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    Please use this identifier to cite or link to this item: http://ir.lib.ncu.edu.tw/handle/987654321/6114


    Title: 螺旋星系M51,M83和M101內恆星形成機制之研究;Mechanism of star-formation in spiral galaxies M51, M83 and M101
    Authors: 陳以忱;I-Chenn Chen
    Contributors: 天文研究所
    Keywords: 恆星形成;密度波;螺旋星系;spiral galaxy;density wave;star-formation
    Date: 2007-06-22
    Issue Date: 2009-09-22 10:13:26 (UTC+8)
    Publisher: 國立中央大學圖書館
    Abstract: 我們利用鹿林一米望遠鏡(LOT)拍攝了三個螺旋星系,M51、M83和M101的Hα影像;接著我們將這些影像和近紅外波段-2MASS的Ks影像做比較。這麼做的原因是為了要比較在星系的旋臂上,和旋臂間的空隙區域的Hα/K的比值。我們發現,在旋臂上,Hα/K的比值的確比在旋臂間的空隙區域來的高;由於Ks波段影像代表的是的星系中密度波的分佈,也就是說,在密度波分佈的區域,有較高的恆星形成率。另外,我們也發現了恆星形成區域(HII區域)大部分分佈在星系密度波分佈區域的前緣。上述兩個結果都暗示著,在我們所觀測的星系中,密度波是激發恆星形成的主要機制。 We have obtained Hαimages of three nearby face-on galaxies, M51, M83 and M101, by using the Lulin One-meter Telescope (LOT). We then compared these images to the near-infrared Ks band data which is obtained from the 2MASS catalog, in order to determine the Hα/K ratio of galaxies’ K-band arm regions and inter-arm regions. We have found that there is a significant enhancement of Hα/K ratio in K-band arm region, which refers to the location of the density wave. We have also found that the distribution of the HII regions locate on the leading edge of the K-band arms. Both evidences hint that the density wave is the dominant mechanism of star formation in these spiral galaxies, which is in agreement with the large-scale shock scenario, which predicts a high star formation efficiency in arm regions.
    Appears in Collections:[天文研究所] 博碩士論文

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