INTERSTELLAR REDDENING IN THE LOCAL BUBBLE AND LOOP I REGION: INSIGHT FROM STRÖMGREN PHOTOMETRY ANALYSIS AND THREE-DIMENSIONAL MODELING
INTERSTELLAR REDDENING IN THE LOCAL BUBBLE AND LOOP I REGION: INSIGHT FROM STRÖMGREN PHOTOMETRY ANALYSIS AND THREE-DIMENSIONAL MODELING
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DOI：
10.1088/0004-637x/734/1/8
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发表时间：
2011-05
期刊：
影响因子：
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通讯作者：
W. Reis;W. Corradi;M. D. de Avillez;F. Santos
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文献类型：
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作者：
W. Reis;W. Corradi;M. D. de Avillez;F. Santos
太阳位于一个密度极低的区域内，称为局部气泡(LB)。尽管已经通过各种技术对它们进行了研究，但其中性边界的轮廓仍然是一个悬而未决的问题。中性边界由一层致密的星际气体和尘埃墙定义。我们的目标是通过Strömgren光度法来确定LB区的星际变红，并通过与高分辨率的局部和环形I气泡的形成和演化的三维(3D)流体动力学模型的比较来验证结论。我们已经利用光度学数据总表的UvbyHβ数据获得了颜色过剩和距离，并得到了来自较新星表的820颗恒星的补充，用于|b|⩽60°。应用了一套限制性排除标准来消除不适合星际介质研究的E(b−y)值。最终的样本有8492颗恒星，位于距离太阳500pc的地方。我们的主要结果如下：(1)星际尘埃在LB层中的大尺度分布是高度不均匀的；(2)在银河面上，E(b−y)⩾0.ͫ040是在距离d≈80-100pc的距离上观测到的，距离从L⩾270°到L⩽45°；(3)色过剩表明在LB壁上有许多隧道和空洞；(4)E(b−y)与从模拟得到的星际气体的空间密度分布有明显的关联。
The Sun is located inside an extremely low density region called the Local Bubble (LB). Although they have been studied through a large variety of techniques, the contours of its neutral boundary, defined by a dense wall of interstellar gas and dust, are still an open issue. Our aim is to determine the interstellar reddening in the LB region by means of Strömgren photometry, validating the conclusions through a comparison with high-resolution three-dimensional (3D) hydrodynamical models of the Local and Loop I bubbles’ formation and evolution. We have obtained color excesses and distances using the uvbyHβ data of the General Catalogue of Photometric Data, complemented by 820 stars from more recent catalogs, for ∣b∣ ⩽ 60°. A set of restrictive exclusion criteria has been applied to eliminate E(b − y) values inappropriate for the study of the interstellar medium (ISM). The final sample has 8492 stars located up to 500 pc from the Sun. Our main results are as follows: (1) the large-scale distribution of the interstellar dust in the LB is highly inhomogeneous; (2) on the Galactic plane, E(b − y) ⩾ 0.ͫ040 is observed at a distance of d ≈ 80–100 pc from l ⩾ 270° until l ⩽ 45°; (3) the color excess suggests that there are many tunnels and holes in the LB wall; and (4) there is a clear correlation between E(b − y) and the spatial density distribution of the interstellar gas inferred from the simulations.