977 resultados para P. m acrospicula L. B. Cai


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Ptilagrostis macrospicula L.B.Cai, sp.nov. Fig.1

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在标本室研究和野外考察的基础上,对中国细柄茅属Ptilagrostis Griseb.几个类群进行了分类修订.双叉细柄茅P. dichotoma Keng ex Tzvelev和窄穗细柄茅P. junatovii Grub.分别被归并到细柄茅P.mongholica (Turcz. ex Trin.)和太白细柄茅P. concinna (Hook. f.) Roshev.中作异名;小花细柄茅P. dichotoma Keng ex Tzvelev var.roshevitsiana Tzvelev则被提升为种P. roshevitsiana (Tzvelev) L. B. Cai.

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Conselho Nacional de Desenvolvimento Científico e Tecnolgico (CNPq)

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Mémoire numérisé par la Direction des bibliothèques de l'Université de Montréal.

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Mémoire numérisé par la Direction des bibliothèques de l'Université de Montréal.

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C17H2602, M, = 262, triclinic, PI, a = 8.513(2), b = 8.970(2), c = 11.741(3)A, a = 120.51 (5), fl = 93.30(4), y = 68.43(4) ° , V = 708.9,/k 3, Z = 2, D O = 1.213, D e = 1.227 Mg m -a, g(Mo Ka, 2 = 0.7107 ,&) = 0.084 mm -1, F(000) = 288. The structure, solved by direct methods, has been refined to an R value of 5.9% using 1361 intensity measurements. The ring junctions, in sequence from either end of the polycycle, are cis, trans and cis.

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<p>We report on our findings based on the analysis of observations of the Type II-L supernova LSQ13cuw within the framework of currently accepted physical predictions of core-collapse supernova explosions. LSQ13cuw was discovered within a day of explosion, hitherto unprecedented for Type II-L supernovae. This motivated a comparative study of Type II-P and II-L supernovae with relatively well-constrained explosion epochs and rise times to maximum (optical) light. From our sample of twenty such events, we find evidence of a positive correlation between the duration of the rise and the peak brightness. On average, SNe II-L tend to have brighter peak magnitudes and longer rise times than SNe II-P. However, this difference is clearest only at the extreme ends of the rise time versus peak brightness relation. Using two different analytical models, we performed a parameter study to investigate the physical parameters that control the rise time behaviour. In general, the models qualitatively reproduce aspects of the observed trends. We find that the brightness of the optical peak increases for larger progenitor radii and explosion energies, and decreases for larger masses. The dependence of the rise time on mass and explosion energy is smaller than the dependence on the progenitor radius. We find no evidence that the progenitors of SNe II-L have significantly smaller radii than those of SNe II-P.p>