博碩士論文 942209011 完整後設資料紀錄

DC 欄位 語言
DC.contributor天文研究所zh_TW
DC.creator陳以忱zh_TW
DC.creatorI-Chenn Chenen_US
dc.date.accessioned2007-7-18T07:39:07Z
dc.date.available2007-7-18T07:39:07Z
dc.date.issued2007
dc.identifier.urihttp://ir.lib.ncu.edu.tw:88/thesis/view_etd.asp?URN=942209011
dc.contributor.department天文研究所zh_TW
DC.description國立中央大學zh_TW
DC.descriptionNational Central Universityen_US
dc.description.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。zh_TW
dc.description.abstractWe 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.en_US
DC.subject恆星形成zh_TW
DC.subject密度波zh_TW
DC.subject螺旋星系zh_TW
DC.subjectspiral galaxyen_US
DC.subjectdensity waveen_US
DC.subjectstar-formationen_US
DC.title螺旋星系M51,M83和M101內恆星形成機制之研究zh_TW
dc.language.isozh-TWzh-TW
DC.titleMechanism of star-formation in spiral galaxies M51, M83 and M101en_US
DC.type博碩士論文zh_TW
DC.typethesisen_US
DC.publisherNational Central Universityen_US

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