Ionisation impact of high-mass stars on interstellar filaments A Herschel study of the RCW 36 bipolar nebula in Vela C ???
Ionisation impact of high-mass stars on interstellar filaments A Herschel study of the RCW 36 bipolar nebula in Vela C ???
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大质量恒星对星际细丝的电离影响 船帆座 C 中 RCW 36 双极星云的赫歇尔研究 ???
DOI：
10.1051/0004-6361/201219423
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发表时间：
2013
影响因子：
6.5
通讯作者：
Minier V
中科院分区：
文献类型：
--
作者：
Minier V
背景化恒星重塑其原始分子云并影响恒星形成，导致壮观的形态，如H区周围的双极星云。正如赫歇尔空间天文台所揭示的那样，分子云是在恒星主要形成的地方形成的。突出的南半球H区，RCW 36，就是这些双极星云之一。目的：我们研究船帆C分子云的丝状结构和RCW 36的双极性形态之间的物理联系，为电离和H区周围的星际结构（明亮的边缘和柱）之间发生的相互作用提供了深入的视角。方法将5个远红外和亚毫米滤光片上的herschelobservations与PACS和SPIRE成像仪进行了比较，并进行了数值模拟和分子线定位。结果rcw36的双极形态是在电离作用下丝状起始的自然演化。结论这些结果表明，丝状结构可能是导致H区边缘形成密集团块的非常动态现象的位置。此外，这些结果可以应用于更好地理解双极星云，这是分子脊或星际细丝内H区膨胀的结果。
ContextIonising stars reshape their original molecular cloud and impact star formation, leading to spectacular morphologies such as bipolar nebulae around H ii regions. Molecular clouds are structured in filaments where stars principally form, as revealed by theHerschelspace observatory. The prominent southern hemisphere H ii region, RCW 36, is one of these bipolar nebulae.AimsWe study the physical connection between the filamentary structures of the Vela C molecular cloud and the bipolar morphology of RCW 36, providing an in-depth view of the interplay occurring between ionisation and interstellar structures (bright-rims and pillars) around an H ii region.MethodsWe have comparedHerschelobservations in five far-infrared and submillimetre filters with the PACS and SPIRE imagers, to dedicated numerical simulations and molecular line mapping.ResultsOur results suggest that the RCW 36 bipolar morphology is a natural evolution of its filamentary beginnings under the impact of ionisation.ConclusionsSuch results demonstrate that, filamentary structures can be the location of very dynamical phenomena inducing the formation of dense clumps at the edge of H ii regions. Moreover, these results could apply to better understanding the bipolar nebulae as a consequence of the expansion of an H ii region within a molecular ridge or an interstellar filament.