lines, especially Na I and K I, play an extraordinary role. Model atmospheres are necessary in order to calculate synthetic spectra and colors and to derive reliable parameters and the atmospheric chemical composition for such objects. Using alkali resonance line profiles [1] and [2], the differences in the synthetic spectra compared to earlier results [3], [4] will be outlined. Besides the line formation process dependent on the effective temperature and the chemistry in the atmosphere will be discussed. For the synthetic spectra, the general purpose stellar atmosphere code PHOENIX [5] is used.