کد مقاله | کد نشریه | سال انتشار | مقاله انگلیسی | نسخه تمام متن |
---|---|---|---|---|
1779533 | 1022006 | 2006 | 9 صفحه PDF | دانلود رایگان |
عنوان انگلیسی مقاله ISI
Very massive close binaries and the puzzling temporal evolution of 14N in the Solar Neighbourhood
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کلمات کلیدی
موضوعات مرتبط
مهندسی و علوم پایه
فیزیک و نجوم
نجوم و فیزیک نجومی
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![عکس صفحه اول مقاله: Very massive close binaries and the puzzling temporal evolution of 14N in the Solar Neighbourhood Very massive close binaries and the puzzling temporal evolution of 14N in the Solar Neighbourhood](/preview/png/1779533.png)
چکیده انگلیسی
Low metallicity very massive stars with an initial mass between 140Mâ and 260Mâ can be subdivided into two groups: those between 140Mâ and 200Mâ which produce a relatively small amount of Fe, and those with a mass between 200Mâ and 260Mâ where the Fe-yield ejected during the supernova explosion is enormous. We first demonstrate that the inclusion of the second group into a chemical evolutionary model for the Solar Neighbourhood predicts an early temporal evolution of Fe, which is at variance with observations whereas it cannot be excluded that the first group could have been present. We then show that a low metallicity binary with very massive components (with a mass corresponding to the first group) can be an efficient site of primary 14N production through the explosion of a binary component that has been polluted by the pair instability supernova ejecta of its companion. When we implement these massive binary 14N yields in a chemical evolution model, we conclude that very massive close binaries may be important sites of 14N enrichment during the early evolution of the Galaxy.
ناشر
Database: Elsevier - ScienceDirect (ساینس دایرکت)
Journal: New Astronomy - Volume 12, Issue 2, November 2006, Pages 95-103
Journal: New Astronomy - Volume 12, Issue 2, November 2006, Pages 95-103
نویسندگان
D. Vanbeveren, E. De Donder,