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我们在[7]中引进了Gorenstein平坦模。本文将这类模的刻画推广到任意n-Gorenstein环上,并利用这类模刻画了n-Gorestein环。而且,我们证明了任意n-Gorenstein环上Gorenstein平坦预包络的存在性,并证得得这种环关于Gorenstein平坦模的内射类的整体维数至多为n-2,当n≤1时,该整体维数为零。 相似文献
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Close LM Lenzen R Guirado JC Nielsen EL Mamajek EE Brandner W Hartung M Lidman C Biller B 《Nature》2005,433(7023):286-289
Mass is the most fundamental parameter of a star, yet it is also one of the most difficult to measure directly. In general, astronomers estimate stellar masses by determining the luminosity and using the 'mass-luminosity' relationship, but this relationship has never been accurately calibrated for young, low-mass stars and brown dwarfs. Masses for these low-mass objects are therefore constrained only by theoretical models. A new high-contrast adaptive optics camera enabled the discovery of a young (50 million years) companion only 0.156 arcseconds (2.3 au) from the more luminous (> 120 times brighter) star AB Doradus A. Here we report a dynamical determination of the mass of the newly resolved low-mass companion AB Dor C, whose mass is 0.090 +/- 0.005 solar masses. Given its measured 1-2-micrometre luminosity, we have found that the standard mass-luminosity relations overestimate the near-infrared luminosity of such objects by about a factor of approximately 2.5 at young ages. The young, cool objects hitherto thought to be substellar in mass are therefore about twice as massive, which means that the frequency of brown dwarfs and planetary mass objects in young stellar clusters has been overestimated. 相似文献
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