The effects of new Na I D line profiles in cool atmospheres
The effects of new Na I D line profiles in cool atmospheres
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新 Na I D 线轮廓在凉爽大气中的效果
DOI：
10.1051/0004-6361:20077074
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发表时间：
2007
影响因子：
6.5
通讯作者：
Whittingham
中科院分区：
文献类型：
--
作者：
Johnas;C. M. S;Hauschildt;Schweitzer;Mullamphy;D. F. T;Whittingham
目的研究新的D线轮廓及其对冷矮星PHOENIX合成谱的影响。钠是最丰富的碱在冷矮大气中，主要负责的形状的opticalspectrum.MethodsIn以前的工作中，我们已经指出了原子氢作为一个扰动的重要性。在这里，加宽由于碰撞原子氢以及完全量子力学计算的配置文件由氦扰动的共振线轮廓。此外，新的线轮廓的影响相比，已经存在的线轮廓calculations.ResultsWe已经计算了一些“GAIA-第二”类模型大气和合成光谱的有效温度从1100 K到3000 K考虑重力为4.5。用磁通贡献函数分析了谱线的形成过程。由于大气结构的变化，有效温度越小，谱线轮廓对合成光谱的影响越大。氢作为扰动的影响是可见的，在较高的有效温度，虽然在同一时间的分子带的强度增加。此外，新引入的完全量子力学计算的加宽的配置文件通过减少钠吸收线的通量和深度来改变合成光谱。
AimsNew D line profiles and their effects on synthetic spectra of cool dwarfs computed with PHOENIX are studied. Sodium is the most abundant alkali in cool dwarf atmospheres and mostly responsible for the shape of the optical spectrum.MethodsIn previous work we have pointed out the importance of atomic hydrogen as a perturber. Here, broadening due to collisions with atomic hydrogen as well as fully quantum mechanically calculated profiles for perturbations by helium are introduced for the resonance line profiles. Furthermore, the effects of the new line profiles are compared to already existing line profile calculations.ResultsWe have calculated a number of “GAIA-cond” class model atmospheres and synthetic spectra for effective temperatures from 1100 K to 3000 K considering a gravity of 4.5. The line formation process has been analyzed with the flux contribution function. Due to changes in atmospheric structure, the effects of the line profiles on the synthetic spectra become larger for smaller effective temperatures. The influence of hydrogen as perturber is visible at higher effective temperatures although at the same time the strength of molecular bands increases. Furthermore, the newly introduced fully quantum mechanically calculated broadened profiles change the synthetic spectra by reducing the flux and the depths of the sodium absorption lines.
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DOI：
--
发表时间：
2006
期刊：
影响因子：
--
作者：
C. Johnas;N. Allard;D. Homeier;P. Hauschildt
通讯作者：
P. Hauschildt
VB 10 的 Keck 高分辨率光谱分析
影响因子：
4.8
作者：
A. Schweitzer;P. Hauschildt;F. Allard;G. Basri
通讯作者：
G. Basri
影响因子：
4.9
作者：
Burrows, A;Volobuyev, M
通讯作者：
Volobuyev, M
影响因子：
64.8
作者：
T. Nakajima;B. Oppenheimer;S. Kulkarni;D. Golimowski;K. Matthews;S. Durrance
通讯作者：
T. Nakajima;B. Oppenheimer;S. Kulkarni;D. Golimowski;K. Matthews;S. Durrance
DOI：
10.1086/308462
发表时间：
1999
期刊：
The Astrophysical Journal
影响因子：
--
作者：
Adam Burrows;M. Marley;C. M. Sharp
通讯作者：
C. M. Sharp