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首页> 外文期刊>The Astrophysical journal >SOLAR CARBON MONOXIDE, THERMAL PROFILING, AND THE ABUNDANCES OF C, O, AND THEIR ISOTOPES
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SOLAR CARBON MONOXIDE, THERMAL PROFILING, AND THE ABUNDANCES OF C, O, AND THEIR ISOTOPES

机译：太阳能一氧化碳，热分析以及C，O及其同位素的丰度

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摘要

A solar photospheric "thermal profiling" analysis is presented, exploiting the infrared (2.3-4.6 μm) rovibrational bands of carbon monoxide (CO) as observed with the McMath-Pierce Fourier transform spectrometer (FTS) at Kitt Peak, and from above the Earth's atmosphere by the Shuttle-borne ATMOS experiment. Visible continuum intensities and center-limb behavior constrained the temperature profile of the deep photosphere, while CO center-limb behavior defined the thermal structure at higher altitudes. The oxygen abundance was self-consistently determined from weak CO absorptions (for C/O ≡ 0.5). Our analysis was meant to complement recent studies based on three-dimensional (3D) convection models, which, among other things, have revised the historical solar oxygen (and carbon) abundance downward by a factor of nearly 2, although in fact our conclusions do not support such a revision. Based on various considerations, an ε_O = 700 ± 100 ppm (parts per million relative to hydrogen) is recommended; the large uncertainty reflects the model sensitivity of CO. New solar isotopic ratios also are reported: ~(12)C/~(13)C = 80 ± 1, ~(16)O/~(17)O = 1700 ± 220, and ~(16)O/~(18)O = 440 ± 6—all significantly lower than terrestrial. CO synthesis experiments utilizing a stripped down version of the 3D model—which has large temperature fluctuations in the middle photosphere, possibly inconsistent with CO "movies" from the Infrared Imaging Spectrometer (IRIS), and a steeper mean temperature gradient than matches visible continuum center-limb measurements—point to a lower oxygen abundance (～500 ppm) and isotopic ratios closer to terrestrial. A low oxygen abundance from CO—and other molecules like OH—thus hinges on the reality of the theoretically predicted midphotospheric convective properties.
机译：提出了一个太阳光球“热轮廓”分析，利用了基特峰和地面上空的麦克马斯-皮尔斯·傅里叶变换光谱仪（FTS）观测到的一氧化碳（CO）的红外（2.3-4.6μm）旋转振动带。大气层由航天飞机进行的ATMOS实验。可见的连续强度和中心肢行为限制了深光层的温度分布，而CO中心肢行为则定义了更高海拔的热结构。氧丰度由弱的CO吸收量自洽确定（对于C / O≥0.5）。我们的分析旨在补充基于三维（3D）对流模型的最新研究，该模型除其他外将历史太阳氧（和碳）丰度向下修正了将近2倍，尽管事实上我们的结论确实不支持这样的修订。基于各种考虑，建议ε_O= 700±100 ppm（相对于氢的百万分之几）。大的不确定性反映了CO的模型敏感性。还报道了新的太阳同位素比：〜（12）C /〜（13）C = 80±1，〜（16）O /〜（17）O = 1700±220，和（16）O /〜（18）O = 440±6-都大大低于地面。使用3D模型的精简版进行CO合成实验，该模型在中间光球中具有较大的温度波动，可能与红外成像光谱仪（IRIS）的CO“运动”不一致，并且平均温度梯度比与可见的连续谱中心相匹配的陡峭-肢体测量-指出较低的氧丰度（〜500 ppm）和同位素比更接近于陆地。因此，CO和其他分子（如OH）的低氧丰度取决于理论上预测的中光层对流特性的现实。

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