Silicate and hydrocarbon emission from Galactic M supergiants
Silicate and hydrocarbon emission from Galactic M supergiants
复制标题
银河 M 超巨星的硅酸盐和碳氢化合物排放
DOI：
10.1046/j.1365-8711.1998.02078.x
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发表时间：
1998
影响因子：
4.8
通讯作者：
M. Barlow
中科院分区：
文献类型：
--
作者：
R. J. Sylvester;C. Skinner;M. Barlow
ABSTRA C T继我们在一些h和x Per的M超巨星中发现了未识别的红外（UIR）带发射之后，我们获得了60个银河系M超巨星样品的10毫米光谱。只有三个新的来源，V1749 Cyg，UWAql和IRCa 40 427，似乎显示UIR波段;其他显示预期的硅酸盐发射或无特征的连续谱。因此，在M超巨星中，h和x Per星系团的UIR波段辐射的发生率比整个银河系要高得多。讨论了富氧超巨星UIR带的起源和分布的可能解释。我们使用我们的光谱，以获得质量损失率范围从10 - 10 - 10 - 4 M（yr-1）的新样品，在硅酸盐特征发射的功率的基础上。讨论了M超巨星的质量损失率与光度之间的关系，并探讨了它们的中红外发射性质之间的相关性。
ABSTRA C T Following our discovery of unidentified infrared (UIR) band emission in a number of M supergiants in h and x Per, we have obtained 10-mm spectra of a sample of 60 galactic M supergiants. Only three new sources, V1749 Cyg, UWAql and IRCa40 427, appear to show the UIR bands; the others show the expected silicate emission or a featureless continuum. The occurrence of UIR-band emission in M supergiants is therefore much higher in the h and x Per cluster than in the Galaxy as a whole. Possible explanations for the origin and distribution of UIR bands in oxygen-rich supergiants are discussed. We use our spectra to derive mass-loss rates ranging from 10 ˇ8 to 10 ˇ4 M( yr ˇ1 for the new sample, based on the power emitted in the silicate feature. The relationship between mass-loss rate and luminosity for M supergiants is discussed, and correlations are explored between their mid-infrared emission properties.